{ "id": 40357, "url": "https://svs.gsfc.nasa.gov/gallery/sdo4k-content/", "page_type": "Gallery", "title": "SDO: 4k Content", "description": "Since 2010, the Solar Dynamics Observatory has taken 60 million images of the sun and 2 comets. Here are a few of our favorites.", "release_date": "2018-09-13T09:22:28-04:00", "update_date": "2024-06-07T00:00:00-04:00", "main_image": { "id": 857386, "url": "https://svs.gsfc.nasa.gov/images/More_Info.jpg", "filename": "More_Info.jpg", "media_type": "Image", "alt_text": "All of the Fermi Gamma-ray Space Telescope's news releases in chronological order", "width": 180, "height": 320, "pixels": 57600 }, "media_groups": [ { "id": 371266, "url": "https://svs.gsfc.nasa.gov/gallery/sdo4k-content/#media_group_371266", "widget": "Basic text (large)", "title": "Overview", "caption": "", "description": "Since 2010, the Solar Dynamics Observatory has taken 60 million images of the sun and 2 comets. Here are a few of our favorites.", "items": [], "extra_data": {} }, { "id": 373537, "url": "https://svs.gsfc.nasa.gov/gallery/sdo4k-content/#media_group_373537", "widget": "Tile gallery", "title": "2024", "caption": "", "description": "", "items": [ { "id": 421707, "type": "details_page", "extra_data": null, "instance": { "id": 5216, "url": "https://svs.gsfc.nasa.gov/5216/", "page_type": "Visualization", "title": "M6.8 flare at Active Region 13559 - January 29, 2024", "description": "Solar Dynamics Observatory (SDO) operates in a geosynchronous orbit around Earth to obtain a continuous view of the Sun. The particular instrument in this visualization records imagery in the ultraviolet portion of the spectrum at wavelengths normally absorbed by Earth's atmosphere - so we need to observe them from space.Active Region 13559 now carried by solar rotation to the upper right limb of the solar disk, launches a mid-range (M6.8 class) flare. For details of this event, see the Space Weather database entry. A large arcade of plasma loops forms after the event, more visible in the 171 angstrom and 304 angstrom filters. An eclipse of the Sun by Earth provides a nice 'curtain close' for the event. For more information on the classification of solar flares, see Solar Flares: What Does It Take to Be X-Class? or X-Class: A Guide to Solar Flares. The point-spread function correction (PSF) has been applied to all this imagery. || ", "release_date": "2024-02-15T00:00:00-05:00", "update_date": "2024-02-12T14:34:19.009000-05:00", "main_image": { "id": 1089234, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a005200/a005216/20240129_AR13559M68_AIA131_PSF_stamped.000486_print.jpg", "filename": "20240129_AR13559M68_AIA131_PSF_stamped.000486_print.jpg", "media_type": "Image", "alt_text": "The M 6.8 flare erupts from Active Region 13559 near the right limb of the image in this view from SDO/AIA 131 angstrom filter. The point-spread function correction (PSF) has been applied to all this imagery. ", "width": 1024, "height": 1024, "pixels": 1048576 } } }, { "id": 421708, "type": "details_page", "extra_data": null, "instance": { "id": 5215, "url": "https://svs.gsfc.nasa.gov/5215/", "page_type": "Visualization", "title": "M5.1 flare 'Double Whammy', at Active Regions 13559 and 13561 - January 23, 2024", "description": "Solar Dynamics Observatory (SDO) operates in a geosynchronous orbit around Earth to obtain a continuous view of the Sun. The particular instrument in this visualization records imagery in the ultraviolet portion of the spectrum at wavelengths normally absorbed by Earth's atmosphere - so we need to observe them from space.Almost simultaneous flares at Active Region 13559 (upper left of disk) and Active Region 13561 (lower right of disk) fire off, with a combined X-ray flux equivalent of an M5.1 solar flare. For details of this event, see the Space Weather database entry for both events.For more information on the classification of solar flares, see Solar Flares: What Does It Take to Be X-Class? or X-Class: A Guide to Solar Flares. The point-spread function correction (PSF) has been applied to all this imagery. || ", "release_date": "2024-02-13T00:00:00-05:00", "update_date": "2024-02-06T08:37:42.772624-05:00", "main_image": { "id": 1089055, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a005200/a005215/20240123_AR13559M51_AIA131_PSF_stamped.000435_print.jpg", "filename": "20240123_AR13559M51_AIA131_PSF_stamped.000435_print.jpg", "media_type": "Image", "alt_text": "Two small flares, within minutes of each other (upper left and lower right), erupt in this view from the SDO/AIA 131 angstrom filter.", "width": 1024, "height": 1024, "pixels": 1048576 } } }, { "id": 421709, "type": "details_page", "extra_data": null, "instance": { "id": 14531, "url": "https://svs.gsfc.nasa.gov/14531/", "page_type": "Produced Video", "title": "February 16, 2024 X2.5 Solar Flare", "description": "NASA’s Solar Dynamics Observatory captured these images of a solar flare – as seen in the bright flash on the right of each image – on Feb. 16, 2024. The images show three subsets of extreme ultraviolet light that highlight the extremely hot material in flares and which are colorized in teal, gold, and red. Credit: NASA/SDO || Feb_16_Flare_Video_multi_still.jpg (1920x1080) [389.3 KB] || Feb_16_Flare_Video_multi_still_searchweb.png (320x180) [85.5 KB] || Feb_16_Flare_Video_multi_still_thm.png (80x40) [7.1 KB] || Feb_16_Flare_Video_multi.mp4 (1920x1080) [53.9 MB] || Feb_16_Flare_Video_multi.mov (1920x1080) [379.3 MB] || ", "release_date": "2024-02-20T10:00:00-05:00", "update_date": "2024-02-20T10:12:16.938068-05:00", "main_image": { "id": 1089343, "url": "https://svs.gsfc.nasa.gov/vis/a010000/a014500/a014531/Feb_16_Flare_Video_multi_still.jpg", "filename": "Feb_16_Flare_Video_multi_still.jpg", "media_type": "Image", "alt_text": "NASA’s Solar Dynamics Observatory captured these images of a solar flare – as seen in the bright flash on the right of each image – on Feb. 16, 2024. The images show three subsets of extreme ultraviolet light that highlight the extremely hot material in flares and which are colorized in teal, gold, and red. Credit: NASA/SDO", "width": 1920, "height": 1080, "pixels": 2073600 } } }, { "id": 429938, "type": "details_page", "extra_data": null, "instance": { "id": 5225, "url": "https://svs.gsfc.nasa.gov/5225/", "page_type": "Visualization", "title": "X2.5 flare at Active Region 13576 - February 16, 2024", "description": "Solar Dynamics Observatory (SDO) operates in a geosynchronous orbit around Earth to obtain a continuous view of the Sun. The particular instrument in this visualization records imagery in the ultraviolet portion of the spectrum at wavelengths normally absorbed by Earth's atmosphere - so we need to observe them from space.Active Region 13576, now carried by solar rotation to the lower right limb of the solar disk, launches an X2.5 class flare. For details of this event, see the Space Weather database entry. Lots of post-flare filament activity on the limb, particularly solar material falling back towards the Sun.For more information on the classification of solar flares, see Solar Flares: What Does It Take to Be X-Class? or X-Class: A Guide to Solar Flares. The point-spread function correction (PSF) has been applied to all this imagery. || ", "release_date": "2024-03-12T00:00:00-04:00", "update_date": "2024-03-06T09:01:22.997521-05:00", "main_image": { "id": 1089943, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a005200/a005225/20240216_AR13576X25_AIA131_PSF_stamped.000286_print.jpg", "filename": "20240216_AR13576X25_AIA131_PSF_stamped.000286_print.jpg", "media_type": "Image", "alt_text": "Active Region 13576, now carried by solar rotation to the lower right limb of the solar disk, launches an X2.5 class flare in this view with the SDO/AIA 131 angstrom filter. Lots of post-flare filament activity on the limb, particularly solar material falling back towards the Sun.", "width": 1024, "height": 1024, "pixels": 1048576 } } }, { "id": 429939, "type": "details_page", "extra_data": null, "instance": { "id": 5224, "url": "https://svs.gsfc.nasa.gov/5224/", "page_type": "Visualization", "title": "M6.5 flare at Active Region 13576 - February 12, 2024", "description": "Solar Dynamics Observatory (SDO) operates in a geosynchronous orbit around Earth to obtain a continuous view of the Sun. The particular instrument in this visualization records imagery in the ultraviolet portion of the spectrum at wavelengths normally absorbed by Earth's atmosphere - so we need to observe them from space.About a day after a previous M-class eruption, Active Region 13576 now launches another mid-range (M6.5 class) flare. For details of this event, see the Space Weather database entry. Near the end of this movie, we can see another lump of hot plasma erupting from the lower right from an active region now on the backside of the Sun from Earth.For more information on the classification of solar flares, see Solar Flares: What Does It Take to Be X-Class? or X-Class: A Guide to Solar Flares. The point-spread function correction (PSF) has been applied to all this imagery. || ", "release_date": "2024-03-12T00:00:00-04:00", "update_date": "2024-03-13T10:44:10.209425-04:00", "main_image": { "id": 1089938, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a005200/a005224/20240212_AR13576M65_AIA131_PSF_stamped.000380_print.jpg", "filename": "20240212_AR13576M65_AIA131_PSF_stamped.000380_print.jpg", "media_type": "Image", "alt_text": "About a day after a previous M-class eruption, Active Region 13576 launches another mid-range (M6.5 class) flare in the view through the SDO/AIA 131 angstrom filter. Near the end of this movie, we can see another lump of hot plasma erupting from the lower right from an active region now on the backside of the Sun from Earth.", "width": 1024, "height": 1024, "pixels": 1048576 } } }, { "id": 429940, "type": "details_page", "extra_data": null, "instance": { "id": 5223, "url": "https://svs.gsfc.nasa.gov/5223/", "page_type": "Visualization", "title": "M9.0 flare at Active Region 13576 - February 10, 2024", "description": "Solar Dynamics Observatory (SDO) operates in a geosynchronous orbit around Earth to obtain a continuous view of the Sun. The particular instrument in this visualization records imagery in the ultraviolet portion of the spectrum at wavelengths normally absorbed by Earth's atmosphere - so we need to observe them from space.Active Region 13576 near the center of the solar disk, launches an M9.0 class flare. A bright filament of plasma is launched to the upper right from the site of the event. For details of this event, see the Space Weather database entry. For more information on the classification of solar flares, see Solar Flares: What Does It Take to Be X-Class? or X-Class: A Guide to Solar Flares. The point-spread function correction (PSF) has been applied to all this imagery. || ", "release_date": "2024-03-12T00:00:00-04:00", "update_date": "2024-03-06T08:07:27.901837-05:00", "main_image": { "id": 1089932, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a005200/a005223/20240210_AR13576M90_AIA131_PSF_stamped.000346_print.jpg", "filename": "20240210_AR13576M90_AIA131_PSF_stamped.000346_print.jpg", "media_type": "Image", "alt_text": "Active Region 13576 near the center of the solar disk, launches an M9.0 class flare in this view through the SDO/AIA 131 angstrom filter. A bright filament of plasma is launched to the upper right from the site of the event.", "width": 1024, "height": 1024, "pixels": 1048576 } } }, { "id": 429941, "type": "details_page", "extra_data": null, "instance": { "id": 5220, "url": "https://svs.gsfc.nasa.gov/5220/", "page_type": "Visualization", "title": "X3.3 flare at Active Region 13575 - February 9, 2024", "description": "Solar Dynamics Observatory (SDO) operates in a geosynchronous orbit around Earth to obtain a continuous view of the Sun. The particular instrument in this visualization records imagery in the ultraviolet portion of the spectrum at wavelengths normally absorbed by Earth's atmosphere - so we need to observe them from space.Just days after an eruption, Active Region 13575, now carried by solar rotation just over the lower right limb of the solar disk, launches an X3.3 class flare. For details of this event, see the Space Weather database entry. For more information on the classification of solar flares, see Solar Flares: What Does It Take to Be X-Class? or X-Class: A Guide to Solar Flares. The point-spread function correction (PSF) has been applied to all this imagery. || ", "release_date": "2024-03-12T00:00:00-04:00", "update_date": "2024-03-05T15:49:45.790720-05:00", "main_image": { "id": 1089896, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a005200/a005220/20240209_AR13575X33_AIA131_PSF_stamped.000670_print.jpg", "filename": "20240209_AR13575X33_AIA131_PSF_stamped.000670_print.jpg", "media_type": "Image", "alt_text": "Active Region 13575 errupts again just over the lower right limb of the solar disk, this time with a powerful X3.3 class solar flare in this view from the SDO/AIA 131 angstrom filter.", "width": 1024, "height": 1024, "pixels": 1048576 } } }, { "id": 429942, "type": "details_page", "extra_data": null, "instance": { "id": 5218, "url": "https://svs.gsfc.nasa.gov/5218/", "page_type": "Visualization", "title": "M5.1 flare at Active Region 13575 - February 7, 2024", "description": "Solar Dynamics Observatory (SDO) operates in a geosynchronous orbit around Earth to obtain a continuous view of the Sun. The particular instrument in this visualization records imagery in the ultraviolet portion of the spectrum at wavelengths normally absorbed by Earth's atmosphere - so we need to observe them from space.Active Region 13575 near the lower right limb of the solar disk erupts with an M5.1 class solar flare. For details of this event, see the Space Weather database entry For more information on the classification of solar flares, see Solar Flares: What Does It Take to Be X-Class? or X-Class: A Guide to Solar Flares. The point-spread function correction (PSF) has been applied to all this imagery. || ", "release_date": "2024-03-12T00:00:00-04:00", "update_date": "2024-03-05T15:13:44.345851-05:00", "main_image": { "id": 1089890, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a005200/a005218/20240207_AR13575M51_AIA131_PSF_stamped.000468_print.jpg", "filename": "20240207_AR13575M51_AIA131_PSF_stamped.000468_print.jpg", "media_type": "Image", "alt_text": "Active Region 13575 near the lower right limb of the solar disk erupts with an M5.1 class solar flare in this view from the SDO/AIA 131 angstrom filter.", "width": 1024, "height": 1024, "pixels": 1048576 } } }, { "id": 429943, "type": "details_page", "extra_data": null, "instance": { "id": 5239, "url": "https://svs.gsfc.nasa.gov/5239/", "page_type": "Visualization", "title": "M7.4 flare at Active Region 13599 - March 10, 2024", "description": "Solar Dynamics Observatory (SDO) operates in a geosynchronous orbit around Earth to obtain a continuous view of the Sun. The particular instrument in this visualization records imagery in the ultraviolet portion of the spectrum at wavelengths normally absorbed by Earth's atmosphere - so we need to observe them from space.Active Region 13559 launches a mid-range (M7.4 class) flare. For details of this event, see the Space Weather database entry. For more information on the classification of solar flares, see Solar Flares: What Does It Take to Be X-Class? or X-Class: A Guide to Solar Flares. The point-spread function correction (PSF) has been applied to all this imagery. || ", "release_date": "2024-03-26T00:00:00-04:00", "update_date": "2024-03-21T07:25:01.936137-04:00", "main_image": { "id": 1090364, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a005200/a005239/20240310_AR13599M74_AIA131_PSF_stamped.000534_print.jpg", "filename": "20240310_AR13599M74_AIA131_PSF_stamped.000534_print.jpg", "media_type": "Image", "alt_text": "An M7.4 flare erupts from Active Region 13599 in the lower right quadrant of the image in this view from SDO/AIA 131 angstrom filter. The point-spread function correction (PSF) has been applied to all this imagery.", "width": 1024, "height": 1024, "pixels": 1048576 } } }, { "id": 429944, "type": "details_page", "extra_data": null, "instance": { "id": 5233, "url": "https://svs.gsfc.nasa.gov/5233/", "page_type": "Visualization", "title": "X6.3 flare at Active Region 13590 - February 22, 2024", "description": "Solar Dynamics Observatory (SDO) operates in a geosynchronous orbit around Earth to obtain a continuous view of the Sun. The particular instrument in this visualization records imagery in the ultraviolet portion of the spectrum at wavelengths normally absorbed by Earth's atmosphere - so we need to observe them from space.And yet again, less than a day after it's X1.7 flare, Active Region 13590 tops off the day with an X6.3 eruption (largest so far this solar cycle) in the upper left quadrant. For details of this event, see the Space Weather database entry. For more information on the classification of solar flares, see Solar Flares: What Does It Take to Be X-Class? or X-Class: A Guide to Solar Flares. The point-spread function correction (PSF) has been applied to all this imagery. || ", "release_date": "2024-03-26T00:00:00-04:00", "update_date": "2024-03-20T14:24:19.566559-04:00", "main_image": { "id": 1090330, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a005200/a005233/20240222_AR13590X63_AIA131_PSF_stamped.000424_print.jpg", "filename": "20240222_AR13590X63_AIA131_PSF_stamped.000424_print.jpg", "media_type": "Image", "alt_text": "An X 6.3 flare erupts from Active Region 13590 in the upper left quadrant of the image in this view from SDO/AIA 131 angstrom filter. The point-spread function correction (PSF) has been applied to all this imagery.", "width": 1024, "height": 1024, "pixels": 1048576 } } }, { "id": 429945, "type": "details_page", "extra_data": null, "instance": { "id": 5232, "url": "https://svs.gsfc.nasa.gov/5232/", "page_type": "Visualization", "title": "X1.7 flare at Active Region 13590 - February 22, 2024", "description": "Solar Dynamics Observatory (SDO) operates in a geosynchronous orbit around Earth to obtain a continuous view of the Sun. The particular instrument in this visualization records imagery in the ultraviolet portion of the spectrum at wavelengths normally absorbed by Earth's atmosphere - so we need to observe them from space.Mere hours after launching an X1.8 flare, Active Region 13590 launches another X-class (X1.7) flare. For details of this event, see the Space Weather database entry.For more information on the classification of solar flares, see Solar Flares: What Does It Take to Be X-Class? or X-Class: A Guide to Solar Flares. The point-spread function correction (PSF) has been applied to all this imagery. || ", "release_date": "2024-03-26T00:00:00-04:00", "update_date": "2024-03-20T13:37:15.246521-04:00", "main_image": { "id": 1090318, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a005200/a005232/20240222_AR13590X17_AIA131_PSF_stamped.000754_print.jpg", "filename": "20240222_AR13590X17_AIA131_PSF_stamped.000754_print.jpg", "media_type": "Image", "alt_text": "An X 1.7 flare erupts from Active Region 13590 in the upper left quadrant of the image in this view from SDO/AIA 131 angstrom filter. The point-spread function correction (PSF) has been applied to all this imagery.", "width": 1024, "height": 1024, "pixels": 1048576 } } }, { "id": 429946, "type": "details_page", "extra_data": null, "instance": { "id": 5231, "url": "https://svs.gsfc.nasa.gov/5231/", "page_type": "Visualization", "title": "X1.8 flare at Active Region 13590 - February 21, 2024", "description": "Solar Dynamics Observatory (SDO) operates in a geosynchronous orbit around Earth to obtain a continuous view of the Sun. The particular instrument in this visualization records imagery in the ultraviolet portion of the spectrum at wavelengths normally absorbed by Earth's atmosphere - so we need to observe them from space.Active Region 13590 in the upper left quadrant of the solar disk, launches a an X1.8 class flare. For details of this event, see the Space Weather database entry. A active region on the lower left limb also exhibits a lot of activity. AR13590 will have a couple more eruptions in the next day... For more information on the classification of solar flares, see Solar Flares: What Does It Take to Be X-Class? or X-Class: A Guide to Solar Flares. The point-spread function correction (PSF) has been applied to all this imagery. || ", "release_date": "2024-03-26T00:00:00-04:00", "update_date": "2024-03-20T13:10:24.926793-04:00", "main_image": { "id": 1090312, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a005200/a005231/20240221_AR13590X18_AIA131_PSF_stamped.000314_print.jpg", "filename": "20240221_AR13590X18_AIA131_PSF_stamped.000314_print.jpg", "media_type": "Image", "alt_text": "An X 1.8 flare erupts from Active Region 13590 in the upper left quadrant of the image in this view from SDO/AIA 131 angstrom filter. The point-spread function correction (PSF) has been applied to all this imagery.", "width": 1024, "height": 1024, "pixels": 1048576 } } }, { "id": 429947, "type": "details_page", "extra_data": null, "instance": { "id": 5244, "url": "https://svs.gsfc.nasa.gov/5244/", "page_type": "Visualization", "title": "M7.4 flare at Active Region 13615 - March 20, 2024", "description": "Solar Dynamics Observatory (SDO) operates in a geosynchronous orbit around Earth to obtain a continuous view of the Sun. The particular instrument in this visualization records imagery in the ultraviolet portion of the spectrum at wavelengths normally absorbed by Earth's atmosphere - so we need to observe them from space.Active Region 13615 launches a mid-range (M7.4 class) flare. For details of this event, see the Space Weather database entry. For more information on the classification of solar flares, see Solar Flares: What Does It Take to Be X-Class? or X-Class: A Guide to Solar Flares. The point-spread function correction (PSF) has been applied to all this imagery. || ", "release_date": "2024-04-04T00:00:00-04:00", "update_date": "2024-04-02T09:32:04.897434-04:00", "main_image": { "id": 1090880, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a005200/a005244/20240320_AR13615M74_AIA131_PSF_stamped.000388_print.jpg", "filename": "20240320_AR13615M74_AIA131_PSF_stamped.000388_print.jpg", "media_type": "Image", "alt_text": "An M7.4 flare erupts from Active Region 13615 in the lower left quadrant of the image in this view from SDO/AIA 131 angstrom filter. The point-spread function correction (PSF) has been applied to all this imagery.", "width": 1024, "height": 1024, "pixels": 1048576 } } }, { "id": 429948, "type": "details_page", "extra_data": null, "instance": { "id": 5243, "url": "https://svs.gsfc.nasa.gov/5243/", "page_type": "Visualization", "title": "M6.7 flare at Active Region 13615 - March 18, 2024", "description": "Solar Dynamics Observatory (SDO) operates in a geosynchronous orbit around Earth to obtain a continuous view of the Sun. The particular instrument in this visualization records imagery in the ultraviolet portion of the spectrum at wavelengths normally absorbed by Earth's atmosphere - so we need to observe them from space.Active Region 13615 launches a mid-range (M6.7 class) flare. For details of this event, see the Space Weather database entry. For more information on the classification of solar flares, see Solar Flares: What Does It Take to Be X-Class? or X-Class: A Guide to Solar Flares. The point-spread function correction (PSF) has been applied to all this imagery. || ", "release_date": "2024-04-04T00:00:00-04:00", "update_date": "2024-04-01T15:01:36.243170-04:00", "main_image": { "id": 1090853, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a005200/a005243/20240318_AR13615M67_AIA131_PSF_stamped.000386_print.jpg", "filename": "20240318_AR13615M67_AIA131_PSF_stamped.000386_print.jpg", "media_type": "Image", "alt_text": "An M6.7 flare erupts from Active Region 13615 in the lower left quadrant of the image in this view from SDO/AIA 131 angstrom filter. The point-spread function correction (PSF) has been applied to all this imagery.", "width": 1024, "height": 1024, "pixels": 1048576 } } }, { "id": 429949, "type": "details_page", "extra_data": null, "instance": { "id": 5246, "url": "https://svs.gsfc.nasa.gov/5246/", "page_type": "Visualization", "title": "M5.3 flare at Active Region 13615 - March 23, 2024", "description": "Solar Dynamics Observatory (SDO) operates in a geosynchronous orbit around Earth to obtain a continuous view of the Sun. The particular instrument in this visualization records imagery in the ultraviolet portion of the spectrum at wavelengths normally absorbed by Earth's atmosphere - so we need to observe them from space.Active Region 13615 launches a mid-range (M5.3 class) flare. For details of this event, see the Space Weather database entry. For more information on the classification of solar flares, see Solar Flares: What Does It Take to Be X-Class? or X-Class: A Guide to Solar Flares. The point-spread function correction (PSF) has been applied to all this imagery. || ", "release_date": "2024-04-18T00:00:00-04:00", "update_date": "2024-04-15T12:43:26.992126-04:00", "main_image": { "id": 1091027, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a005200/a005246/20240323_AR13615M53_AIA131_PSF_stamped.000272_print.jpg", "filename": "20240323_AR13615M53_AIA131_PSF_stamped.000272_print.jpg", "media_type": "Image", "alt_text": "An M5.3 flare erupts from Active Region 13615 near the center of the solar disk in this view from SDO/AIA 131 angstrom filter. The point-spread function correction (PSF) has been applied to all this imagery.", "width": 1024, "height": 1024, "pixels": 1048576 } } }, { "id": 429950, "type": "details_page", "extra_data": null, "instance": { "id": 5245, "url": "https://svs.gsfc.nasa.gov/5245/", "page_type": "Visualization", "title": "X1.1 flare at Active Region 13614 and more - March 23, 2024", "description": "Solar Dynamics Observatory (SDO) operates in a geosynchronous orbit around Earth to obtain a continuous view of the Sun. The particular instrument in this visualization records imagery in the ultraviolet portion of the spectrum at wavelengths normally absorbed by Earth's atmosphere - so we need to observe them from space.Active Regions 13614 (upper middle) and 13615 (lower middle) appear to launch dual solar flares with an equivalent class of X1.1. For details of this event, see the Space Weather database entry. For more information on the classification of solar flares, see Solar Flares: What Does It Take to Be X-Class? or X-Class: A Guide to Solar Flares. The point-spread function correction (PSF) has been applied to all this imagery. || ", "release_date": "2024-04-18T00:00:00-04:00", "update_date": "2024-04-15T11:49:28.117172-04:00", "main_image": { "id": 1091022, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a005200/a005245/20240323_AR13615X11_AIA131_PSF_stamped.000375_print.jpg", "filename": "20240323_AR13615X11_AIA131_PSF_stamped.000375_print.jpg", "media_type": "Image", "alt_text": "Active Regions 13614 (upper) and 13615 (lower) near the center of the solar disk, appear to launch dual solar flares with an equivalent class of X1.1 in this view through the SDO/AIA 131 angstrom filter.", "width": 1024, "height": 1024, "pixels": 1048576 } } }, { "id": 429951, "type": "details_page", "extra_data": null, "instance": { "id": 5268, "url": "https://svs.gsfc.nasa.gov/5268/", "page_type": "Visualization", "title": "Double Filament Eruptions from AR 13614 - March 21, 2024", "description": "Solar Dynamics Observatory (SDO) operates in a geosynchronous orbit around Earth to obtain a continuous view of the Sun. The particular instrument in this visualization records imagery in the ultraviolet portion of the spectrum at wavelengths normally absorbed by Earth's atmosphere - so we need to observe them from space.Active Region 13614 (upper left) launches two CMEs on March 21, 2024. For details of this event, see the Space Weather database entry. || ", "release_date": "2024-05-08T00:00:00-04:00", "update_date": "2024-04-23T09:29:47.100710-04:00", "main_image": { "id": 1091415, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a005200/a005268/20240321_DoubleEruption_AIA171_PSF_stamped.001230_print.jpg", "filename": "20240321_DoubleEruption_AIA171_PSF_stamped.001230_print.jpg", "media_type": "Image", "alt_text": "Two plasma filaments are launched from Active Region 13614 (upper left) in this view from SDO with the AIA 171 Angstrom filter.", "width": 1024, "height": 1024, "pixels": 1048576 } } }, { "id": 429952, "type": "details_page", "extra_data": null, "instance": { "id": 5256, "url": "https://svs.gsfc.nasa.gov/5256/", "page_type": "Visualization", "title": "An M 9.4 flare from Active Region 13615 - March 30, 2024", "description": "Solar Dynamics Observatory (SDO) operates in a geosynchronous orbit around Earth to obtain a continuous view of the Sun. The particular instrument in this visualization records imagery in the ultraviolet portion of the spectrum at wavelengths normally absorbed by Earth's atmosphere - so we need to observe them from space.Active Region 13615 (center right limb) launches an M9.4 class flare. For details of this event, see the Space Weather database entry. For more information on the classification of solar flares, see Solar Flares: What Does It Take to Be X-Class? or X-Class: A Guide to Solar Flares. The point-spread function correction (PSF) has been applied to all this imagery. || ", "release_date": "2024-05-13T00:00:00-04:00", "update_date": "2024-06-05T15:29:55.584615-04:00", "main_image": { "id": 1091915, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a005200/a005256/20240330_AR13615M94_AIA131_PSF_stamped.000398_print.jpg", "filename": "20240330_AR13615M94_AIA131_PSF_stamped.000398_print.jpg", "media_type": "Image", "alt_text": "Active Region 13615 (center right limb) launches an M9.4 flare off the solar limb in this view through the SDO AIA 131 angstrom filter.", "width": 1024, "height": 1024, "pixels": 1048576 } } }, { "id": 429953, "type": "details_page", "extra_data": null, "instance": { "id": 5255, "url": "https://svs.gsfc.nasa.gov/5255/", "page_type": "Visualization", "title": "A Busy Day of flares at Active Region 13615 - March 28, 2024", "description": "Solar Dynamics Observatory (SDO) operates in a geosynchronous orbit around Earth to obtain a continuous view of the Sun. The particular instrument in this visualization records imagery in the ultraviolet portion of the spectrum at wavelengths normally absorbed by Earth's atmosphere - so we need to observe them from space.Multiple M-class and an X-class flares erupt from Active Region AR 13615 on March 28, 2024. For more details, see the Space Weather Database: M7.0, M6.1, M9.7, X1.1.For more information on the classification of solar flares, see Solar Flares: What Does It Take to Be X-Class? or X-Class: A Guide to Solar Flares. The point-spread function correction (PSF) has been applied to all this imagery. || ", "release_date": "2024-05-13T00:00:00-04:00", "update_date": "2024-05-06T14:23:28.805198-04:00", "main_image": { "id": 1091930, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a005200/a005255/20240328_AR13615many_AIA131_PSF_stamped.000428_print.jpg", "filename": "20240328_AR13615many_AIA131_PSF_stamped.000428_print.jpg", "media_type": "Image", "alt_text": "Active Region 13615 (near the lower right limb) erupts with multiple M-class and an X-class solar flares on March 28, 2024 in this view through the SDO AIA 131 angstrom filter.", "width": 1024, "height": 1024, "pixels": 1048576 } } }, { "id": 429954, "type": "details_page", "extra_data": null, "instance": { "id": 14592, "url": "https://svs.gsfc.nasa.gov/14592/", "page_type": "Produced Video", "title": "Largest Flare yet from Solar Cycle 25", "description": "On May 14, 2024, the Sun emitted a strong solar flare. This solar flare is the largest of Solar Cycle 25 and is classified as an X8.7 flare. X-class denotes the most intense flares, while the number provides more information about its strength.A solar flare is an intense burst of radiation, or light, on the Sun. Flares are our solar system’s most powerful explosive events. Light only takes about 8 minutes to travel from the Sun to Earth, so that’s how long it would take the energy from a flare to reach our planet. Stronger solar flares — those rated class M5 or above — can have impacts on technology that depends on Earth’s ionosphere (our electrically charged upper atmosphere), like high-frequency radio used for navigation and GPS.NASA’s Solar Dynamics Observatory (SDO) captured these images of the flare, which peaked at 12:51 p.m. ET on May 14. The X8.7 flare appears on the lower right edge of the Sun. (A small eruption appears afterward in the upper left.) SDO sees the Sun in more than 10 distinct wavelengths of light, showing solar material at different temperatures. Different wavelengths are shown in this video to highlight different features of the flare.Music credit: “Ethereal Mirrorscape” from the album Reflections written and produced by Lars LeonhardWatch this video on the NASA Goddard YouTube channel.Complete transcript available. || X8pt7_flare_May_14_2024.00_00_40_22.Still001.jpg (3840x2160) [3.0 MB] || X8pt7_flare_May_14_2024.00_00_40_22.Still001_print.jpg (1024x576) [342.3 KB] || X8pt7_flare_May_14_2024.00_00_40_22.Still001_searchweb.png (320x180) [75.1 KB] || X8pt7_flare_May_14_2024.00_00_40_22.Still001_web.png (320x180) [75.1 KB] || X8pt7_flare_May_14_2024.00_00_40_22.Still001_thm.png (80x40) [6.1 KB] || 14592_SDO_X8pt7_flare_May_14_2024_ProRes_Outro.webm (3840x2160) [20.4 MB] || 14592_SDO_X8pt7_flare_May_14_2024_Good_Outro.mp4 (3840x2160) [175.9 MB] || 14592_SDO_X8pt7_flare_May_14_2024_YouTube_Outro.mp4 (3840x2160) [673.0 MB] || 14592_SDO_X8pt7_flare_May_14_2024_ProRes_Outro.mov (3840x2160) [4.2 GB] || ", "release_date": "2024-05-14T00:00:00-04:00", "update_date": "2025-03-09T23:18:57.886911-04:00", "main_image": { "id": 1092219, "url": "https://svs.gsfc.nasa.gov/vis/a010000/a014500/a014592/X8pt7_Flare_1651_May_14_2024_131-193-304_crop.jpg", "filename": "X8pt7_Flare_1651_May_14_2024_131-193-304_crop.jpg", "media_type": "Image", "alt_text": "NASA’s Solar Dynamics Observatory captured this image of a solar flare – as seen in the bright flash on the right – on May 14, 2024. The image shows a subset of extreme ultraviolet light that highlights the extremely hot material in flares and which is colorized in red and yellow. Credit: NASA/SDO", "width": 1920, "height": 1080, "pixels": 2073600 } } } ], "extra_data": {} }, { "id": 371267, "url": "https://svs.gsfc.nasa.gov/gallery/sdo4k-content/#media_group_371267", "widget": "Tile gallery", "title": "2023", "caption": "", "description": "", "items": [ { "id": 421710, "type": "details_page", "extra_data": null, "instance": { "id": 5210, "url": "https://svs.gsfc.nasa.gov/5210/", "page_type": "Visualization", "title": "The Active Christmas Eve 2023 Ultraviolet Sun", "description": "Solar Dynamics Observatory (SDO) operates in a geosynchronous orbit around Earth to obtain a continuous view of the Sun. The particular instrument in this visualization records imagery in the ultraviolet portion of the spectrum at wavelengths normally absorbed by Earth's atmosphere - so we need to observe them from space.Solar Dynamics Observatory (SDO) observes a very active hemisphere of the Sun on Christmas Eve 2023. No significant flares - just fifteen hours of small eruptions, bright coronal loops, dark filaments hovering above photosphere, and other small-scale phenomena in the life of a star evolving towards the peak of it's activity cycle.The point-spread function correction (PSF) has been applied to all this imagery. || ", "release_date": "2024-02-16T00:00:00-05:00", "update_date": "2024-02-12T17:15:33.680193-05:00", "main_image": { "id": 1089241, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a005200/a005210/ChristmasEve2023_AIA171_PSF_stamped.001200_print.jpg", "filename": "ChristmasEve2023_AIA171_PSF_stamped.001200_print.jpg", "media_type": "Image", "alt_text": "This view of the Sun, through the SDO/AIA 171 angstrom filter, reveals the flows of hot plasma along the magnetic field lines, glowing from the emission of light by ionized iron atoms which have lost eight electrons (aka Fe IX).", "width": 1024, "height": 1024, "pixels": 1048576 } } }, { "id": 421711, "type": "details_page", "extra_data": null, "instance": { "id": 5206, "url": "https://svs.gsfc.nasa.gov/5206/", "page_type": "Visualization", "title": "X5.0 flare (\"New Years Eve Flare\") at Active Region 13536 - December 31, 2023", "description": "Solar Dynamics Observatory (SDO) operates in a geosynchronous orbit around Earth to obtain a continuous view of the Sun. The particular instrument in this visualization records imagery in the ultraviolet portion of the spectrum at wavelengths normally absorbed by Earth's atmosphere - so we need to observe them from space.The Sun, getting more active as it continues towards the peak of Solar Cycle 25, ends 2023 with a bang as Active Region 13536 on the left limb erupts with an X 5.0 flare, the largest observed so far this cycle. Note that this is probably the same active region (just renumbered) which launched an X2.8 flare a couple weeks earlier (X2.8 flare at Active Region 13514 - December 14, 2023), when solar rotation carried this region over the right limb of the Sun. For details of this event, see the Space Weather database entry.For more information on the classification of solar flares, see Solar Flares: What Does It Take to Be X-Class? or X-Class: A Guide to Solar Flares. The point-spread function correction (PSF) has been applied to all this imagery. || ", "release_date": "2024-02-13T00:00:00-05:00", "update_date": "2024-02-07T13:39:45.382918-05:00", "main_image": { "id": 1089093, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a005200/a005206/20231231_AR13536X50_AIA131_PSF_stamped.000506_print.jpg", "filename": "20231231_AR13536X50_AIA131_PSF_stamped.000506_print.jpg", "media_type": "Image", "alt_text": "Active Region 13536 ends 2023 with a bang as it releases an X5.0 flare as it comes around the left solar limb in this view from the SDO/AIA 131 angstrom filter.", "width": 1024, "height": 1024, "pixels": 1048576 } } }, { "id": 421712, "type": "details_page", "extra_data": null, "instance": { "id": 5205, "url": "https://svs.gsfc.nasa.gov/5205/", "page_type": "Visualization", "title": "M6.3 & M6.9 'double' flares at Active Region 13514 - December 15, 2023", "description": "Solar Dynamics Observatory (SDO) operates in a geosynchronous orbit around Earth to obtain a continuous view of the Sun. The particular instrument in this visualization records imagery in the ultraviolet portion of the spectrum at wavelengths normally absorbed by Earth's atmosphere - so we need to observe them from space.Active Region 13514 near the right limb of the solar disk does a 'double' eruption with two M6 class solar flares minutes apart. For details of this event, see the Space Weather database entry for M6.3 and Space Weather database entry for M6.9.For more information on the classification of solar flares, see Solar Flares: What Does It Take to Be X-Class? or X-Class: A Guide to Solar Flares. The point-spread function correction (PSF) has been applied to all this imagery. || ", "release_date": "2024-01-23T00:00:00-05:00", "update_date": "2024-01-17T09:27:31.268083-05:00", "main_image": { "id": 1088634, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a005200/a005205/20231215_AR13514M63_AIA131_PSF_stamped.000376_print.jpg", "filename": "20231215_AR13514M63_AIA131_PSF_stamped.000376_print.jpg", "media_type": "Image", "alt_text": "The M6.3 and M6.9 'double flare' erupts from Active Region 13514 near the right limb of the image in this view from SDO/AIA 131 angstrom filter. The point-spread function correction (PSF) has been applied to all this imagery.", "width": 1024, "height": 1024, "pixels": 1048576 } } }, { "id": 421713, "type": "details_page", "extra_data": null, "instance": { "id": 5203, "url": "https://svs.gsfc.nasa.gov/5203/", "page_type": "Visualization", "title": "M 5.8 flare at Active Region 13514 - December 14, 2023", "description": "Solar Dynamics Observatory (SDO) operates in a geosynchronous orbit around Earth to obtain a continuous view of the Sun. The particular instrument in this visualization records imagery in the ultraviolet portion of the spectrum at wavelengths normally absorbed by Earth's atmosphere - so we need to observe them from space.Active Region 13514 near the right limb of the solar disk erupts with a class M5.8 flare. For details of this event, see the Space Weather database entry.For more information on the classification of solar flares, see Solar Flares: What Does It Take to Be X-Class? or X-Class: A Guide to Solar Flares. The point-spread function correction (PSF) has been applied to all this imagery. || ", "release_date": "2024-01-11T00:00:00-05:00", "update_date": "2024-01-08T12:57:30.204794-05:00", "main_image": { "id": 1088421, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a005200/a005203/20231214_AR13514M58_AIA131_PSF_stamped.000368_print.jpg", "filename": "20231214_AR13514M58_AIA131_PSF_stamped.000368_print.jpg", "media_type": "Image", "alt_text": "The M 5.8 flare erupts from Active Region 13514 near the right limb of the image in this view from SDO/AIA 131 angstrom filter. The point-spread function correction (PSF) has been applied to all this imagery.", "width": 1024, "height": 1024, "pixels": 1048576 } } }, { "id": 421714, "type": "details_page", "extra_data": null, "instance": { "id": 5204, "url": "https://svs.gsfc.nasa.gov/5204/", "page_type": "Visualization", "title": "X2.8 flare at Active Region 13514 - December 14, 2023", "description": "Solar Dynamics Observatory (SDO) operates in a geosynchronous orbit around Earth to obtain a continuous view of the Sun. The particular instrument in this visualization records imagery in the ultraviolet portion of the spectrum at wavelengths normally absorbed by Earth's atmosphere - so we need to observe them from space.Active Region 13514 near the right limb of the solar disk erupts with a class X2.8 flare. For details of this event, see the Space Weather database entry.For more information on the classification of solar flares, see Solar Flares: What Does It Take to Be X-Class? or X-Class: A Guide to Solar Flares. The point-spread function correction (PSF) has been applied to all this imagery. || ", "release_date": "2024-01-11T00:00:00-05:00", "update_date": "2024-01-08T13:06:29.475781-05:00", "main_image": { "id": 1088427, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a005200/a005204/20231214_AR13514X28_AIA131_PSF_stamped.000304_print.jpg", "filename": "20231214_AR13514X28_AIA131_PSF_stamped.000304_print.jpg", "media_type": "Image", "alt_text": "The X 2.8 flare erupts from Active Region 13514 near the right limb of the image in this view from SDO/AIA 131 angstrom filter. The point-spread function correction (PSF) has been applied to all this imagery.", "width": 1024, "height": 1024, "pixels": 1048576 } } }, { "id": 421715, "type": "details_page", "extra_data": null, "instance": { "id": 5202, "url": "https://svs.gsfc.nasa.gov/5202/", "page_type": "Visualization", "title": "M 5.4 flare at Active Region 13511 - December 8, 2023", "description": "Solar Dynamics Observatory (SDO) operates in a geosynchronous orbit around Earth to obtain a continuous view of the Sun. The particular instrument in this visualization records imagery in the ultraviolet portion of the spectrum at wavelengths normally absorbed by Earth's atmosphere - so we need to observe them from space.Active Region 13511 near the lower right of the solar disk erupts with a class M5.4 flare. A particularly bright loop forms afterwards, apparently as part of the eruption. For details of this event, see the Space Weather database entry.For more information on the classification of solar flares, see Solar Flares: What Does It Take to Be X-Class? or X-Class: A Guide to Solar Flares. The point-spread function correction (PSF) has been applied to all this imagery. || ", "release_date": "2023-12-22T00:00:00-05:00", "update_date": "2023-12-20T07:45:01.732095-05:00", "main_image": { "id": 1088217, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a005200/a005202/20231208_AR13511M54_AIA131_PSF_stamped.000330_print.jpg", "filename": "20231208_AR13511M54_AIA131_PSF_stamped.000330_print.jpg", "media_type": "Image", "alt_text": "The M 5.4 flare erupts from Active Region 13511 in the lower right of the image in this view from SDO/AIA 131 angstrom filter. The point-spread function correction (PSF) has been applied to all this imagery.", "width": 1024, "height": 1024, "pixels": 1048576 } } }, { "id": 421716, "type": "details_page", "extra_data": null, "instance": { "id": 5201, "url": "https://svs.gsfc.nasa.gov/5201/", "page_type": "Visualization", "title": "M 9.8 flare at Active Region 13500 - November 28, 2023", "description": "Solar Dynamics Observatory (SDO) operates in a geosynchronous orbit around Earth to obtain a continuous view of the Sun. The particular instrument in this visualization records imagery in the ultraviolet portion of the spectrum at wavelengths normally absorbed by Earth's atmosphere - so we need to observe them from space.Active Region 13500 near the center of the solar disk erupts with a class M9.8 flare. A nice loop arcade forms, apparently as part of the eruption. For details of this event, see the Space Weather database entry.For more information on the classification of solar flares, see Solar Flares: What Does It Take to Be X-Class? or X-Class: A Guide to Solar Flares. The point-spread function correction (PSF) has been applied to all this imagery. || ", "release_date": "2023-12-13T00:00:00-05:00", "update_date": "2023-12-11T09:23:49.761727-05:00", "main_image": { "id": 1087942, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a005200/a005201/20231128_AR13500M98_AIA131_PSF_stamped.000250_print.jpg", "filename": "20231128_AR13500M98_AIA131_PSF_stamped.000250_print.jpg", "media_type": "Image", "alt_text": "The M 9.8 flare (just short of an X-class flare) erupts on the lower center of the solar disk in this view from SDO/AIA 131 angstrom filter. A nice coronal loop arcade forms afterwards. The point-spread function correction (PSF) has been applied to all this imagery.", "width": 1024, "height": 1024, "pixels": 1048576 } } }, { "id": 421717, "type": "details_page", "extra_data": null, "instance": { "id": 5167, "url": "https://svs.gsfc.nasa.gov/5167/", "page_type": "Visualization", "title": "M 8.7 flare at Active Region 13435 - September 21, 2023", "description": "Solar Dynamics Observatory (SDO) operates in a geosynchronous orbit around Earth to obtain a continuous view of the Sun. The particular instrument in this visualization records imagery in the ultraviolet portion of the spectrum at wavelengths normally absorbed by Earth's atmosphere - so we need to observe them from space.Active Region 13435 near the solar equator erupts with an M8.7 flare as it approaches the center of the solar disk. A similar event had erupted the prior day. For details of this event, see the Space Weather database entry.For more information on the classification of solar flares, see Solar Flares: What Does It Take to Be X-Class? or X-Class: A Guide to Solar Flares. The point-spread function correction (PSF) has been applied to all this imagery. || ", "release_date": "2023-12-13T00:00:00-05:00", "update_date": "2023-10-23T12:50:31.173800-04:00", "main_image": { "id": 860266, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a005100/a005167/20230921_AR13435M87_AIA131_PSF_stamped.000278_print.jpg", "filename": "20230921_AR13435M87_AIA131_PSF_stamped.000278_print.jpg", "media_type": "Image", "alt_text": "Active Region AR13435 launches another M-class flare (M8.7) as it approaches the center of the solar disk in this view from the SDO/AIA 131A filter. The point-spread function correction (PSF) has been applied to all this imagery.", "width": 1024, "height": 1024, "pixels": 1048576 } } }, { "id": 421718, "type": "details_page", "extra_data": null, "instance": { "id": 5166, "url": "https://svs.gsfc.nasa.gov/5166/", "page_type": "Visualization", "title": "M 8.2 flare at Active Region 13435 - September 20, 2023", "description": "Solar Dynamics Observatory (SDO) operates in a geosynchronous orbit around Earth to obtain a continuous view of the Sun. The particular instrument in this visualization records imagery in the ultraviolet portion of the spectrum at wavelengths normally absorbed by Earth's atmosphere - so we need to observe them from space.Active Region 13435 near the solar equator erupts with an M8.2 flare as it approaches the center of the solar disk. A second similar event will erupt the next day. For details of this event, see the Space Weather database entry.For more information on the classification of solar flares, see Solar Flares: What Does It Take to Be X-Class? or X-Class: A Guide to Solar Flares. The point-spread function correction (PSF) has been applied to all this imagery. || ", "release_date": "2023-12-13T00:00:00-05:00", "update_date": "2023-12-12T13:32:09.530999-05:00", "main_image": { "id": 1087957, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a005100/a005166/20230920_AR13435M82_AIA131_PSF_stamped.000637_print.jpg", "filename": "20230920_AR13435M82_AIA131_PSF_stamped.000637_print.jpg", "media_type": "Image", "alt_text": "Active Region AR13435 launches an M8.2 flare as it approaches the center of the solar disk in this view from the SDO/AIA 131A filter. It will erupt again the next day. The point-spread function correction (PSF) has been applied to all this imagery.", "width": 1024, "height": 1024, "pixels": 1048576 } } }, { "id": 410372, "type": "details_page", "extra_data": null, "instance": { "id": 5140, "url": "https://svs.gsfc.nasa.gov/5140/", "page_type": "Visualization", "title": "X 1.5 flare at Active Region 13386 - August 7, 2023", "description": "Solar Dynamics Observatory (SDO) operates in a geosynchronous orbit around Earth to obtain a continuous view of the Sun. The particular instrument in this visualization records imagery in the ultraviolet portion of the spectrum at wavelengths normally absorbed by Earth's atmosphere - so we need to observe them from space.For the third day in a row, the Active Region 13386 erupts with flares exceeding M5 intensity. Here is the X1.5 flare from August 7, 2023 with a nice loop arcade formation afterwards on the limb. For details of this event, see the Space Weather database entry.For more information on the classification of solar flares, see Solar Flares: What Does It Take to Be X-Class? or X-Class: A Guide to Solar Flares. The point-spread function correction (PSF) has been applied to all this imagery. || ", "release_date": "2023-08-29T00:00:00-04:00", "update_date": "2023-08-28T10:28:33.252587-04:00", "main_image": { "id": 858241, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a005100/a005140/20230807_AR13386X15_AIA131_PSF_stamped.000306_print.jpg", "filename": "20230807_AR13386X15_AIA131_PSF_stamped.000306_print.jpg", "media_type": "Image", "alt_text": "Active Region AR13386 launches an X 1.5 flare as it approaches the right limb of the Sun in this view from the SDO/AIA 131A filter. This region launched flares the previous two days before rotating over the limb as seen from Earth. The point-spread function correction (PSF) has been applied to all this imagery.", "width": 1024, "height": 1024, "pixels": 1048576 } } }, { "id": 410373, "type": "details_page", "extra_data": null, "instance": { "id": 5139, "url": "https://svs.gsfc.nasa.gov/5139/", "page_type": "Visualization", "title": "M 5.5 5lare at Active Region 13386 - August 6, 2023", "description": "Solar Dynamics Observatory (SDO) operates in a geosynchronous orbit around Earth to obtain a continuous view of the Sun. The particular instrument in this visualization records imagery in the ultraviolet portion of the spectrum at wavelengths normally absorbed by Earth's atmosphere - so we need to observe them from space.The day after an X1.6 flare from Active Region 13386, a (smaller) M5.5 flare erupts from the same region. For details of this event, see the Space Weather database entry.For more information on the classification of solar flares, see Solar Flares: What Does It Take to Be X-Class? or X-Class: A Guide to Solar Flares. The point-spread function correction (PSF) has been applied to all this imagery. || ", "release_date": "2023-08-29T00:00:00-04:00", "update_date": "2023-08-24T10:02:47.612628-04:00", "main_image": { "id": 858066, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a005100/a005139/20230806_AR13386M55_AIA131_PSF_stamped.000396_print.jpg", "filename": "20230806_AR13386M55_AIA131_PSF_stamped.000396_print.jpg", "media_type": "Image", "alt_text": "Active Region AR13386 launches an M 5.5 flare as it approaches the right limb of the Sun in this view from the SDO/AIA 131A filter. This region launched a flare the previous day and will launch another one the next day, before rotating over the limb as seen from Earth. The point-spread function correction (PSF) has been applied to all this imagery.", "width": 1024, "height": 1024, "pixels": 1048576 } } }, { "id": 410374, "type": "details_page", "extra_data": null, "instance": { "id": 5138, "url": "https://svs.gsfc.nasa.gov/5138/", "page_type": "Visualization", "title": "X 1.6 flare at Active Region 13386 - August 5, 2023", "description": "Solar Dynamics Observatory (SDO) operates in a geosynchronous orbit around Earth to obtain a continuous view of the Sun. The particular instrument in this visualization records imagery in the ultraviolet portion of the spectrum at wavelengths normally absorbed by Earth's atmosphere - so we need to observe them from space.An X 1.6 flare erupts near the right limb of the Sun on August 5, 2023. The flare peaks around 22:21 UTC on that date. Space Weather Database Entry: Event Description.For more information on the classification of solar flares, see Solar Flares: What Does It Take to Be X-Class? or X-Class: A Guide to Solar Flares. The point-spread function correction (PSF) has been applied to all this imagery. || ", "release_date": "2023-08-29T00:00:00-04:00", "update_date": "2023-08-22T08:07:44.547443-04:00", "main_image": { "id": 857915, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a005100/a005138/20230805_AR13386X16_AIA131_PSF_stamped.000467_print.jpg", "filename": "20230805_AR13386X16_AIA131_PSF_stamped.000467_print.jpg", "media_type": "Image", "alt_text": "Active Region AR13386 launches an X 1.6 flare as it approaches the right limb of the Sun in this view from the SDO/AIA 131A filter. This region will erupt a couple more times before rotating over the limb. The point-spread function correction (PSF) has been applied to all this imagery.", "width": 1024, "height": 1024, "pixels": 1048576 } } }, { "id": 410375, "type": "details_page", "extra_data": null, "instance": { "id": 5128, "url": "https://svs.gsfc.nasa.gov/5128/", "page_type": "Visualization", "title": "X 1.0 flare at Active Region 13354 - July 2, 2023", "description": "Solar Dynamics Observatory (SDO) operates in a geosynchronous orbit around Earth to obtain a continuous view of the Sun. The particular instrument in this visualization records imagery in the ultraviolet portion of the spectrum at wavelengths normally absorbed by Earth's atmosphere - so we need to observe them from space.An X 1.0 flare erupts near the right limb of the Sun on July 2, 2023. The flare peaks around 23:14 UTC on that date. For more information on the classification of solar flares, see Solar Flares: What Does It Take to Be X-Class? or X-Class: A Guide to Solar Flares. The point-spread function correction (PSF) has been applied to all this imagery.Space Weather Database Entry: Event Description. || ", "release_date": "2023-07-28T00:00:00-04:00", "update_date": "2023-07-26T08:27:57.127983-04:00", "main_image": { "id": 857006, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a005100/a005128/20230702_AR13354X10_AIA171_PSF_stamped.000374_print.jpg", "filename": "20230702_AR13354X10_AIA171_PSF_stamped.000374_print.jpg", "media_type": "Image", "alt_text": "Active Region AR13354 launches an X 1.0 flare just before rotating over the upper right limb of the Sun in this view from the SDO/AIA 171A filter. The point-spread function correction (PSF) has been applied to all this imagery.", "width": 1024, "height": 1024, "pixels": 1048576 } } }, { "id": 410376, "type": "details_page", "extra_data": null, "instance": { "id": 5125, "url": "https://svs.gsfc.nasa.gov/5125/", "page_type": "Visualization", "title": "X 1.1 flare at Active Region 13341 - June 20, 2023", "description": "Solar Dynamics Observatory (SDO) operates in a geosynchronous orbit around Earth to obtain a continuous view of the Sun. The particular instrument in this visualization records imagery in the ultraviolet portion of the spectrum at wavelengths normally absorbed by Earth's atmosphere - so we need to observe them from space.An X 1.1 flare erupts from the left limb of the Sun on June 20, 2023. For more information on the classification of solar flares, see Solar Flares: What Does It Take to Be X-Class? or X-Class: A Guide to Solar Flares. The point-spread function correction (PSF) has been applied to all this imagery.Event Description. || ", "release_date": "2023-07-14T00:00:00-04:00", "update_date": "2023-07-10T09:28:30.055262-04:00", "main_image": { "id": 856658, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a005100/a005125/20230620_AR13341X11_AIA171_PSF_stamped.000350_print.jpg", "filename": "20230620_AR13341X11_AIA171_PSF_stamped.000350_print.jpg", "media_type": "Image", "alt_text": "Active region AR 13341 launches an X1.1 class solar flare (lower left) in this view from SDO/AIA in the 171 angstrom filter.", "width": 1024, "height": 1024, "pixels": 1048576 } } }, { "id": 410377, "type": "details_page", "extra_data": null, "instance": { "id": 5108, "url": "https://svs.gsfc.nasa.gov/5108/", "page_type": "Visualization", "title": "An 9.6 M-class flare and Filament - May 16, 2023", "description": "Solar Dynamics Observatory (SDO) operates in a geosynchronous orbit around Earth to obtain a continuous view of the Sun. The particular instrument in this visualization records imagery in the ultraviolet portion of the spectrum at wavelengths normally absorbed by Earth's atmosphere - so we need to observe them from space.Active region AR13310 at the lower left solar limb launches an M 9.6 class flare followed by a bright filament launched almost tangent to the limb. For more information on the classification of solar flares, see Solar Flares: What Does It Take to Be X-Class? or X-Class: A Guide to Solar Flares. The point-spread function correction (PSF) has been applied to all this imagery.Event Description. || ", "release_date": "2023-06-27T00:00:00-04:00", "update_date": "2023-06-22T08:03:26.278999-04:00", "main_image": { "id": 856288, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a005100/a005108/20230516_Filament_M96_AIA171_PSF_stamped.000522_print.jpg", "filename": "20230516_Filament_M96_AIA171_PSF_stamped.000522_print.jpg", "media_type": "Image", "alt_text": "An M 9.6 class flare erupts from the lower left limb of the Sun from Active Region 13310 followed by a bright filament. This is a view through the 171 angstrom filter on the SDO AIA instrument.", "width": 1024, "height": 1024, "pixels": 1048576 } } }, { "id": 410378, "type": "details_page", "extra_data": null, "instance": { "id": 5103, "url": "https://svs.gsfc.nasa.gov/5103/", "page_type": "Visualization", "title": "Dancing on the Limb - May 1, 2023", "description": "Solar Dynamics Observatory (SDO) operates in a geosynchronous orbit around Earth to obtain a continuous view of the Sun. The particular instrument in this visualization records imagery in the ultraviolet portion of the spectrum at wavelengths normally absorbed by Earth's atmosphere - so we need to observe them from space.A large loop of solar plasma executes some interesting long-lived (15 hours in this series) gyrations on the lower solar limb. || ", "release_date": "2023-05-24T00:00:00-04:00", "update_date": "2023-05-19T09:20:23.150857-04:00", "main_image": { "id": 855383, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a005100/a005103/20230501_LimbEvent_AIA171_PSF_stamped.002000_print.jpg", "filename": "20230501_LimbEvent_AIA171_PSF_stamped.002000_print.jpg", "media_type": "Image", "alt_text": "A view of a very active coronal plasma loop (lower solar limb) in this long view using the SDO AIA 171A filter.", "width": 1024, "height": 1024, "pixels": 1048576 } } }, { "id": 410379, "type": "details_page", "extra_data": null, "instance": { "id": 5096, "url": "https://svs.gsfc.nasa.gov/5096/", "page_type": "Visualization", "title": "X 1.2 flare at Active Region 13256 - March 29, 2023", "description": "Solar Dynamics Observatory (SDO) operates in a geosynchronous orbit around Earth to obtain a continuous view of the Sun. The particular instrument in this visualization records imagery in the ultraviolet portion of the spectrum at wavelengths normally absorbed by Earth's atmosphere - so we need to observe them from space.Active region AR13256 near the lower right solar limb launches an X 1.2 class flare. For more information on the classification of solar flares, see Solar Flares: What Does It Take to Be X-Class? or X-Class: A Guide to Solar Flares. The point-spread function correction (PSF) has been applied to all this imagery.Event Description. || ", "release_date": "2023-04-17T12:00:00-04:00", "update_date": "2023-05-03T11:43:36.576847-04:00", "main_image": { "id": 854628, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a005000/a005096/20230329_AR13256X12_AIA171_PSF_stamped.000314_print.jpg", "filename": "20230329_AR13256X12_AIA171_PSF_stamped.000314_print.jpg", "media_type": "Image", "alt_text": "Active Region 13256 (lower right of solar disk) fires off an X1.2 flare in this view from SDO/AIA filter 171 angstroms.", "width": 1024, "height": 1024, "pixels": 1048576 } } }, { "id": 410380, "type": "details_page", "extra_data": null, "instance": { "id": 5085, "url": "https://svs.gsfc.nasa.gov/5085/", "page_type": "Visualization", "title": "X 2.0 flare at Active Region 13234 - March 3, 2023", "description": "Solar Dynamics Observatory (SDO) operates in a geosynchronous orbit around Earth to obtain a continuous view of the Sun. The particular instrument in this visualization records imagery in the ultraviolet portion of the spectrum at wavelengths normally absorbed by Earth's atmosphere - so we need to observe them from space.Active region AR13234 on the right solar limb launches an X 2.0 class flare. The point-spread function correction (PSF) has been applied to all this imagery.Event Description. || ", "release_date": "2023-04-05T00:00:00-04:00", "update_date": "2023-05-09T11:46:59.904818-04:00", "main_image": { "id": 842206, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a005000/a005085/20230303_AR13234X20_AIA171_PSF_stamped.000300_print.jpg", "filename": "20230303_AR13234X20_AIA171_PSF_stamped.000300_print.jpg", "media_type": "Image", "alt_text": "Active Region AR13234 launches an X 2.0 flare just before rotating over the upper right limb of the Sun in this view from the SDO/AIA 1771A filter. The point-spread function correction (PSF) has been applied to all this imagery.", "width": 1024, "height": 1024, "pixels": 1048576 } } }, { "id": 410381, "type": "details_page", "extra_data": null, "instance": { "id": 5084, "url": "https://svs.gsfc.nasa.gov/5084/", "page_type": "Visualization", "title": "Several impressive filament eruptions leading up to an M 8.7 Flare at Active Region 13234 - February 27-28, 2023", "description": "Solar Dynamics Observatory (SDO) operates in a geosynchronous orbit around Earth to obtain a continuous view of the Sun. The particular instrument in this visualization records imagery in the ultraviolet portion of the spectrum at wavelengths normally absorbed by Earth's atmosphere - so we need to observe them from space.Some impressive filaments erupt on the solar limb (lower left and lower right) in the early part of this image series. Later (17:46:42 TAI), an active region in the upper right quadrant of the solar disk launches a mid-level M 8.7 class flare.Event Description || ", "release_date": "2023-06-06T00:00:00-04:00", "update_date": "2023-05-31T09:52:33.068028-04:00", "main_image": { "id": 855590, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a005000/a005084/20230227_AR13234M86_AIA304_PSF_stamped.001120_print.jpg", "filename": "20230227_AR13234M86_AIA304_PSF_stamped.001120_print.jpg", "media_type": "Image", "alt_text": "Large filaments appear off the limb of the Sun (lower left and lower right) in this view from SDO/AIA 304 Angstrom filter. Note the lower right filament visible in this 304 Angstrom image is NOT visible in the 171 Angstrom filter.", "width": 1024, "height": 1024, "pixels": 1048576 } } }, { "id": 410382, "type": "details_page", "extra_data": null, "instance": { "id": 5083, "url": "https://svs.gsfc.nasa.gov/5083/", "page_type": "Visualization", "title": "M 6.3 flare at Active Region 13229 - February 25, 2023", "description": "Solar Dynamics Observatory (SDO) operates in a geosynchronous orbit around Earth to obtain a continuous view of the Sun. The particular instrument in this visualization records imagery in the ultraviolet portion of the spectrum at wavelengths normally absorbed by Earth's atmosphere - so we need to observe them from space.The very next day (after the event on February 24), active region near the center of the solar disk (AR 13229) launches a mid-level M 6.3 class flare and forms a loop arcade. The point-spread function correction (PSF) has been applied to all the imagery on this page.Event Description || ", "release_date": "2023-03-22T00:00:00-04:00", "update_date": "2023-08-14T22:45:30.592114-04:00", "main_image": { "id": 789276, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a005000/a005083/20230225_AR13229M63_AIA171_PSF_stamped.000301_print.jpg", "filename": "20230225_AR13229M63_AIA171_PSF_stamped.000301_print.jpg", "media_type": "Image", "alt_text": "February 25, 2023. Active Region 13229. A 6.3 M-class flare see in SDO/AIA 171 angstrom filter. The point-spread function correction (PSF) has been applied to all this imagery.", "width": 1024, "height": 1024, "pixels": 1048576 } } }, { "id": 410383, "type": "details_page", "extra_data": null, "instance": { "id": 5080, "url": "https://svs.gsfc.nasa.gov/5080/", "page_type": "Visualization", "title": "X 2.2 Flare - February 17, 2023", "description": "Solar Dynamics Observatory (SDO) operates in a geosynchronous orbit around Earth to obtain a continuous view of the Sun. The particular instrument in this visualization records imagery in the ultraviolet portion of the spectrum at wavelengths normally absorbed by Earth's atmosphere - so we need to observe them from space.An active region coming around the left limb of the sun launches an X 2.2 class flare. The point-spread function correction (PSF) has been applied to all the imagery on this page.Event Description || ", "release_date": "2023-03-14T12:00:00-04:00", "update_date": "2025-03-09T23:00:40.361545-04:00", "main_image": { "id": 765104, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a005000/a005080/20230217_AR13229X22_AIA171_PSF_stamped.000636_print.jpg", "filename": "20230217_AR13229X22_AIA171_PSF_stamped.000636_print.jpg", "media_type": "Image", "alt_text": "Active Region 13229 (upper left limb of solar disk) fires off an X2.2 flare in this view from SDO/AIA filter 171 angstroms. The point-spread function correction (PSF) has been applied to all this imagery.", "width": 1024, "height": 1024, "pixels": 1048576 } } }, { "id": 410384, "type": "details_page", "extra_data": null, "instance": { "id": 5079, "url": "https://svs.gsfc.nasa.gov/5079/", "page_type": "Visualization", "title": "X1.1 Flare, Active Region 13217 - February 11, 2023", "description": "Solar Dynamics Observatory (SDO) operates in a geosynchronous orbit around Earth to obtain a continuous view of the Sun. The particular instrument in this visualization records imagery in the ultraviolet portion of the spectrum at wavelengths normally absorbed by Earth's atmosphere - so we need to observe them from space.Here, Active Region 13217 (lower left of solar disk) fires off an X-class flare (X1.1). (Solar Flares: What does it take to be X-class?). The point-spread function correction (PSF) has been applied to all the imagery on this page. Event Description || ", "release_date": "2023-03-14T12:00:00-04:00", "update_date": "2023-05-03T11:43:40.170732-04:00", "main_image": { "id": 765076, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a005000/a005079/20230211_AR13217X11_AIA131.PSF_000268_print.jpg", "filename": "20230211_AR13217X11_AIA131.PSF_000268_print.jpg", "media_type": "Image", "alt_text": "Active Region 13217 (lower left of solar disk) fires off an X1.1 flare in this view from SDO/AIA filter 131 angstroms.", "width": 1024, "height": 1024, "pixels": 1048576 } } }, { "id": 410385, "type": "details_page", "extra_data": null, "instance": { "id": 5082, "url": "https://svs.gsfc.nasa.gov/5082/", "page_type": "Visualization", "title": "M 3.7 Flare and filament eruption at Active Region 13229 - February 24, 2023", "description": "Solar Dynamics Observatory (SDO) operates in a geosynchronous orbit around Earth to obtain a continuous view of the Sun. The particular instrument in this visualization records imagery in the ultraviolet portion of the spectrum at wavelengths normally absorbed by Earth's atmosphere - so we need to observe them from space.A active region AR13229 near the center of the solar disk launches a mid-level M 3.7 class flare followed by a large filament eruption. The point-spread function correction (PSF) has been applied to all the imagery on this page.Event Description || ", "release_date": "2023-03-21T12:00:00-04:00", "update_date": "2023-05-03T11:43:39.229160-04:00", "main_image": { "id": 789273, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a005000/a005082/20230224_AR13229M37_AIA171_PSF_stamped.000152_print.jpg", "filename": "20230224_AR13229M37_AIA171_PSF_stamped.000152_print.jpg", "media_type": "Image", "alt_text": "Active Region 13229 fires off a small M3.7 flare and filament in this view from SDO/AIA filter 171 angstroms. The point-spread function correction (PSF) has been applied to all this imagery.", "width": 1024, "height": 1024, "pixels": 1048576 } } }, { "id": 410386, "type": "details_page", "extra_data": null, "instance": { "id": 5077, "url": "https://svs.gsfc.nasa.gov/5077/", "page_type": "Visualization", "title": "M1 Flare and Eruption on Solar Limb - February 7, 2023", "description": "Solar Dynamics Observatory (SDO) operates in a geosynchronous orbit around Earth to obtain a continuous view of the Sun. The particular instrument in this visualization records imagery in the ultraviolet portion of the spectrum at wavelengths normally absorbed by Earth's atmosphere - so we need to observe them from space.An active region coming around the left limb of the sun launches a small M1 class flare and then an impressive flame-like eruption of solar material. The point-spread function correction (PSF) has been applied to all the imagery on this page. || ", "release_date": "2023-02-27T00:00:00-05:00", "update_date": "2023-08-14T22:45:30.598812-04:00", "main_image": { "id": 764955, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a005000/a005077/20230207_EruptM10_AIA304_PSF_stamped.000244_print.jpg", "filename": "20230207_EruptM10_AIA304_PSF_stamped.000244_print.jpg", "media_type": "Image", "alt_text": "A large eruption of solar material, visible here in the SDO/AIA 304 angstrom filter, is launched from an active region on the left limb of the Sun, associated with an M1-class solar flare. The point-spread function correction (PSF) has been applied to all this imagery.", "width": 1024, "height": 1024, "pixels": 1048576 } } }, { "id": 410387, "type": "details_page", "extra_data": null, "instance": { "id": 5063, "url": "https://svs.gsfc.nasa.gov/5063/", "page_type": "Visualization", "title": "An X1.9 Class Solar Flare and its Aftermath - January 9, 2023", "description": "Solar Dynamics Observatory (SDO) operates in a geosynchronous orbit around Earth to obtain a continuous view of the Sun. The particular instrument in this visualization records imagery in the ultraviolet portion of the spectrum at wavelengths normally absorbed by Earth's atmosphere - so we need to observe them from space.Here, Active Region 13164 (near the lower left limb of the solar disk) fires off a hefty X-class flare (X1.9). (Solar Flares: What does it take to be X-class?). The region continues some active evolution with loops and filaments more visible in the 171A and 304A filters. Smaller M-Class flares erupt later in this sequence, an M 5.1 at the upper left limb and an M 2.6 in the lower right center. The point-spread function correction (PSF) has been applied to all the imagery on this page. || ", "release_date": "2023-02-10T00:00:00-05:00", "update_date": "2023-05-03T11:43:43.568651-04:00", "main_image": { "id": 552423, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a005000/a005063/20230109_AR13184X19_AIA131_PSF_stamped.000254_print.jpg", "filename": "20230109_AR13184X19_AIA131_PSF_stamped.000254_print.jpg", "media_type": "Image", "alt_text": "The X1.9 flare event of January 9, 2023 as seen in the SDO AIA 131 angstrom filter. Two smaller M-class flares occur at later times on other regions on the solar disk. The dark region around the central 'X' marking the flare is an artifact of the PSF correction. 'Flickering' in the images around the flare are created due to the 'flare mode' images which have a shorter exposure. Normalizing the solar disk to the same brightness in these frames enhances the background noise off the solar disk.", "width": 1024, "height": 1024, "pixels": 1048576 } } }, { "id": 410388, "type": "details_page", "extra_data": null, "instance": { "id": 5066, "url": "https://svs.gsfc.nasa.gov/5066/", "page_type": "Visualization", "title": "An X1.0 Class Solar Flare - January 10, 2023", "description": "Solar Dynamics Observatory (SDO) operates in a geosynchronous orbit around Earth to obtain a continuous view of the Sun. The particular instrument in this visualization records imagery in the ultraviolet portion of the spectrum at wavelengths normally absorbed by Earth's atmosphere - so we need to observe them from space.Here, Active Region 13186 (upper left of solar disk) fires off an X-class flare (X1.0). (Solar Flares: What does it take to be X-class?). The point-spread function correction (PSF) has been applied to all the imagery on this page. || ", "release_date": "2023-02-10T00:00:00-05:00", "update_date": "2023-05-03T11:43:43.715844-04:00", "main_image": { "id": 552450, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a005000/a005066/20230110_AR13186X10_AIA131_PSF_stamped.000256_print.jpg", "filename": "20230110_AR13186X10_AIA131_PSF_stamped.000256_print.jpg", "media_type": "Image", "alt_text": "Active Region 13186 (upper left of solar disk) fires off an X-class flare (X1.0) in this view from SDO/AIA filter 131 angstroms.", "width": 1024, "height": 1024, "pixels": 1048576 } } }, { "id": 410389, "type": "details_page", "extra_data": null, "instance": { "id": 5068, "url": "https://svs.gsfc.nasa.gov/5068/", "page_type": "Visualization", "title": "Impressive solar filament eruption - January 20, 2023", "description": "Solar Dynamics Observatory (SDO) operates in a geosynchronous orbit around Earth to obtain a continuous view of the Sun. The particular instrument in this visualization records imagery in the ultraviolet portion of the spectrum at wavelengths normally absorbed by Earth's atmosphere - so we need to observe them from space.A large solar filament hovers above the solar surface (lower right) for several hours before eventually launching into space. || ", "release_date": "2023-02-10T00:00:00-05:00", "update_date": "2023-05-03T11:43:43.824844-04:00", "main_image": { "id": 552547, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a005000/a005068/20230120_FilamentErupt_AIA304_PSF_stamped.001530_print.jpg", "filename": "20230120_FilamentErupt_AIA304_PSF_stamped.001530_print.jpg", "media_type": "Image", "alt_text": "In this imagery from the SDO/AIA 304 angstrom filter, a large solar filament hovers above the solar surface (lower right) for several hours before eventually launching into space.", "width": 1024, "height": 1024, "pixels": 1048576 } } }, { "id": 410390, "type": "details_page", "extra_data": null, "instance": { "id": 5062, "url": "https://svs.gsfc.nasa.gov/5062/", "page_type": "Visualization", "title": "Active Region AR13182 launches an X1.2 Class Solar Flare - January 6, 2023", "description": "Solar Dynamics Observatory (SDO) operates in a geosynchronous orbit around Earth to obtain a continuous view of the Sun. The particular instrument in this visualization records imagery in the ultraviolet portion of the spectrum at wavelengths normally absorbed by Earth's atmosphere - so we need to observe them from space.Here, Active Region 13182 (lower left of solar disk on limb) launches an X1.2-class flare in early January 2023 (Solar Flares: What does it take to be X-class?). The point-spread function correction (PSF) has been applied to all the imagery on this page. || ", "release_date": "2023-01-19T12:00:00-05:00", "update_date": "2023-05-03T11:43:45.305413-04:00", "main_image": { "id": 552282, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a005000/a005062/20230106_AR13182X12_AIA131_PSF_stamped.000282_print.jpg", "filename": "20230106_AR13182X12_AIA131_PSF_stamped.000282_print.jpg", "media_type": "Image", "alt_text": "The X1.2 flare event of January 6, 2023 as seen in the SDO AIA 131 angstrom filter. The dark region around the central 'X' marking the flare is an artifact of the PSF correction. 'Flickering' in the images around the flare are created due to the 'flare mode' images which have a shorter exposure. Normalizing the solar disk to the same brightness in these frames enhances the background noise off the solar disk.", "width": 1024, "height": 1024, "pixels": 1048576 } } }, { "id": 410391, "type": "details_page", "extra_data": null, "instance": { "id": 5055, "url": "https://svs.gsfc.nasa.gov/5055/", "page_type": "Visualization", "title": "A Cluster of M-class solar flares from Active Region 13165", "description": "Solar Dynamics Observatory (SDO) operates in a geosynchronous orbit around Earth to obtain a continuous view of the Sun. The particular instrument in this visualization records imagery in the ultraviolet portion of the spectrum at wavelengths normally absorbed by Earth's atmosphere - so we need to observe them from space.Here, Active Region 13165 (lower right of solar disk) fires of a cluster of M-class flares over a couple of days in mid-December 2022 (Solar Flares: What does it take to be X-class?). The point-spread function correction (PSF) has been applied to all the imagery on this page. An M6.3 flare erupts followed shortly by a smaller M3.2 flare. || ", "release_date": "2023-01-10T12:00:00-05:00", "update_date": "2023-05-03T11:43:46.936774-04:00", "main_image": { "id": 551835, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a005000/a005055/20221214_AR13165M06_AIA131_PSF_stamped.000222_print.jpg", "filename": "20221214_AR13165M06_AIA131_PSF_stamped.000222_print.jpg", "media_type": "Image", "alt_text": "The double flare event (M6.3 & M 3.2) of December 14, 2022 as seen in the SDO AIA 131 angstrom filter. The dark region around the central 'X' marking the flare is an artifact of the PSF correction. 'Flickering' in the images around the flare are created due to the 'flare mode' images which have a shorter exposure. Normalizing the solar disk to the same brightness in these frames enhances the background noise off the solar disk.", "width": 1024, "height": 1024, "pixels": 1048576 } } }, { "id": 410392, "type": "details_page", "extra_data": null, "instance": { "id": 5109, "url": "https://svs.gsfc.nasa.gov/5109/", "page_type": "Visualization", "title": "M-flare Saturday - a group of M-flares for the Weekend - May 20, 2023", "description": "Solar Dynamics Observatory (SDO) operates in a geosynchronous orbit around Earth to obtain a continuous view of the Sun. The particular instrument in this visualization records imagery in the ultraviolet portion of the spectrum at wavelengths normally absorbed by Earth's atmosphere - so we need to observe them from space.On Saturday May 20, 2023, a battery of multiple M-class flares erupted from two active regions (AR 13311 and AR 13312) near the left limb of the Sun. For more information on the classification of solar flares, see Solar Flares: What Does It Take to Be X-Class? or X-Class: A Guide to Solar Flares. The point-spread function correction (PSF) has been applied to all this imagery. || ", "release_date": "2023-06-27T00:00:00-04:00", "update_date": "2023-06-22T08:50:20.839135-04:00", "main_image": { "id": 856294, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a005100/a005109/20230520_MFlareSaturday_AIA131_PSF_stamped.000418_print.jpg", "filename": "20230520_MFlareSaturday_AIA131_PSF_stamped.000418_print.jpg", "media_type": "Image", "alt_text": "Multiple M-flares erupt during May 20, 2023 in this view through the SDO/AIA 131 angstrom filter.", "width": 1024, "height": 1024, "pixels": 1048576 } } } ], "extra_data": {} }, { "id": 371268, "url": "https://svs.gsfc.nasa.gov/gallery/sdo4k-content/#media_group_371268", "widget": "Tile gallery", "title": "2022", "caption": "", "description": "", "items": [ { "id": 410393, "type": "details_page", "extra_data": null, "instance": { "id": 5016, "url": "https://svs.gsfc.nasa.gov/5016/", "page_type": "Visualization", "title": "A Small (M5) but Complex flare from Active Region 13141", "description": "Solar Dynamics Observatory (SDO) operates in a geosynchronous orbit around Earth to obtain a continuous view of the Sun. The particular instrument in this visualization records imagery in the ultraviolet portion of the spectrum at wavelengths normally absorbed by Earth's atmosphere - so we need to observe them from space.Here, Active Region 13141 (upper left of solar disk) erupts with a class M5.2 solar flare (more visible in the 304 angstrom image) and a thin stream of plasma. || ", "release_date": "2022-11-25T00:00:00-05:00", "update_date": "2023-05-03T11:43:50.839228-04:00", "main_image": { "id": 369713, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a005000/a005016/20221107_AR13141M05_AIA171_PSF_stamped.000210_print.jpg", "filename": "20221107_AR13141M05_AIA171_PSF_stamped.000210_print.jpg", "media_type": "Image", "alt_text": "The slow build-up of a solar active region erupts with an M5.2 flare and ejection of some solar material, as seen in AIA 171 Angstrom filter. The actual flare is more visible in AIA304 below. Correction is applied for the instrument Point-Spread Function (PSF).", "width": 1024, "height": 1024, "pixels": 1048576 } } }, { "id": 410394, "type": "details_page", "extra_data": null, "instance": { "id": 5102, "url": "https://svs.gsfc.nasa.gov/5102/", "page_type": "Visualization", "title": "When Coronal Holes are Smiling.... - October 26, 2022", "description": "Solar Dynamics Observatory (SDO) operates in a geosynchronous orbit around Earth to obtain a continuous view of the Sun. The particular instrument in this visualization records imagery in the ultraviolet portion of the spectrum at wavelengths normally absorbed by Earth's atmosphere - so we need to observe them from space.In another example of pareidolia (Wikipedia) we have what appears to be a smiling face in the SDO/AIA 193 Angstrom filters formed by the arrangement of the darker coronal holes. Coronal holes form at the footpoints of open magnetic field lines which form a 'fast track' for the outflowing solar wind. These 'open' field lines do not connect back to the Sun but instead reach out to the heliopause and interstellar medium. The fast solar wind has an average speed of about 750 kilometers per second, compared to the slow solar wind with speeds from 300 to 500 kilometers per second.For comparison, we include the same time frame from the AIA 171 Angstrom filter where the 'face' is much less pronounced. || ", "release_date": "2023-05-11T12:00:00-04:00", "update_date": "2025-01-06T00:37:02.824441-05:00", "main_image": { "id": 855157, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a005100/a005102/20221026_FlybySmile_AIA193_PSF_stamped.000994_print.jpg", "filename": "20221026_FlybySmile_AIA193_PSF_stamped.000994_print.jpg", "media_type": "Image", "alt_text": "Several solar coronal holes are visible in an entertaining configuration in this SDO imagery taken from the AIA camera with the 193 Angstrom filter.", "width": 1024, "height": 1024, "pixels": 1048576 } } }, { "id": 410395, "type": "details_page", "extra_data": null, "instance": { "id": 5042, "url": "https://svs.gsfc.nasa.gov/5042/", "page_type": "Visualization", "title": "Solar X-Flare - October 2, 2022 (X1.0 class)", "description": "Solar Dynamics Observatory (SDO) operates in a geosynchronous orbit around Earth to obtain a continuous view of the Sun. The particular instrument in this visualization records imagery in the ultraviolet portion of the spectrum at wavelengths normally absorbed by Earth's atmosphere - so we need to observe them from space.Here we have multi-wavelength views of an X1.0 class flare from early October 2022 (upper right of image). Solar flares are classified by the amount of energy released (Solar Flares: What Does It Take to Be X-Class?). Several long filaments or prominences (the dark ribbons) meander across the lower hemisphere. || ", "release_date": "2022-10-21T00:00:00-04:00", "update_date": "2023-05-03T11:43:55.213489-04:00", "main_image": { "id": 371373, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a005000/a005042/20221002_AR13110X10_AIA131_PSF_stamped.000738_print.jpg", "filename": "20221002_AR13110X10_AIA131_PSF_stamped.000738_print.jpg", "media_type": "Image", "alt_text": "The solar flare as seen in AIA 131 Angstrom filter. Correction is applied for the instrument Point-Spread Function (PSF). The dark area around the flare event is an artifact of the point-spread function correction process.", "width": 1024, "height": 1024, "pixels": 1048576 } } }, { "id": 410396, "type": "details_page", "extra_data": null, "instance": { "id": 14202, "url": "https://svs.gsfc.nasa.gov/14202/", "page_type": "Produced Video", "title": "A Week Filled with Flares, August 2022", "description": "The Solar Dynamics Observatory (SDO) spotted 11 significant flares on the Sun from August 12-18, 2022. Here's what that looked like at 171 angstroms, one of the wavelengths of light that SDO captures.Credit: NASA's Goddard Space Flight Center/SDOMusic: \"Rhombus\" from Geometric Shapes. Written and produced by Lars Leonhard.Watch this video on the NASA Goddard YouTube channel.Complete transcript available. || Flare_Week_Still_1_print.jpg (1024x576) [359.4 KB] || Flare_Week_Still_1.jpg (3840x2160) [2.6 MB] || Flare_Week_Still_1_searchweb.png (320x180) [77.4 KB] || Flare_Week_Still_1_thm.png (80x40) [6.3 KB] || 14202_Flare_Week_August2022_1080.mp4 (1920x1080) [359.6 MB] || 14202_Flare_Week_August2022_1080.webm (1920x1080) [25.0 MB] || 14202_Flare_Week_August2022_ProRes_3840x2160_2997.mov (3840x2160) [12.1 GB] || 14202_Flare_Week_August2022_4k_best.mp4 (3840x2160) [1.1 GB] || 14202_Flare_Week_August2022_4k.mp4 (3840x2160) [453.5 MB] || 14202_Flare_Week_SRT_Captions.en_US.srt [2.2 KB] || 14202_Flare_Week_SRT_Captions.en_US.vtt [2.2 KB] || ", "release_date": "2022-09-01T10:00:00-04:00", "update_date": "2023-05-03T11:44:01.124218-04:00", "main_image": { "id": 369538, "url": "https://svs.gsfc.nasa.gov/vis/a010000/a014200/a014202/Flare_Week_Still_1_print.jpg", "filename": "Flare_Week_Still_1_print.jpg", "media_type": "Image", "alt_text": "The Solar Dynamics Observatory (SDO) spotted 11 significant flares on the Sun from August 12-18, 2022. Here's what that looked like at 171 angstroms, one of the wavelengths of light that SDO captures.Credit: NASA's Goddard Space Flight Center/SDOMusic: \"Rhombus\" from Geometric Shapes. Written and produced by Lars Leonhard.Watch this video on the NASA Goddard YouTube channel.Complete transcript available.", "width": 1024, "height": 576, "pixels": 589824 } } }, { "id": 410397, "type": "details_page", "extra_data": null, "instance": { "id": 14163, "url": "https://svs.gsfc.nasa.gov/14163/", "page_type": "Produced Video", "title": "Sun Produces Sparkling Flare on May 19, 2022", "description": "Video of the May 19th M5.6 solar flare captured by SDO in 171 angstrom light. This view shows the full solar disk and an inset focusing on the region where the flare occured.Credit: NASA/GSFC/SDO || May_19_Flare_inset_video_STILL.jpg (1920x1080) [397.3 KB] || May_19_Flare_inset_video_STILL_searchweb.png (320x180) [87.4 KB] || May_19_Flare_inset_video_STILL_thm.png (80x40) [7.5 KB] || May_19_M5pt6_Flare_171_inset_video_1.mp4 (1920x1080) [49.7 MB] || May_19_M5pt6_Flare_171_inset_video_1.webm (1920x1080) [1.8 MB] || May_19_M5pt6_Flare_171_inset_ProRes_1920x1080.mov (1920x1080) [278.1 MB] || ", "release_date": "2022-05-26T00:00:00-04:00", "update_date": "2023-05-03T11:44:09.017741-04:00", "main_image": { "id": 371020, "url": "https://svs.gsfc.nasa.gov/vis/a010000/a014100/a014163/May_19_Flare_inset_video_STILL.jpg", "filename": "May_19_Flare_inset_video_STILL.jpg", "media_type": "Image", "alt_text": "Video of the May 19th M5.6 solar flare captured by SDO in 171 angstrom light. This view shows the full solar disk and an inset focusing on the region where the flare occured.Credit: NASA/GSFC/SDO", "width": 1920, "height": 1080, "pixels": 2073600 } } }, { "id": 410398, "type": "details_page", "extra_data": null, "instance": { "id": 5008, "url": "https://svs.gsfc.nasa.gov/5008/", "page_type": "Visualization", "title": "A Peek from SDO: An Eruption on the Solar Limb", "description": "Solar Dynamics Observatory (SDO) operates in a geosynchronous orbit around Earth to obtain a continuous view of the Sun. The particular instrument in this visualization records imagery in the ultraviolet portion of the spectrum at wavelengths normally absorbed by Earth's atmosphere - so we need to observe them from space.A large eruption occurs off the limb of the Sun (lower right) in this image sequence from May 2022. || ", "release_date": "2022-08-19T00:00:00-04:00", "update_date": "2025-01-06T00:24:45.810865-05:00", "main_image": { "id": 370806, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a005000/a005008/20220519_AR13007Erupt_AIA304_PSF_stamped.000260_print.jpg", "filename": "20220519_AR13007Erupt_AIA304_PSF_stamped.000260_print.jpg", "media_type": "Image", "alt_text": "The solar flare as seen in AIA 304 Angstrom filter. Correction is applied for the instrument Point-Spread Function (PSF).", "width": 1024, "height": 1024, "pixels": 1048576 } } }, { "id": 410399, "type": "details_page", "extra_data": null, "instance": { "id": 14160, "url": "https://svs.gsfc.nasa.gov/14160/", "page_type": "Produced Video", "title": "Sun Emits X1.5 Flare on May 10, 2022", "description": "Short video of the X1.5 flare emitted by the Sun on May 10, 2022 and captured by the Solar Dynamics Observatory in three wavelengths of extreme ultraviolet light that highlight different temperatures and features of the Sun's atmosphere, the corona.Credit: NASA/GSFC/SDOMusic: \"Examples\" from Universal Production MusicComplete transcript available. || May102022_X1pt5Flare_171-131-304.jpg (1920x1080) [979.2 KB] || May102022_X1pt5Flare_171-131-304_searchweb.png (320x180) [55.6 KB] || May102022_X1pt5Flare_171-131-304_thm.png (80x40) [4.4 KB] || 14160_May102022_X1pt5_Flare_ProRes_1920x1080_2997.mov (1920x1080) [829.3 MB] || 14160_May102022_X1pt5_Flare_Best_1080.mp4 (1920x1080) [138.6 MB] || 14160_May102022_X1pt5_Flare_1080.mp4 (1920x1080) [57.0 MB] || 14160_May102022_X1pt5_Flare_ProRes_1920x1080_2997.webm (1920x1080) [5.6 MB] || 14160_May102022_X1pt5_Flare_SRT_Captions.en_US.srt [547 bytes] || 14160_May102022_X1pt5_Flare_SRT_Captions.en_US.vtt [560 bytes] || ", "release_date": "2022-05-21T13:00:00-04:00", "update_date": "2023-05-03T11:44:09.206678-04:00", "main_image": { "id": 371103, "url": "https://svs.gsfc.nasa.gov/vis/a010000/a014100/a014160/May102022_X1pt5Flare_171-131-304.jpg", "filename": "May102022_X1pt5Flare_171-131-304.jpg", "media_type": "Image", "alt_text": "Short video of the X1.5 flare emitted by the Sun on May 10, 2022 and captured by the Solar Dynamics Observatory in three wavelengths of extreme ultraviolet light that highlight different temperatures and features of the Sun's atmosphere, the corona.Credit: NASA/GSFC/SDOMusic: \"Examples\" from Universal Production MusicComplete transcript available.", "width": 1920, "height": 1080, "pixels": 2073600 } } }, { "id": 410400, "type": "details_page", "extra_data": null, "instance": { "id": 5005, "url": "https://svs.gsfc.nasa.gov/5005/", "page_type": "Visualization", "title": "Solar X1.5 flare - May 10, 2022", "description": "Solar Dynamics Observatory (SDO) operates in a geosynchronous orbit around Earth to obtain a continuous view of the Sun. The particular instrument in this visualization records imagery in the ultraviolet portion of the spectrum at wavelengths normally absorbed by Earth's atmosphere - so we need to observe them from space.This imagery is focused on an X1.5 flare on May 10, 2022. || ", "release_date": "2022-08-19T00:00:00-04:00", "update_date": "2023-05-03T11:44:02.764978-04:00", "main_image": { "id": 370964, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a005000/a005005/20220510_FlareX15_AIA304_noPSF_stamped.000290_print.jpg", "filename": "20220510_FlareX15_AIA304_noPSF_stamped.000290_print.jpg", "media_type": "Image", "alt_text": "The solar flare as seen in AIA 304 Angstrom filter. No correction is applied for the instrument Point-Spread Function (PSF).", "width": 1024, "height": 1024, "pixels": 1048576 } } }, { "id": 410401, "type": "details_page", "extra_data": null, "instance": { "id": 5000, "url": "https://svs.gsfc.nasa.gov/5000/", "page_type": "Visualization", "title": "Solar X-flare. May 3, 2022", "description": "Solar Dynamics Observatory (SDO) operates in a geosynchronous orbit around Earth to obtain a continuous view of the Sun. The particular instrument in this visualization records imagery in the ultraviolet portion of the spectrum at wavelengths normally absorbed by Earth's atmosphere - so we need to observe them from space.These imagery cover the time frame of an X1.1 flare (lower left). || ", "release_date": "2022-08-19T00:00:00-04:00", "update_date": "2023-05-03T11:44:02.594503-04:00", "main_image": { "id": 371306, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a005000/a005000/20220503_AR12994X11_AIA131_noPSF_stamped.000428_print.jpg", "filename": "20220503_AR12994X11_AIA131_noPSF_stamped.000428_print.jpg", "media_type": "Image", "alt_text": "The solar flare as seen in AIA 131 Angstrom filter. No correction is applied for the instrument Point-Spread Function (PSF).", "width": 1024, "height": 1024, "pixels": 1048576 } } }, { "id": 410402, "type": "details_page", "extra_data": null, "instance": { "id": 4999, "url": "https://svs.gsfc.nasa.gov/4999/", "page_type": "Visualization", "title": "Solar X-Flare - April 20, 2022 (X2.2 class)", "description": "Solar Dynamics Observatory (SDO) operates in a geosynchronous orbit around Earth to obtain a continuous view of the Sun. The particular instrument in this visualization records imagery in the ultraviolet portion of the spectrum at wavelengths normally absorbed by Earth's atmosphere - so we need to observe them from space.An X2.2 class solar flare erupts on the southern limb of the Sun in the early hours of April 20, 2022. This flare is very close to the lower right of the solar limb and most visible in the 131 Angstrom filter (teal color table). Solar flares are classified by the amount of energy released (Solar Flares: What Does It Take to Be X-Class?) || ", "release_date": "2022-09-22T00:00:00-04:00", "update_date": "2025-01-06T00:24:29.347558-05:00", "main_image": { "id": 371240, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a004900/a004999/20220420_AR12992X22_AIA171_PSF_stamped.000390_print.jpg", "filename": "20220420_AR12992X22_AIA171_PSF_stamped.000390_print.jpg", "media_type": "Image", "alt_text": "The solar flare as seen in the SDO AIA 171 Angstrom filter. Correction has been applied for the instrument point-spread-function (PSF).", "width": 1024, "height": 1024, "pixels": 1048576 } } }, { "id": 410403, "type": "details_page", "extra_data": null, "instance": { "id": 5015, "url": "https://svs.gsfc.nasa.gov/5015/", "page_type": "Visualization", "title": "A Small (M5) Flare from Active Region 13078", "description": "Solar Dynamics Observatory (SDO) operates in a geosynchronous orbit around Earth to obtain a continuous view of the Sun. The particular instrument in this visualization records imagery in the ultraviolet portion of the spectrum at wavelengths normally absorbed by Earth's atmosphere - so we need to observe them from space.These movies were generated around a small M5 class solar flare that occurred on April 17, 2022 near the center of the lower hemisphere || ", "release_date": "2022-08-25T00:00:00-04:00", "update_date": "2023-05-03T11:44:01.688515-04:00", "main_image": { "id": 369683, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a005000/a005015/20220816_AR13078M05_AIA171.PSF_002890_print.jpg", "filename": "20220816_AR13078M05_AIA171.PSF_002890_print.jpg", "media_type": "Image", "alt_text": "The M5 solar flare (lower center of solar disk) as seen in AIA 171 Angstrom filter. Correction is applied for the instrument Point-Spread Function (PSF).", "width": 1024, "height": 1024, "pixels": 1048576 } } }, { "id": 410404, "type": "details_page", "extra_data": null, "instance": { "id": 4998, "url": "https://svs.gsfc.nasa.gov/4998/", "page_type": "Visualization", "title": "Solar X-flare - April 17, 2022. Active Region 12994, X1.1", "description": "Solar Dynamics Observatory (SDO) operates in a geosynchronous orbit around Earth to obtain a continuous view of the Sun. The particular instrument in this visualization records imagery in the ultraviolet portion of the spectrum at wavelengths normally absorbed by Earth's atmosphere - so we need to observe them from space.These movies were generated around an X1.1 class solar flare that occurred on April 17, 2022. || ", "release_date": "2022-08-19T00:00:00-04:00", "update_date": "2025-02-02T22:56:54.929307-05:00", "main_image": { "id": 371185, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a004900/a004998/Flares_AIA171_PSF_stamped.000330_print.jpg", "filename": "Flares_AIA171_PSF_stamped.000330_print.jpg", "media_type": "Image", "alt_text": "The solar flare as seen in AIA 171 Angstrom filter. Correction is applied for the instrument Point-Spread Function (PSF).", "width": 1024, "height": 1024, "pixels": 1048576 } } }, { "id": 410405, "type": "details_page", "extra_data": null, "instance": { "id": 4966, "url": "https://svs.gsfc.nasa.gov/4966/", "page_type": "Visualization", "title": "AR 12938 - Slow Building Active Region on Left Limb", "description": "The slow build-up of a solar active region, as seen in AIA 171 Angstrom filter. 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Correction is applied for the instrument Point-Spread Function (PSF).", "width": 1024, "height": 1024, "pixels": 1048576 } } } ], "extra_data": {} }, { "id": 371269, "url": "https://svs.gsfc.nasa.gov/gallery/sdo4k-content/#media_group_371269", "widget": "Card gallery", "title": "2021", "caption": "", "description": "", "items": [ { "id": 410406, "type": "details_page", "extra_data": null, "instance": { "id": 13982, "url": "https://svs.gsfc.nasa.gov/13982/", "page_type": "Produced Video", "title": "Active October Sun Emits X-class Flare", "description": "Brighter than a shimmering ghost, faster than the flick of a black cat’s tail, the Sun cast a spell in our direction, just in time for Halloween. This imagery captured by NASA’s Solar Dynamics Observatory covers a busy few days of activity between Oct. 25-28 that ended with a significant solar flare. From late afternoon Oct. 25 through mid-morning Oct. 26, an active region on the left limb of the Sun flickered with a series of small flares and petal-like eruptions of solar material. Meanwhile, the Sun was sporting more active regions at its lower center, directly facing Earth. On Oct. 28, the biggest of these released a significant flare, which peaked at 11:35 a.m. EDT. Credit: NASA/GSFC/SDOMusic: \"Immersion\" from Above and Below. Written and produced by Lars LeonhardWatch this video on the NASA Goddard YouTube channel.Complete transcript available. || ActiveOctober_Still.jpg (1920x1080) [956.2 KB] || 13982_ActiveOctober_ProRes_1920x1080_2997.mov (1920x1080) [2.4 GB] || 13982_ActiveOctober_1080_Best.mp4 (1920x1080) [436.2 MB] || 13982_ActiveOctober_1080.mp4 (1920x1080) [188.1 MB] || 13982_ActiveOctober_1080_Best.webm (1920x1080) [19.7 MB] || 13982_ActiveOctober_SRT_Captions.en_US.srt [574 bytes] || 13982_ActiveOctober_SRT_Captions.en_US.vtt [587 bytes] || ", "release_date": "2021-10-28T14:00:00-04:00", "update_date": "2023-05-03T13:43:48.345129-04:00", "main_image": { "id": 375678, "url": "https://svs.gsfc.nasa.gov/vis/a010000/a013900/a013982/SDO_X1_Flare_10-28_304-171Blend.jpg", "filename": "SDO_X1_Flare_10-28_304-171Blend.jpg", "media_type": "Image", "alt_text": "An X1.0 class solar flare flashes in center of the Sun on Oct. 28, 2021. This image was captured by NASA's Solar Dynamics Observatory and shows a blend of light from the 171 and 304 angstrom wavelengths.Credit: NASA/GSFC/SDO", "width": 4096, "height": 4096, "pixels": 16777216 } } } ], "extra_data": {} }, { "id": 371270, "url": "https://svs.gsfc.nasa.gov/gallery/sdo4k-content/#media_group_371270", "widget": "Card gallery", "title": "2020", "caption": "", "description": "", "items": [ { "id": 410407, "type": "media_group", "extra_data": null, "title": "Solar Activity Continues to Rise with 'Anemone' Eruption", "caption": "This imagery captured by NASA’s Solar Dynamics Observatory shows a solar flare and a subsequent eruption of solar material that occurred over the left limb of the Sun on November 29, 2020. From its foot point over the limb, some of the light and energy was blocked from reaching Earth – a little like seeing light from a lightbulb with the bottom half covered up. \r\n\r\nAlso visible in the imagery is an eruption of solar material that achieved escape velocity and moved out into space as a giant cloud of gas and magnetic fields known as a coronal mass ejection, or CME. A third, but invisible, feature of such eruptive events also blew off the Sun: a swarm of fast-moving solar energetic particles. Such particles are guided by the magnetic fields streaming out from the Sun, which, due to the Sun’s constant rotation, point backwards in a big spiral much the way water comes out of a spinning sprinkler. The solar energetic particles, therefore, emerging as they did from a part of the Sun not yet completely rotated into our view, traveled along that magnetic spiral away from Earth toward the other side of the Sun. \r\n\r\nWhile the solar material didn’t head toward Earth, it did pass by some spacecraft: NASA’s Parker Solar Probe, NASA’s STEREO and ESA/NASA’s Solar Orbiter. Equipped to measure magnetic fields and the particles that pass over them, we may be able to study fast-moving solar energetic particles in the observations once they are downloaded. These sun-watching missions are all part of a larger heliophysics fleet that help us understand both what causes such eruptions on the Sun -- as well as how solar activity affects interplanetary space, including near Earth, where they have the potential to affect astronauts and satellites.", "instance": { "id": 380813, "url": "https://svs.gsfc.nasa.gov/vis/a010000/a013700/a013778/Anemone_Eruption_131-171_Blend_searchweb.png", "filename": "Anemone_Eruption_131-171_Blend_searchweb.png", "media_type": "Image", "alt_text": "This imagery captured by NASA’s Solar Dynamics Observatory shows a solar flare and a subsequent eruption of solar material that occurred over the left limb of the Sun on November 29, 2020. From its foot point over the limb, some of the light and energy was blocked from reaching Earth – a little like seeing light from a lightbulb with the bottom half covered up. \r\n\r\nAlso visible in the imagery is an eruption of solar material that achieved escape velocity and moved out into space as a giant cloud of gas and magnetic fields known as a coronal mass ejection, or CME. A third, but invisible, feature of such eruptive events also blew off the Sun: a swarm of fast-moving solar energetic particles. Such particles are guided by the magnetic fields streaming out from the Sun, which, due to the Sun’s constant rotation, point backwards in a big spiral much the way water comes out of a spinning sprinkler. The solar energetic particles, therefore, emerging as they did from a part of the Sun not yet completely rotated into our view, traveled along that magnetic spiral away from Earth toward the other side of the Sun. \r\n\r\nWhile the solar material didn’t head toward Earth, it did pass by some spacecraft: NASA’s Parker Solar Probe, NASA’s STEREO and ESA/NASA’s Solar Orbiter. Equipped to measure magnetic fields and the particles that pass over them, we may be able to study fast-moving solar energetic particles in the observations once they are downloaded. These sun-watching missions are all part of a larger heliophysics fleet that help us understand both what causes such eruptions on the Sun -- as well as how solar activity affects interplanetary space, including near Earth, where they have the potential to affect astronauts and satellites.", "width": 180, "height": 320, "pixels": 57600 } }, { "id": 410408, "type": "details_page", "extra_data": null, "instance": { "id": 4854, "url": "https://svs.gsfc.nasa.gov/4854/", "page_type": "Visualization", "title": "Coronal Holes at Solar Minimum and Solar Maximum", "description": "A sample of solar coronal holes around the time of the maximum of sunspot activity (April 2014). Note the polar regions are devoid of coronal holes but a large hole appears in the southern hemisphere. || CoronalHoleMax_AIA193_00150_print.jpg (1024x1024) [173.1 KB] || CoronalHoleMax_AIA193_00150_searchweb.png (320x180) [89.6 KB] || CoronalHoleMax_AIA193_00150_thm.png (80x40) [7.4 KB] || CoronalHoleMax_AIA193_2048p30.mp4 (2048x2048) [61.7 MB] || CoronalHoleMax_AIA193_2048p30.webm (2048x2048) [2.9 MB] || AIA193-Time (4096x4096) [64.0 KB] || AIA193-Frames (4096x4096) [64.0 KB] || CoronalHoleMax_Timestamp (600x100) [64.0 KB] || ", "release_date": "2020-09-15T10:00:00-04:00", "update_date": "2023-05-03T13:44:42.633288-04:00", "main_image": { "id": 382963, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a004800/a004854/CoronalHoleMax_AIA193_00150_print.jpg", "filename": "CoronalHoleMax_AIA193_00150_print.jpg", "media_type": "Image", "alt_text": "A sample of solar coronal holes around the time of the maximum of sunspot activity (April 2014). Note the polar regions are devoid of coronal holes but a large hole appears in the southern hemisphere.", "width": 1024, "height": 1024, "pixels": 1048576 } } }, { "id": 410409, "type": "details_page", "extra_data": null, "instance": { "id": 4776, "url": "https://svs.gsfc.nasa.gov/4776/", "page_type": "Visualization", "title": "Ten Years of Solar Dynamics Observatory", "description": "Ten years of SDO AIA 171 angstrom data with day time stamp overlay. Frames are sampled approximately one image every hour. || SDOat10_AIA171_stand.UHD2160.01500_print.jpg (1024x576) [47.4 KB] || SDOat10_AIA171_stand.UHD2160.01500_searchweb.png (320x180) [40.9 KB] || SDOat10_AIA171_stand.UHD2160.01500_thm.png (80x40) [4.0 KB] || SDOat10_AIA171.1080p30.webm (1920x1080) [348.5 MB] || SDOat10_AIA171.baseimage (3840x2160) [0 Item(s)] || SDOat10_AIA171.1080p30.mp4 (1920x1080) [3.9 GB] || SDOat10_AIA171.UHD2160_p30.mp4 (3840x2160) [13.0 GB] || SDOat10_AIA171.1080p30.mp4.hwshow [188 bytes] || ", "release_date": "2020-06-24T10:00:00-04:00", "update_date": "2025-01-06T00:15:33.638324-05:00", "main_image": { "id": 388504, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a004700/a004776/SDOat10_AIA171.01500_print.jpg", "filename": "SDOat10_AIA171.01500_print.jpg", "media_type": "Image", "alt_text": "Ten years of SDO AIA 171 angstrom data, 4Kx4K with color table. Frames are sampled approximately one image every hour.", "width": 1024, "height": 1024, "pixels": 1048576 } } } ], "extra_data": {} }, { "id": 371271, "url": "https://svs.gsfc.nasa.gov/gallery/sdo4k-content/#media_group_371271", "widget": "Card gallery", "title": "2019", "caption": "", "description": "", "items": [ { "id": 410410, "type": "details_page", "extra_data": null, "instance": { "id": 4763, "url": "https://svs.gsfc.nasa.gov/4763/", "page_type": "Visualization", "title": "Mercury Transit, 2019 (SDO 4K imagery)", "description": "Mercury transit visible through the 171 angstrom filter on SDO. || AIA171_00025_print.jpg (1024x1024) [108.7 KB] || AIA171_00025_searchweb.png (320x180) [65.6 KB] || AIA171_00025_thm.png (80x40) [5.2 KB] || AIA171_2048p30.mp4 (2048x2048) [19.2 MB] || AIA171_1024p30.mp4 (1024x1024) [3.7 MB] || AIA171-Frames (4096x4096) [0 Item(s)] || AIA171-Time (4096x4096) [0 Item(s)] || AIA171_4096p30_h265.mp4 (4096x4096) [13.6 MB] || AIA171_4096p30_h265.webm (4096x4096) [2.7 MB] || ", "release_date": "2019-11-11T16:30:00-05:00", "update_date": "2025-02-02T22:42:44.095832-05:00", "main_image": { "id": 391227, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a004700/a004763/AIA171_00025_print.jpg", "filename": "AIA171_00025_print.jpg", "media_type": "Image", "alt_text": "Mercury transit visible through the 171 angstrom filter on SDO.", "width": 1024, "height": 1024, "pixels": 1048576 } } }, { "id": 410411, "type": "details_page", "extra_data": null, "instance": { "id": 4761, "url": "https://svs.gsfc.nasa.gov/4761/", "page_type": "Visualization", "title": "New sites for magnetic reconnection", "description": "HD and UHD movie views of the plasma flowing along magnetic fields lines visible at 171Å. || May2012_Reconn_171A_stand.HD1080i.00951_print.jpg (1024x576) [52.0 KB] || May2012_Reconn_171A_stand.HD1080i.00951_searchweb.png (320x180) [43.5 KB] || May2012_Reconn_171A_stand.HD1080i.00951_thm.png (80x40) [4.2 KB] || AIA171A (1920x1080) [0 Item(s)] || May2012_Reconn_171A.HD1080i_p30.mp4 (1920x1080) [21.9 MB] || May2012_Reconn_171A.HD1080i_p30.webm (1920x1080) [7.0 MB] || AIA171A (3840x2160) [0 Item(s)] || May2012_Reconn_171A_2160p30.mp4 (3840x2160) [107.3 MB] || May2012_Reconn_171A.HD1080i_p30.mp4.hwshow [197 bytes] || ", "release_date": "2019-12-17T10:00:00-05:00", "update_date": "2025-01-06T00:15:05.590503-05:00", "main_image": { "id": 391680, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a004700/a004761/May2012_Reconn_171A.00951_print.jpg", "filename": "May2012_Reconn_171A.00951_print.jpg", "media_type": "Image", "alt_text": "4Kx4K frames of the plasma flowing along magnetic fields lines visible at 171Å.", "width": 1024, "height": 1024, "pixels": 1048576 } } } ], "extra_data": {} }, { "id": 371272, "url": "https://svs.gsfc.nasa.gov/gallery/sdo4k-content/#media_group_371272", "widget": "Card gallery", "title": "2018", "caption": "", "description": "", "items": [ { "id": 410412, "type": "details_page", "extra_data": null, "instance": { "id": 4659, "url": "https://svs.gsfc.nasa.gov/4659/", "page_type": "Visualization", "title": "Incredible Solar Flare, Prominence Eruption and CME Event (hydrogen alpha filter)", "description": "This movie is generated from imagery collected by the NSO GONG network of solar observatories. It is not time-synchronized to the related observations by the Solar Dynamics Observatory (SDO). || BBSO_Halpha_2011JuneUh_stand.HD1080i.00187_print.jpg (1024x576) [25.1 KB] || BBSO_Halpha_2011JuneUh_stand.HD1080i.00187_searchweb.png (320x180) [20.9 KB] || BBSO_Halpha_2011JuneUh_stand.HD1080i.00187_thm.png (80x40) [2.3 KB] || 1920x1080_16x9_30p (1920x1080) [0 Item(s)] || BBSO_Halpha_2011JuneUh_HD1080i_p30.mp4 (1920x1080) [2.8 MB] || BBSO_Halpha_2011JuneUh_HD1080i_p30.webm (1920x1080) [1.2 MB] || 3840x2160_16x9_30p (3840x2160) [0 Item(s)] || BBSO_Halpha_2011JuneUh_2160p30.mp4 (3840x2160) [11.4 MB] || BBSO_Halpha_2011JuneUh_HD1080i_p30.mp4.hwshow [200 bytes] || ", "release_date": "2018-06-27T00:00:00-04:00", "update_date": "2025-02-02T22:38:32.606927-05:00", "main_image": { "id": 402596, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a004600/a004659/BBSO_Halpha_2011JuneUh.00187_print.jpg", "filename": "BBSO_Halpha_2011JuneUh.00187_print.jpg", "media_type": "Image", "alt_text": "This movie is generated by the raw 2Kx2K imagery. Frames are available as sequentially numbered or time-stamp in file name.", "width": 1024, "height": 1024, "pixels": 1048576 } } } ], "extra_data": {} }, { "id": 371273, "url": "https://svs.gsfc.nasa.gov/gallery/sdo4k-content/#media_group_371273", "widget": "Card gallery", "title": "2017", "caption": "", "description": "", "items": [ { "id": 410413, "type": "details_page", "extra_data": null, "instance": { "id": 4491, "url": "https://svs.gsfc.nasa.gov/4491/", "page_type": "Visualization", "title": "The X8.2 Flare of September 2017, as Seen by SDO", "description": "40 hours of AIA 131 angstrom imager at 12 second cadence viewing the time around the X8.2 solar flare. || Sept2017_X8Flare_131A_stand.UHD3840.07800_print.jpg (1024x576) [61.1 KB] || AIA131A (1920x1080) [0 Item(s)] || Sept2017_X8Flare_131A.HD1080i_p30.webm (1920x1080) [47.6 MB] || Sept2017_X8Flare_131A.HD1080i_p30.mp4 (1920x1080) [843.8 MB] || AIA131A (3840x2160) [0 Item(s)] || Sept2017_X8Flare_131A.HD1080i_p30.mp4.hwshow || ", "release_date": "2019-05-01T00:00:00-04:00", "update_date": "2025-05-28T00:07:50.233342-04:00", "main_image": { "id": 398032, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a004400/a004491/Sept2017_X8Flare_171A.07800_print.jpg", "filename": "Sept2017_X8Flare_171A.07800_print.jpg", "media_type": "Image", "alt_text": "40 hours of AIA 171 angstrom imager (4Kx4K) at 12 second cadence viewing the time around the X8.2 solar flare.", "width": 1024, "height": 1024, "pixels": 1048576 } } }, { "id": 410414, "type": "details_page", "extra_data": null, "instance": { "id": 12737, "url": "https://svs.gsfc.nasa.gov/12737/", "page_type": "Produced Video", "title": "September Flares 4k", "description": "4k frames and ProRes video from SDO quicklook products. This footage is in 131 angstrom extreme ultraviolet light at approximately 30 second imaging cadence. It covers the time period of 14:59 to 17:00UTC 9/10/2017. || SDO_20170910_131_AR12673X8.00680_print.jpg (1024x1024) [220.6 KB] || SDO_20170910_131_AR12673X8.00680_searchweb.png (180x320) [55.4 KB] || SDO_20170910_131_AR12673X8.00680_thm.png (80x40) [4.7 KB] || SDO_20170910_131_AR12673X8_4k.mov (4096x4096) [958.7 MB] || 131X8 (4096x4096) [16.0 KB] || SDO_20170910_131_AR12673X8_4k.webm (4096x4096) [37.1 MB] || SDO_20170910_131_AR12673X8.00680.tif (4096x4096) [12.7 MB] || ", "release_date": "2017-10-06T11:00:00-04:00", "update_date": "2023-05-03T13:47:18.629698-04:00", "main_image": { "id": 410530, "url": "https://svs.gsfc.nasa.gov/vis/a010000/a012700/a012737/SDO_20170910_131_AR12673X8.00680_print.jpg", "filename": "SDO_20170910_131_AR12673X8.00680_print.jpg", "media_type": "Image", "alt_text": "4k frames and ProRes video from SDO quicklook products. This footage is in 131 angstrom extreme ultraviolet light at approximately 30 second imaging cadence. It covers the time period of 14:59 to 17:00UTC 9/10/2017.", "width": 1024, "height": 1024, "pixels": 1048576 } } }, { "id": 410415, "type": "details_page", "extra_data": null, "instance": { "id": 4551, "url": "https://svs.gsfc.nasa.gov/4551/", "page_type": "Visualization", "title": "A Solar Cycle from Solar Dynamics Observatory", "description": "4K x 4K imagery from the SDO/HMI instrument. || SolarCycleHMI.02000_print.jpg (1024x1024) [154.4 KB] || SolarCycleHMI.02000_searchweb.png (320x180) [50.4 KB] || SolarCycleHMI.02000_thm.png (80x40) [3.7 KB] || SolarCycleHMI_1024p30.mp4 (1024x1024) [333.3 MB] || SolarCycleHMI_1024p30.webm (1024x1024) [19.2 MB] || Intensity-Frames (4096x4096) [512.0 KB] || Intensity-Time (4096x4096) [512.0 KB] || ", "release_date": "2017-02-11T10:00:00-05:00", "update_date": "2024-04-26T05:54:50.546633-04:00", "main_image": { "id": 416836, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a004500/a004551/SolarCycleHMI.02000_print.jpg", "filename": "SolarCycleHMI.02000_print.jpg", "media_type": "Image", "alt_text": "4K x 4K imagery from the SDO/HMI instrument.", "width": 1024, "height": 1024, "pixels": 1048576 } } }, { "id": 410416, "type": "details_page", "extra_data": null, "instance": { "id": 4002, "url": "https://svs.gsfc.nasa.gov/4002/", "page_type": "Visualization", "title": "AR2665: The Lonely Sunspot of Solar Minimum", "description": "Full-disk view of sunspot group moving across the solar disk, AIA 171 ångstrom band. || July2017_AR2665_AIA171_stand.HD1080i.01000_print.jpg (1024x576) [53.8 KB] || AIA171 (1920x1080) [0 Item(s)] || July2017_AR2665_AIA171.HD1080i_p30.mp4 (1920x1080) [53.5 MB] || July2017_AR2665_AIA171.HD1080i_p30.webm (1920x1080) [8.5 MB] || July2017_AR2665_AIA171_2048p30.mp4 (2048x2048) [264.8 MB] || 171A-Frames (4096x4096) [0 Item(s)] || 171A-Time (4096x4096) [0 Item(s)] || July2017_AR2665_AIA171.HD1080i_p30.mp4.hwshow [200 bytes] || ", "release_date": "2017-08-04T10:00:00-04:00", "update_date": "2025-02-02T22:09:18.420764-05:00", "main_image": { "id": 412744, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a004000/a004002/July2017_AR2665_AIA171M24_stand.HD1080i.00500_print.jpg", "filename": "July2017_AR2665_AIA171M24_stand.HD1080i.00500_print.jpg", "media_type": "Image", "alt_text": "M2.4 flare on July 14, 2017 in SDO/AIA 171 ångstrom filter.", "width": 1024, "height": 576, "pixels": 589824 } } } ], "extra_data": {} }, { "id": 371274, "url": "https://svs.gsfc.nasa.gov/gallery/sdo4k-content/#media_group_371274", "widget": "Card gallery", "title": "2016", "caption": "", "description": "", "items": [ { "id": 410417, "type": "details_page", "extra_data": null, "instance": { "id": 4463, "url": "https://svs.gsfc.nasa.gov/4463/", "page_type": "Visualization", "title": "Mercury Transit 2016 from SDO/AIA at 304 Ångstroms", "description": "Composited full-disk imagery sampled at 12 second intervals. || AIA304MercuryComposite.01500_print.jpg (1024x1024) [195.3 KB] || AIA304MercuryComposite.01500_searchweb.png (320x180) [69.7 KB] || AIA304MercuryComposite.01500_thm.png (80x40) [4.7 KB] || AIA304MercuryComposite_2048p30.webm (720x720) [9.5 MB] || AIA304MercuryComposite_2048p30.mp4 (2048x2048) [597.8 MB] || 304A-Frames (4096x4096) [0 Item(s)] || 304A-Time (4096x4096) [0 Item(s)] || ", "release_date": "2016-06-01T10:00:00-04:00", "update_date": "2023-05-03T13:48:34.696523-04:00", "main_image": { "id": 424506, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a004400/a004463/AIA304MercuryComposite.01500_print.jpg", "filename": "AIA304MercuryComposite.01500_print.jpg", "media_type": "Image", "alt_text": "Composited full-disk imagery sampled at 12 second intervals.", "width": 1024, "height": 1024, "pixels": 1048576 } } }, { "id": 410418, "type": "details_page", "extra_data": null, "instance": { "id": 4462, "url": "https://svs.gsfc.nasa.gov/4462/", "page_type": "Visualization", "title": "Mercury Transit 2016 from SDO/AIA at 171 Ångstroms", "description": "Composited full-disk imagery sampled at 12 second intervals. || AIA171MercuryComposite.01500_print.jpg (1024x1024) [187.2 KB] || AIA171MercuryComposite.01500_searchweb.png (320x180) [82.8 KB] || AIA171MercuryComposite.01500_thm.png (80x40) [6.3 KB] || aia171mercurycomposite_2048p30.webm (720x720) [6.6 MB] || AIA171MercuryComposite_2048p30.mp4 (2048x2048) [297.0 MB] || 171A-Frames (4096x4096) [0 Item(s)] || 171A-Time (4096x4096) [0 Item(s)] || ", "release_date": "2016-06-01T10:00:00-04:00", "update_date": "2023-05-03T13:48:34.615140-04:00", "main_image": { "id": 424498, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a004400/a004462/AIA171MercuryComposite.01500_print.jpg", "filename": "AIA171MercuryComposite.01500_print.jpg", "media_type": "Image", "alt_text": "Composited full-disk imagery sampled at 12 second intervals.", "width": 1024, "height": 1024, "pixels": 1048576 } } }, { "id": 410419, "type": "details_page", "extra_data": null, "instance": { "id": 4461, "url": "https://svs.gsfc.nasa.gov/4461/", "page_type": "Visualization", "title": "Mercury Transit 2016 from SDO/HMI", "description": "Full-Disk imagery sampled at 3 second cadence. || HMIMercuryComposite_stand.4Kx4K.04000_print.jpg (1024x1024) [141.4 KB] || HMIMercuryComposite_stand.4Kx4K.04000_searchweb.png (320x180) [50.3 KB] || HMIMercuryComposite_stand.4Kx4K.04000_thm.png (80x40) [3.9 KB] || HMIMercuryComposite_stand.2Kx2Kp30.webm (2048x2048) [30.4 MB] || HMIMercuryComposite_stand.2Kx2Kp30.mp4 (2048x2048) [637.1 MB] || 4096x4096_1x1_30p (4096x4096) [0 Item(s)] || ", "release_date": "2016-06-01T10:00:00-04:00", "update_date": "2023-05-03T13:48:34.525140-04:00", "main_image": { "id": 424493, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a004400/a004461/HMIMercuryComposite_stand.4Kx4K.04000_print.jpg", "filename": "HMIMercuryComposite_stand.4Kx4K.04000_print.jpg", "media_type": "Image", "alt_text": "Full-Disk imagery sampled at 3 second cadence.", "width": 1024, "height": 1024, "pixels": 1048576 } } }, { "id": 410420, "type": "details_page", "extra_data": null, "instance": { "id": 12144, "url": "https://svs.gsfc.nasa.gov/12144/", "page_type": "Produced Video", "title": "SDO: Year 6", "description": "This ultra-high definition (3840x2160) video shows the sun in the 171 angstrom wavelength of extreme ultraviolet light. It covers a time period of January 2, 2015 to January 28, 2016 at a cadence of one frame every hour, or 24 frames per day. This timelapse is repeated with narration by solar scientist Nicholeen Viall and contains close-ups and annotations. 171 angstrom light highlights material around 600,000 Kelvin and shows features in the upper transition region and quiet corona of the sun. The video is available to download here at 59.94 frames per second, double the rate YouTube currently allows for UHD content. The music is titled \"Tides\" and is from Killer Tracks.Watch this video on the NASA Goddard YouTube channel.Complete transcript available. || SDO_Year6_HCblend_HD.png (1920x1080) [5.3 MB] || SDO_Year6_HCblend_HD.jpg (1920x1080) [545.9 KB] || SDO_Year6_HCblend_HD_print.jpg (1024x576) [179.5 KB] || SDO_Year6_HCblend_UHD.png (3840x2160) [19.7 MB] || SDO_Year6_HCblend_UHD.jpg (3840x2160) [1.2 MB] || SDO_Year6_HCblend_HD_searchweb.png (180x320) [59.6 KB] || SDO_Year6_HCblend_HD_thm.png (80x40) [4.8 KB] || 12144_SDO_Year_6_appletv.webm (1280x720) [50.5 MB] || 12144_SDO_Year_6_appletv.m4v (1280x720) [241.9 MB] || 12144_SDO_Year_6_appletv_appletv_subtitles.m4v (1280x720) [242.1 MB] || SDO_Year_6_SRT_Captions.en_US.srt [6.3 KB] || SDO_Year_6_SRT_Captions.en_US.vtt [6.3 KB] || 12144_SDO_Year_6_H264_Good_1920x1080_2997.mov (1920x1080) [1.4 GB] || 12144_SDO_Year_6_H264_Good_3840x2160_2997.mov (3840x2160) [9.1 GB] || 12144_SDO_Year_6_H264_Good_3840x2160_5994.mov (3840x2160) [10.2 GB] || 12144_SDO_Year_6_ProRes_3840x2160_5994.mov (3840x2160) [50.3 GB] || ", "release_date": "2016-02-12T09:00:00-05:00", "update_date": "2023-05-03T13:48:54.988843-04:00", "main_image": { "id": 427343, "url": "https://svs.gsfc.nasa.gov/vis/a010000/a012100/a012144/SDO_Year6_HCblend_HD.png", "filename": "SDO_Year6_HCblend_HD.png", "media_type": "Image", "alt_text": "This ultra-high definition (3840x2160) video shows the sun in the 171 angstrom wavelength of extreme ultraviolet light. It covers a time period of January 2, 2015 to January 28, 2016 at a cadence of one frame every hour, or 24 frames per day. This timelapse is repeated with narration by solar scientist Nicholeen Viall and contains close-ups and annotations. 171 angstrom light highlights material around 600,000 Kelvin and shows features in the upper transition region and quiet corona of the sun. The video is available to download here at 59.94 frames per second, double the rate YouTube currently allows for UHD content. The music is titled \"Tides\" and is from Killer Tracks.Watch this video on the NASA Goddard YouTube channel.Complete transcript available.", "width": 1920, "height": 1080, "pixels": 2073600 } } }, { "id": 410421, "type": "details_page", "extra_data": null, "instance": { "id": 4422, "url": "https://svs.gsfc.nasa.gov/4422/", "page_type": "Visualization", "title": "SDO Year 6: A Year of the Sun", "description": "A year of SDO solar observations in HD1080. || SDOYear6hourly_171A_stand.HD1080i.02000_print.jpg (1024x576) [64.8 KB] || 1920x1080_16x9_30p (1920x1080) [0 Item(s)] || SDOYear6hourly_171A.HD1080.webm (1920x1080) [37.4 MB] || SDOYear6hourly_171A_1080p30.mp4 (1920x1080) [424.4 MB] || SDOYear6hourly_171A.HD1080.mov (1920x1080) [1.1 GB] || SDOYear6hourly_171A_1080p30.mp4.hwshow [193 bytes] || ", "release_date": "2016-02-12T09:30:00-05:00", "update_date": "2025-01-05T22:59:02.965659-05:00", "main_image": { "id": 427543, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a004400/a004422/SDOYear6hourly_171A.04000_print.jpg", "filename": "SDOYear6hourly_171A.04000_print.jpg", "media_type": "Image", "alt_text": "Full disk 4Kx4K frames.", "width": 1024, "height": 1024, "pixels": 1048576 } } } ], "extra_data": {} }, { "id": 371275, "url": "https://svs.gsfc.nasa.gov/gallery/sdo4k-content/#media_group_371275", "widget": "Card gallery", "title": "2015", "caption": "", "description": "", "items": [ { "id": 410422, "type": "details_page", "extra_data": null, "instance": { "id": 11868, "url": "https://svs.gsfc.nasa.gov/11868/", "page_type": "Produced Video", "title": "NASA's SDO Observes a Cinco de Mayo Solar Flare", "description": "Video of May 5, 2015 X2.7 flare.Credit: NASA/GSFC/SDO || May_5_2015_Flare_Still_304-171.png (1920x1080) [8.1 MB] || May_5_2015_Flare_Still_304-171.jpg (1920x1080) [415.9 KB] || May_5_2015_Flare_Still_304-171_print.jpg (1024x576) [145.7 KB] || May_5_2015_Flare_Still_304-171_web.png (320x180) [83.3 KB] || 11868_May_5_X_Flare_MPEG4_1920X1080_2997.mp4 (1920x1080) [42.2 MB] || 11868_May_5_X_Flare_H264_Good_1920x1080_2997.webm (1920x1080) [4.8 MB] || 11868_May_5_X_Flare_1280x720.wmv (1280x720) [23.1 MB] || 11868_May_5_X_Flare_appletv.m4v (960x540) [19.0 MB] || 11868_May_5_X_Flare_appletv_subtitles.m4v (960x540) [19.0 MB] || 11868_May_5_X_Flare_ipod_lg.m4v (640x360) [7.1 MB] || 11868_May_5_X_Flare_ipod_sm.mp4 (320x240) [3.6 MB] || 11868_May_5_X_Flare_SRT_Captions.en_US.srt [230 bytes] || 11868_May_5_X_Flare_SRT_Captions.en_US.vtt [243 bytes] || 11868_May_5_X_Flare_ProRes_1920x1080_2997.mov (1920x1080) [674.9 MB] || 11868_May_5_X_Flare_H264_Best_1920x1080_2997.mov (1920x1080) [682.7 MB] || 11868_May_5_X_Flare_H264_Good_1920x1080_2997.mov (1920x1080) [219.1 MB] || ", "release_date": "2015-05-06T09:45:00-04:00", "update_date": "2024-10-06T23:38:49.781474-04:00", "main_image": { "id": 443402, "url": "https://svs.gsfc.nasa.gov/vis/a010000/a011800/a011868/May_5_2015_Five_Across_no_Labels_print.jpg", "filename": "May_5_2015_Five_Across_no_Labels_print.jpg", "media_type": "Image", "alt_text": "NASA's Solar Dynamics Observatory captured these images of a solar flare – as seen in the bright flash on the left – on May 5, 2015. Each image shows a different wavelength of extreme ultraviolet light that highlights a different temperature of material on the sun. By comparing different images, scientists can better understand the movement of solar matter and energy during a flare. From left to right, the wavelengths are: visible light, 171 angstroms, 304 angstroms, 193 angstroms and 131 angstroms. Each wavelength has been colorized. Unlabeled.Credit: NASA/GSFC/SDO", "width": 1024, "height": 576, "pixels": 589824 } } }, { "id": 410423, "type": "details_page", "extra_data": null, "instance": { "id": 4323, "url": "https://svs.gsfc.nasa.gov/4323/", "page_type": "Visualization", "title": "Summer Sun from SDO: Eruption and Coronal Loops on the Solar Limb", "description": "HD1080 movie of the Sun in the AIA 304 angstrom filter. Note the coronal loop structures on the lower right limb. || June2015LimbLoops_304A_stand.HD1080i.00256_print.jpg (1024x576) [68.0 KB] || June2015LimbLoops_304A_1080p.webm (1920x1080) [5.1 MB] || June2015LimbLoops_304AHD (1920x1080) [128.0 KB] || June2015LimbLoops_304A_1080p.mp4 (1920x1080) [34.7 MB] || June2015LimbLoops_304A.HD1080.mov (1920x1080) [108.5 MB] || June2015LimbLoops_304A_1080p.mp4.hwshow [228 bytes] || ", "release_date": "2016-02-11T00:00:00-05:00", "update_date": "2024-10-09T00:05:26.245792-04:00", "main_image": { "id": 442277, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a004300/a004323/June2015LimbLoops_171A.00992_print.jpg", "filename": "June2015LimbLoops_171A.00992_print.jpg", "media_type": "Image", "alt_text": "The Sun in the AIA 171 angstrom filter. Note the coronal loop structures on the lower right limb.", "width": 1024, "height": 1024, "pixels": 1048576 } } }, { "id": 410424, "type": "details_page", "extra_data": null, "instance": { "id": 4319, "url": "https://svs.gsfc.nasa.gov/4319/", "page_type": "Visualization", "title": "Solar Dynamics Observatory: April 21, 2015 Eruption on the Solar Limb", "description": "Movie of plasma eruption (upper left limb). || Apr2015LimbErupt_304A_stand.HD1080i.00945_print.jpg (1024x576) [73.9 KB] || Apr2015LimbErupt_304A_stand.HD1080i.00945_searchweb.png (320x180) [41.0 KB] || Apr2015LimbErupt_304A_stand.HD1080i.00945_thm.png (80x40) [3.5 KB] || Apr2015LimbErupt_304A_stand_1080p.webm (1920x1080) [6.4 MB] || 1920x1080_16x9_30p (1920x1080) [0 Item(s)] || Apr2015LimbErupt_304A_stand_1080p.mp4 (1920x1080) [43.2 MB] || Apr2015LimbErupt_304A_stand_1080p.mp4.hwshow [199 bytes] || ", "release_date": "2016-02-11T00:00:00-05:00", "update_date": "2025-01-05T22:46:34.235053-05:00", "main_image": { "id": 442483, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a004300/a004319/Apr2015LimbErupt_304A.01000_print.jpg", "filename": "Apr2015LimbErupt_304A.01000_print.jpg", "media_type": "Image", "alt_text": "Full disk 4Kx4K image sequences of SDO/AIA 304 ångstrom filter.", "width": 1024, "height": 1024, "pixels": 1048576 } } } ], "extra_data": {} }, { "id": 371276, "url": "https://svs.gsfc.nasa.gov/gallery/sdo4k-content/#media_group_371276", "widget": "Tile gallery", "title": "2014", "caption": "", "description": "", "items": [ { "id": 410425, "type": "details_page", "extra_data": null, "instance": { "id": 4963, "url": "https://svs.gsfc.nasa.gov/4963/", "page_type": "Visualization", "title": "Fifty Days of Continuous Sun from Solar Dynamics Observatory (171A filter)", "description": "Solar Dynamics Observatory (SDO) operates in a geosynchronous orbit around Earth to obtain a continuous view of the Sun. The particular instrument in this visualization records imagery in the ultraviolet portion of the spectrum at wavelengths normally absorbed by Earth's atmosphere - so we need to observe them from space.This movie was generated as a test case for a new movie pipeline for SDO, here's SDO AIA 171A imagery, sampled every two minutes for 50 days (April 12 through June 3, 2014), resulting in 30 minutes of continuous play (at 20 frames per second). || ", "release_date": "2022-08-19T00:00:00-04:00", "update_date": "2023-05-03T11:44:02.180193-04:00", "main_image": { "id": 373827, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a004900/a004963/ExtendedRun_AIA171_PSF_stamped.005000_print.jpg", "filename": "ExtendedRun_AIA171_PSF_stamped.005000_print.jpg", "media_type": "Image", "alt_text": "Fifty days of continuous SDO/AIA 171 angstrom filter day, at two minute cadence. This version has the point-spread-function (PSF) correction applied and date-stamp.", "width": 1024, "height": 1024, "pixels": 1048576 } } }, { "id": 410426, "type": "details_page", "extra_data": null, "instance": { "id": 4211, "url": "https://svs.gsfc.nasa.gov/4211/", "page_type": "Visualization", "title": "Just over the Limb Solar Event captured by SDO and IRIS", "description": "On May 9, 2014, an active region has just rotated over the limb of the Sun when it launches a large amount of plasma into space. Both SDO and IRIS caught the event. || ", "release_date": "2015-02-11T00:00:00-05:00", "update_date": "2023-05-03T13:50:00.730632-04:00", "main_image": { "id": 451881, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a004200/a004211/Flare20140509_304A.00400_print.jpg", "filename": "Flare20140509_304A.00400_print.jpg", "media_type": "Image", "alt_text": "Full-disk 4Kx4K SDO images.", "width": 1024, "height": 1024, "pixels": 1048576 } } }, { "id": 410427, "type": "details_page", "extra_data": null, "instance": { "id": 4232, "url": "https://svs.gsfc.nasa.gov/4232/", "page_type": "Visualization", "title": "Twelve Days of AR12192 from SDO and GOES", "description": "SDO 131 angstrom visual with overlaid plot of GOES X-ray flux during the time span. || AR12192_131_GOES.composite.01500_print.jpg (1024x1024) [274.5 KB] || AR12192_131_GOES.composite.01500_searchweb.png (320x180) [72.8 KB] || AR12192_131_GOES.composite.01500_thm.png (80x40) [6.4 KB] || AR12192_131_GOES.composite.01500_web.png (320x320) [102.2 KB] || AR12192_131_GOES-composite_1024.webm (1024x1024) [13.7 MB] || AR12192_131_GOES-composite_1024.mp4 (1024x1024) [312.6 MB] || Composite (4096x4096) [0 Item(s)] || AR12192_131_GOES-composite_1024_4232.pptx [62.0 MB] || AR12192_131_GOES-composite_1024_4232.key [64.5 MB] || AR12192_131_GOES.mp4 (4096x4096) [5.3 GB] || ", "release_date": "2015-02-11T00:00:00-05:00", "update_date": "2025-02-02T22:15:56.918350-05:00", "main_image": { "id": 449577, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a004200/a004232/AR12192_131_GOES.composite.01500_print.jpg", "filename": "AR12192_131_GOES.composite.01500_print.jpg", "media_type": "Image", "alt_text": "SDO 131 angstrom visual with overlaid plot of GOES X-ray flux during the time span.", "width": 1024, "height": 1024, "pixels": 1048576 } } }, { "id": 410428, "type": "details_page", "extra_data": null, "instance": { "id": 4235, "url": "https://svs.gsfc.nasa.gov/4235/", "page_type": "Visualization", "title": "October X-flare from Solar Dynamics Observatory", "description": "Active Region AR12192 erupts with an X-class flare in the visualization in the SDO AIA 171 angstrom filter. || Oct2014Xflare_171A_stand.HD1080i.00334_print.jpg (1024x576) [65.0 KB] || Oct2014Xflare_171A_stand.HD1080i.00334_searchweb.png (320x180) [44.3 KB] || Oct2014Xflare_171A_stand.HD1080i.00334_web.png (320x180) [44.3 KB] || Oct2014Xflare_171A_stand.HD1080i.00334_thm.png (80x40) [4.1 KB] || Oct2014Xflare_171A_stand_1080.webmhd.webm (960x540) [2.1 MB] || Oct2014Xflare_171A_stand_1080.mp4 (1920x1080) [19.7 MB] || 1920x1080_16x9_30p (1920x1080) [0 Item(s)] || Oct2014Xflare_171A_stand_1080.hwshow [82 bytes] || ", "release_date": "2015-02-11T00:00:00-05:00", "update_date": "2025-01-05T22:32:58.236015-05:00", "main_image": { "id": 449409, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a004200/a004235/Oct2014Xflare_171A.00335_print.jpg", "filename": "Oct2014Xflare_171A.00335_print.jpg", "media_type": "Image", "alt_text": "Full resolution 4Kx4K imagery for the 171 angstrom filter.", "width": 1024, "height": 1024, "pixels": 1048576 } } }, { "id": 410429, "type": "details_page", "extra_data": null, "instance": { "id": 4228, "url": "https://svs.gsfc.nasa.gov/4228/", "page_type": "Visualization", "title": "The Little Flux Rope that Couldn't", "description": "HD1080 version of full disk SDO imagery in the 131 Angstrom filter. || Sept2014_FluxRope_stand.HD1080i.00400_print.jpg (1024x576) [50.9 KB] || Sept2014_FluxRope_stand.HD1080i.00400_searchweb.png (320x180) [29.8 KB] || Sept2014_FluxRope_stand.HD1080i.00400_thm.png (80x40) [2.6 KB] || 1920x1080_16x9_30p (1920x1080) [0 Item(s)] || Sept2014_FluxRope.HD1080i_p30.mp4 (1920x1080) [15.8 MB] || Sept2014_FluxRope.HD1080i_p30.webm (1920x1080) [3.3 MB] || Sept2014_FluxRope.HD1080i_p30.mp4.hwshow [195 bytes] || ", "release_date": "2017-08-11T10:00:00-04:00", "update_date": "2025-01-05T22:32:09.905506-05:00", "main_image": { "id": 412406, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a004200/a004228/Sept2014_FluxRope.00500_print.jpg", "filename": "Sept2014_FluxRope.00500_print.jpg", "media_type": "Image", "alt_text": "4Kx4K image sequences of full disk SDO imagery in the 131 Angstrom filter.", "width": 1024, "height": 1024, "pixels": 1048576 } } }, { "id": 410430, "type": "details_page", "extra_data": null, "instance": { "id": 11136, "url": "https://svs.gsfc.nasa.gov/11136/", "page_type": "Produced Video", "title": "Sun unleashes first X-class flare of 2014", "description": "The sun emitted a significant solar flare peaking at 1:32 p.m. EST on Jan.7, 2014. This is the first significant flare of 2014, and follows on the heels of mid-level flare earlier in the day. Each flare was centered over a different area of a large sunspot group currently situated at the center of the sun, about half way through its 14-day journey across the front of the disk along with the rotation of the sun. This flare is classified as an X1.2-class flare. X-class denotes the most intense flares, while the number provides more information about its strength. An X2 is twice as intense as an X1, an X3 is three times as intense, etc. || ", "release_date": "2014-01-07T16:00:00-05:00", "update_date": "2023-05-03T13:51:19.627276-04:00", "main_image": { "id": 459508, "url": "https://svs.gsfc.nasa.gov/vis/a010000/a011100/a011136/Jan_7_X_Flare_1600-304_crop_web.jpg", "filename": "Jan_7_X_Flare_1600-304_crop_web.jpg", "media_type": "Image", "alt_text": "This closeup of the Sun taken by NASA's Solar Dynamics Observatory, shows large sunspot AR1944 and the source area of the X1.2 class solar flare, which appears to be from adjacent, smaller sunspot AR1943.Image Credit:NASA/SDO/Goddard Space Flight Center", "width": 320, "height": 240, "pixels": 76800 } } }, { "id": 410431, "type": "details_page", "extra_data": null, "instance": { "id": 4267, "url": "https://svs.gsfc.nasa.gov/4267/", "page_type": "Visualization", "title": "December 2014 Sparkling X-Flare from Solar Dynamics Observatory", "description": "A view of the X-flare in the 131 angstrom filter. || Dec2014SparkleX_131A_stand.HD1080i.01300_print.jpg (1024x576) [80.6 KB] || Dec2014SparkleX_131A_stand.HD1080i.01300_searchweb.png (320x180) [42.1 KB] || Dec2014SparkleX_131A_stand.HD1080i.01300_thm.png (80x40) [4.0 KB] || Dec2014SparkleX_131A_stand_HD1080.mp4 (1920x1080) [140.7 MB] || Dec2014SparkleX_131A.HD1080.mov (1920x1080) [531.0 MB] || Dec2014SparkleX_131A (1920x1080) [256.0 KB] || Dec2014SparkleX_131A.HD1080.webm (1920x1080) [10.1 MB] || ", "release_date": "2015-02-11T00:00:00-05:00", "update_date": "2023-05-03T13:50:02.168676-04:00", "main_image": { "id": 446837, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a004200/a004267/Dec2014SparkleX_131A.00700_print.jpg", "filename": "Dec2014SparkleX_131A.00700_print.jpg", "media_type": "Image", "alt_text": "4Kx4K frames of the X-flare in the 131 angstrom filter.", "width": 1024, "height": 1024, "pixels": 1048576 } } }, { "id": 410432, "type": "details_page", "extra_data": null, "instance": { "id": 11463, "url": "https://svs.gsfc.nasa.gov/11463/", "page_type": "Produced Video", "title": "SDO Lunar Transit, Prominence Eruption, and M-Class Flare", "description": "On Jan 30, 2014, beginning at 8:31 a.m EST, the moon moved between NASA’s Solar Dynamics Observatory, or SDO, and the sun, giving the observatory a view of a partial solar eclipse from space. Such a lunar transit happens two to three times each year. This one lasted two and one half hours, which is the longest ever recorded. When the next one will occur is as of yet unknown due to planned adjustments in SDO's orbit.Note in the pictures how crisp the horizon is on the moon, a reflection of the fact that the moon has no atmosphere around it to distort the light from the sun.The sun emitted a mid-level solar flare, peaking at 11:11 a.m. EST on Jan. 30, 2014. Images of the flare were captured by NASA's Solar Dynamics Observatory, or SDO, shortly after the observatory witnessed a lunar transit. The black disk of the moon can be seen in the lower right of the images. || ", "release_date": "2014-01-30T13:00:00-05:00", "update_date": "2023-05-03T13:51:16.030444-04:00", "main_image": { "id": 458509, "url": "https://svs.gsfc.nasa.gov/vis/a010000/a011400/a011463/1-30-14_Eclipse-PE_171-304_web.jpg", "filename": "1-30-14_Eclipse-PE_171-304_web.jpg", "media_type": "Image", "alt_text": "NASA's Solar Dynamics Observatory captured this image of the moon crossing in front of its view of the sun on Jan. 30, 2014, at 10:30 a.m. EST in 171 and 304 angstrom light. The two wavelengths are blended together. Credit: NASA/SDO", "width": 320, "height": 320, "pixels": 102400 } } }, { "id": 410433, "type": "details_page", "extra_data": null, "instance": { "id": 4246, "url": "https://svs.gsfc.nasa.gov/4246/", "page_type": "Visualization", "title": "The Big Sunspot of 2014", "description": "The view from the SDO AIA 171 angstrom filter of AR 12192 moving across the solar disk. || Oct2014BigSpot_171A_stand.HD1080i.01300_print.jpg (1024x576) [64.8 KB] || Oct2014BigSpot_171A_stand.HD1080i.01300_searchweb.png (320x180) [44.4 KB] || Oct2014BigSpot_171A_stand.HD1080i.01300_web.png (320x180) [44.4 KB] || Oct2014BigSpot_171A_stand.HD1080i.01300_thm.png (80x40) [4.1 KB] || Oct2014BigSpot_171AHD (1920x1080) [256.0 KB] || Oct2014BigSpot_171A_stand_HD1080.mp4 (1920x1080) [73.8 MB] || Oct2014BigSpot_171A.HD1080.webm (1920x1080) [9.1 MB] || Oct2014BigSpot_171A.HD1080.mov (1920x1080) [218.3 MB] || ", "release_date": "2015-02-11T00:00:00-05:00", "update_date": "2023-05-03T13:50:01.756255-04:00", "main_image": { "id": 448018, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a004200/a004246/Oct2014BigSpot_171A.01300_print.jpg", "filename": "Oct2014BigSpot_171A.01300_print.jpg", "media_type": "Image", "alt_text": "Full resolution 4Kx4K imagery in the AIA 171 angstrom filter.", "width": 1024, "height": 1024, "pixels": 1048576 } } }, { "id": 410434, "type": "details_page", "extra_data": null, "instance": { "id": 4244, "url": "https://svs.gsfc.nasa.gov/4244/", "page_type": "Visualization", "title": "December 4, 2014: M6 Flare as Seen by Solar Dynamics Observatory & GOES", "description": "SDO 131 angstrom visual with overlaid plot of GOES X-ray flux during the time span. || 20141204_131AIA-GOES.composite.00500_print.jpg (1024x1024) [337.7 KB] || 20141204_131AIA-GOES.composite.00500_searchweb.png (320x180) [70.8 KB] || 20141204_131AIA-GOES.composite.00500_web.png (320x320) [107.2 KB] || 20141204_131AIA-GOES.composite.00500_thm.png (80x40) [6.1 KB] || 20141204_131AIA-GOES_1024x1024.webm (1024x1024) [3.0 MB] || 20141204_131AIA-GOES_1024x1024.mp4 (1024x1024) [68.0 MB] || SDO131AnGOES (4096x4096) [64.0 KB] || 20141204_131AIA-GOES.mp4 (4096x4096) [1.2 GB] || ", "release_date": "2015-02-11T00:00:00-05:00", "update_date": "2023-05-03T13:50:01.523328-04:00", "main_image": { "id": 448455, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a004200/a004244/SDO_2014-12-04_131_M6flare.00400_print.jpg", "filename": "SDO_2014-12-04_131_M6flare.00400_print.jpg", "media_type": "Image", "alt_text": "4Kx4K SDO Quick-Look imagery at 5 minute cadence using the 131 angstrom filter and standard color table.", "width": 1024, "height": 1024, "pixels": 1048576 } } }, { "id": 410435, "type": "details_page", "extra_data": null, "instance": { "id": 4065, "url": "https://svs.gsfc.nasa.gov/4065/", "page_type": "Visualization", "title": "The X-Class Flare of January 2014", "description": "Early January of 2014 saw one of the largest sunspot groups of solar cycle 24 and some X-class flares near the center of the solar disk from active region AR 11943. These flares launched a few small coronal mass ejections towards the Earth. || ", "release_date": "2014-02-11T10:00:00-05:00", "update_date": "2025-02-02T22:10:48.975734-05:00", "main_image": { "id": 459196, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a004000/a004065/January2014Flare_1600A_stand.HD1080i.00360.jpg", "filename": "January2014Flare_1600A_stand.HD1080i.00360.jpg", "media_type": "Image", "alt_text": "At the ultraviolet wavelength of 160 nm, we see an image which still resembles the view in visible light, but with the faculae surrounding the sunspots more visible. The flare appears like a bright arc from the regions.", "width": 1920, "height": 1080, "pixels": 2073600 } } }, { "id": 410436, "type": "details_page", "extra_data": null, "instance": { "id": 4225, "url": "https://svs.gsfc.nasa.gov/4225/", "page_type": "Visualization", "title": "The M7 Flare of October 2, 2014, seen from SDO", "description": "In this 171 ångstrom image, the group of coronal loops on the lower right of the solar limb launches a stream of plasma. || Oct2014Mflare_171A_stand.HD1080i.00748_print.jpg (1024x576) [68.2 KB] || Oct2014Mflare_171A_stand.HD1080i.00748_searchweb.png (320x180) [46.9 KB] || Oct2014Mflare_171A_stand.HD1080i.00748_thm.png (80x40) [4.4 KB] || Oct2014Mflare_171A_stand.HD1080i.00748_web.png (320x180) [46.9 KB] || Oct2014Mflare_171A_stand_1080.mp4 (1920x1080) [23.2 MB] || Oct2014Mflare_171A (1920x1080) [128.0 KB] || Oct2014Mflare_171A_stand_720.mp4 (1280x720) [9.7 MB] || Oct2014Mflare_171A_stand_720.webmhd.webm (960x540) [2.9 MB] || Oct2014Mflare_171A_stand_360.mp4 (640x360) [2.6 MB] || ", "release_date": "2015-02-11T00:00:00-05:00", "update_date": "2023-05-03T13:50:00.990109-04:00", "main_image": { "id": 450615, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a004200/a004225/Oct2014Mflare_171A.00748_print.jpg", "filename": "Oct2014Mflare_171A.00748_print.jpg", "media_type": "Image", "alt_text": "Full resolution 4Kx4K imagery for the 171 ångstrom filter", "width": 1024, "height": 1024, "pixels": 1048576 } } }, { "id": 410437, "type": "details_page", "extra_data": null, "instance": { "id": 4216, "url": "https://svs.gsfc.nasa.gov/4216/", "page_type": "Visualization", "title": "September 2014 X-Flare", "description": "On September 10, 2014, the sun erupts with an X-flare of intensity X1.6 in the center of the solar disk. The event also launches a coronal mass ejection earthward. || ", "release_date": "2015-02-11T00:00:00-05:00", "update_date": "2023-05-03T13:50:00.861073-04:00", "main_image": { "id": 451155, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a004200/a004216/Sept2014Xflare_131A.00400_print.jpg", "filename": "Sept2014Xflare_131A.00400_print.jpg", "media_type": "Image", "alt_text": "Full resolution 4Kx4K imagery for the 131 angstrom filter.", "width": 1024, "height": 1024, "pixels": 1048576 } } }, { "id": 410438, "type": "details_page", "extra_data": null, "instance": { "id": 4202, "url": "https://svs.gsfc.nasa.gov/4202/", "page_type": "Visualization", "title": "August 24, 2014: Magnificent M-flare", "description": "M-flares are not the most powerful flares the Sun can emit, but sometimes even they can exhibit visually exciting behavior.Here we show the lead-up to an M-flare which lauches a large amount of plasma into space. The eruption takes place starting around 12:00 UTC and launches over the next 15 minutes. But stay with it, and you'll also see some of the plasma falling back towards the Sun around 13:50 UTC. || ", "release_date": "2015-02-11T00:00:00-05:00", "update_date": "2023-05-03T13:50:00.609467-04:00", "main_image": { "id": 452282, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a004200/a004202/Aug2014MagnificentM_304A.01364_print.jpg", "filename": "Aug2014MagnificentM_304A.01364_print.jpg", "media_type": "Image", "alt_text": "The flare at ejected CME launches from the western limb of the Sun (lower left of image) in this sequence from the SDO/AIA 304 angstrom filter. Full resolution 4Kx4K frames.", "width": 1024, "height": 1024, "pixels": 1048576 } } }, { "id": 410439, "type": "details_page", "extra_data": null, "instance": { "id": 4166, "url": "https://svs.gsfc.nasa.gov/4166/", "page_type": "Visualization", "title": "March 2014: Erupting Solar Prominence", "description": "A solar filament, in the upper left quadrant of the image, erupts from the Sun (about time stamp 2014 March 29 01:54:00 UTC).There is a gap of 40 minutes in the data coverage, from 03:00 - 03:40 UT. || ", "release_date": "2015-02-11T00:00:00-05:00", "update_date": "2023-05-03T13:50:00.354317-04:00", "main_image": { "id": 455815, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a004100/a004166/March2014Filament_171A_stand.HD1080i.00146.jpg", "filename": "March2014Filament_171A_stand.HD1080i.00146.jpg", "media_type": "Image", "alt_text": "Prominence eruption in the SDO/AIA 17.1nm filter.", "width": 1920, "height": 1080, "pixels": 2073600 } } }, { "id": 410440, "type": "details_page", "extra_data": null, "instance": { "id": 4125, "url": "https://svs.gsfc.nasa.gov/4125/", "page_type": "Visualization", "title": "The Fast X4 Flare from February 2014", "description": "The Sun launches a fast X-ray flare in late February 2014 and is seen by the Solar Dynamics Observatory (SDO). The eruption sends a bright ribbon of plasma off the limb of the Sun. || ", "release_date": "2015-02-11T00:00:00-05:00", "update_date": "2025-02-02T22:12:32.428758-05:00", "main_image": { "id": 457066, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a004100/a004125/Feb2014XFlare_131A_stand.HD1080i.00226.jpg", "filename": "Feb2014XFlare_131A_stand.HD1080i.00226.jpg", "media_type": "Image", "alt_text": "The X-flare eruption seen in the SDO/AIA 13.1nm filter.", "width": 1920, "height": 1080, "pixels": 2073600 } } }, { "id": 410441, "type": "details_page", "extra_data": null, "instance": { "id": 4182, "url": "https://svs.gsfc.nasa.gov/4182/", "page_type": "Visualization", "title": "Double Solar Flare of June 10, 2014 as Seen by SDO", "description": "Multiple flares erupted from the same active region just a few hours apart on June 10, 2014. The first flare, an M-class, erupted near the limb of the sun. Within a couple of hours, two more X-class flares erupted (see Classifying Solar Eruptions) peaked at 12:52UT. A number of smaller flares erupted from the same region before and after the largest events. || ", "release_date": "2015-02-11T00:00:00-05:00", "update_date": "2023-05-03T13:50:00.481410-04:00", "main_image": { "id": 453693, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a004100/a004182/Jun2014DoubleFlare_131A_stand.HD1080i.00163.png", "filename": "Jun2014DoubleFlare_131A_stand.HD1080i.00163.png", "media_type": "Image", "alt_text": "Full disk HD movie in the SDO 131 ångstrom filter.", "width": 1920, "height": 1080, "pixels": 2073600 } } }, { "id": 410442, "type": "details_page", "extra_data": null, "instance": { "id": 4164, "url": "https://svs.gsfc.nasa.gov/4164/", "page_type": "Visualization", "title": "A Multi-Mission View of a Solar Flare: Optical to Gamma-rays", "description": "To improve our understanding of complex phenomena such as solar flares, a wide variety of tools are needed. In the case of astronomy, those tools enable us to analyze the light in many different wavelengths and many different ways.Many different instruments are observing the Sun almost continuously, both from space and on the surface of the Earth. On March 29, 2014, the Dunn Solar Telescope at Sacramento Peak, New Mexico was observing a solar active region and requested other observatories to watch as well. As a result of this coordination, the region was being observed by a large number of different instruments, ground and space-based, when it subsequently erupted with an X-class flare. This visualization presents various combinations of the datasets collected during this effort. The color text represents the dominant color of the dataset in the imagery.Solar Dynamics Observatory (SDO): HMI (617.1nm). This data represents the Sun is visible light similar to how we see it from the ground.Solar Dynamics Observatory (SDO): AIA (17.1nm). Solar ultraviolet emission, which can only be seen from space, reveals plasma flowing, and escaping, along magnetic fields.IRIS Slit-Jaw Imager: 140.0nm. This high-resolution imager also contains a slit (the dark vertical line in the center of the field) which directs the light to an ultraviolet spectrometer which is used to extract even more information about the light. The imager slews back-and-forth across the region, providing spectra over a larger area of the Sun.Hinode/X-ray Telescope: x-ray band. Indicates very hot plasma.RHESSI: 50-100 keV. High-energy gamma-ray emission. Emission from these locations represent the very highest energy photons from the flare event.Dunn Solar Telescope: G-band filter. This filter, showing much of the solar surface (photosphere) in visible light, provides a detailed view of the sunspots and convection cells. The view moves because the instrument was repointed several times during the observation.Dunn Solar Telescope: IBIS ( Hydrogen alpha, 656.3nm; Calcium 854.2 nm; Iron 630.15nm). This is the small rectangular view within the Dunn Solar Telescope G-band view. This instrument can tune the wavelength during the observation, which provides views of the solar atmosphere at different depths. || ", "release_date": "2014-05-07T10:00:00-04:00", "update_date": "2023-05-03T13:50:57.113603-04:00", "main_image": { "id": 455928, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a004100/a004164/MMXFGroundView_stand.HD1080i.01819.jpg", "filename": "MMXFGroundView_stand.HD1080i.01819.jpg", "media_type": "Image", "alt_text": "A view of the visible light solar disk from SDO/HMI and zoom-in to show visible light, hydrogen-alpha, and a calcium line from the Sacremento Peak observatory.", "width": 1920, "height": 1080, "pixels": 2073600 } } }, { "id": 410443, "type": "details_page", "extra_data": null, "instance": { "id": 11564, "url": "https://svs.gsfc.nasa.gov/11564/", "page_type": "Produced Video", "title": "Sun Emits 3 X-class Flares in 2 Days", "description": "The sun emitted a significant solar flare, peaking at 7:42 a.m. EDT on June 10, 2014. NASA's Solar Dynamics Observatory – which typically observes the entire sun 24 hours a day — captured images of the flare. This flare is classified as an X2.2 flare. X-class denotes the most intense flares, while the number provides more information about its strength. An X2 is twice as intense as an X1, an X3 is three times as intense, etc.About one hour later, the sun released a second X-class flare, peaking at 8:52 a.m. EDT on June 10, 2014. This is classified as an X1.5 flare. || ", "release_date": "2014-06-10T11:00:00-04:00", "update_date": "2023-05-03T13:50:50.228979-04:00", "main_image": { "id": 454660, "url": "https://svs.gsfc.nasa.gov/vis/a010000/a011500/a011564/June_10_2014_X2pt2_Flare_Crop_web.jpg", "filename": "June_10_2014_X2pt2_Flare_Crop_web.jpg", "media_type": "Image", "alt_text": "A solar flare bursts off the left limb of the sun in this image captured by NASA's Solar Dynamics Observatory on June 10, 2014, at 7:41 a.m. EDT. This is classified as an X2.2 flare, shown in a blend of two wavelengths of light: 171 and 131 angstroms, colorized in gold and red, respectively. Cropped.Image Credit: NASA/SDO/Goddard/Wiessinger", "width": 320, "height": 240, "pixels": 76800 } } }, { "id": 410444, "type": "details_page", "extra_data": null, "instance": { "id": 11651, "url": "https://svs.gsfc.nasa.gov/11651/", "page_type": "Produced Video", "title": "September 10, 2014 X1.6 flare", "description": "The sun emitted a significant solar flare, peaking at 1:48 p.m. EDT on Sept. 10, 2014. NASA's Solar Dynamics Observatory captured images of the event. Solar flares are powerful bursts of radiation. Harmful radiation from a flare cannot pass through Earth's atmosphere to physically affect humans on the ground. However — when intense enough — they can disturb the atmosphere in the layer where GPS and communications signals travel.This flare is classified as an X1.6 class flare. \"X-class\" denotes the most intense flares, while the number provides more information about its strength. An X2 is twice as intense as an X1, an X3 is three times as intense, etc. || ", "release_date": "2014-09-11T08:00:00-04:00", "update_date": "2023-05-03T13:50:35.229498-04:00", "main_image": { "id": 451763, "url": "https://svs.gsfc.nasa.gov/vis/a010000/a011600/a011651/20140910_174246_4096_0131_print.jpg", "filename": "20140910_174246_4096_0131_print.jpg", "media_type": "Image", "alt_text": "An X1.6 class solar flare flashes in the middle of the sun on Sept. 10, 2014. This image was captured by NASA's Solar Dynamics Observatory and shows light in the 131 angstrom wavelength, which is typically colorized in teal.Credit: NASA/SDO", "width": 1024, "height": 1024, "pixels": 1048576 } } }, { "id": 410445, "type": "details_page", "extra_data": null, "instance": { "id": 11670, "url": "https://svs.gsfc.nasa.gov/11670/", "page_type": "Produced Video", "title": "Sun Emits Mid-Level Flare on October 2, 2014", "description": "The sun emitted a mid-level solar flare, peaking at 3:01 p.m. EDT on Oct. 2, 2014. NASA's Solar Dynamics Observatory, which watches the sun 24-hours a day, captured images of the flare. Solar flares are powerful bursts of radiation. Harmful radiation from a flare cannot pass through Earth's atmosphere to physically affect humans on the ground, however — when intense enough — they can disturb the atmosphere in the layer where GPS and communications signals travel.This flare is classified as an M7.3 flare. M-class flares are one-tenth as powerful as the most powerful flares, which are designated X-class flares. || ", "release_date": "2014-10-03T15:00:00-04:00", "update_date": "2023-05-03T13:50:29.586105-04:00", "main_image": { "id": 450865, "url": "https://svs.gsfc.nasa.gov/vis/a010000/a011600/a011670/Oct_2_Blend_Still.jpg", "filename": "Oct_2_Blend_Still.jpg", "media_type": "Image", "alt_text": "Video of flare and eruption in several wavelengths. It begins with 304 angstrom, then 171, and finally a blend of 304, 171 and 131, which shows the hottest flaring regions.Music: \"No Comment Before Sunset\" by Lars Leonhard, courtesy of the artist and BineMusic.Watch this video on the NASA Goddard YouTube channel.For complete transcript, click here.", "width": 1920, "height": 1080, "pixels": 2073600 } } }, { "id": 410446, "type": "details_page", "extra_data": null, "instance": { "id": 4907, "url": "https://svs.gsfc.nasa.gov/4907/", "page_type": "Visualization", "title": "A Big Sunspot from Solar Cycle 24", "description": "A large sunspot rotates across the view in SDO/HMI || BigSunspot_HMIintensity_stand.HD1080i.00300_print.jpg (1024x576) [50.6 KB] || BigSunspot_HMIintensity_stand.HD1080i.00300_searchweb.png (320x180) [21.8 KB] || BigSunspot_HMIintensity_stand.HD1080i.00300_thm.png (80x40) [2.6 KB] || 1920x1080_16x9_30p (1920x1080) [0 Item(s)] || BigSunspot_HMIintensity.HD1080i_p30.mp4 (1920x1080) [29.1 MB] || BigSunspot_HMIintensity.HD1080i_p30.webm (1920x1080) [2.2 MB] || 3840x2160_16x9_30p (3840x2160) [0 Item(s)] || BigSunspot_HMIintensity.UHD2160_p30.mp4 (3840x2160) [171.4 MB] || BigSunspot_HMIintensity.HD1080i_p30.mp4.hwshow [201 bytes] || ", "release_date": "2021-06-18T11:00:00-04:00", "update_date": "2025-01-31T00:12:58.820530-05:00", "main_image": { "id": 378575, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a004900/a004907/BigSunspot_HMIintensity.00200_print.jpg", "filename": "BigSunspot_HMIintensity.00200_print.jpg", "media_type": "Image", "alt_text": "4Kx4K frames of the large sunspot", "width": 1024, "height": 1024, "pixels": 1048576 } } }, { "id": 410447, "type": "details_page", "extra_data": null, "instance": { "id": 11721, "url": "https://svs.gsfc.nasa.gov/11721/", "page_type": "Produced Video", "title": "Holiday Lights on the Sun", "description": "The sun emitted an X1.8-class solar flare, peaking at 7:24 p.m. EST on Dec. 19, 2014.Watch this video on the NASAexplorer YouTube channel. || decemberthumbnail.jpg (1280x720) [139.0 KB] || decemberthumbnail_web.jpg (320x180) [38.0 KB] || decemberthumbnail_searchweb.png (320x180) [119.9 KB] || decemberthumbnail_thm.png (80x40) [21.5 KB] || solarholidaylights2014V2_H264_Best_1280x720_59.94.mov (1920x1080) [714.9 MB] || solarholidaylights2014V2_prores.mov (1280x720) [1.1 GB] || solarholidaylights2014V2_appletv.m4v (960x540) [32.2 MB] || solarholidayights2014V2_youtube_hq.mov (1280x720) [82.5 MB] || solarholidaylights2014V2_1280x720.wmv (1280x720) [37.3 MB] || solarholidaylights2014V2_appletv.webm (960x540) [8.7 MB] || solarholidaylights2014V2_appletv_subtitles.m4v (960x540) [32.2 MB] || solarholidaylights2014V2_ipod_lg.m4v (640x360) [13.0 MB] || decemberlightsV2.en_US.srt [633 bytes] || decemberlightsV2.en_US.vtt [646 bytes] || solarholidaylights2014V2_ipod_sm.mp4 (320x240) [6.8 MB] || ", "release_date": "2014-12-22T08:30:00-05:00", "update_date": "2023-05-03T13:50:11.518722-04:00", "main_image": { "id": 447849, "url": "https://svs.gsfc.nasa.gov/vis/a010000/a011700/a011721/decemberthumbnail.jpg", "filename": "decemberthumbnail.jpg", "media_type": "Image", "alt_text": "The sun emitted an X1.8-class solar flare, peaking at 7:24 p.m. EST on Dec. 19, 2014.Watch this video on the NASAexplorer YouTube channel.", "width": 1280, "height": 720, "pixels": 921600 } } } ], "extra_data": {} }, { "id": 371277, "url": "https://svs.gsfc.nasa.gov/gallery/sdo4k-content/#media_group_371277", "widget": "Tile gallery", "title": "2013", "caption": "", "description": "", "items": [ { "id": 410448, "type": "details_page", "extra_data": null, "instance": { "id": 4031, "url": "https://svs.gsfc.nasa.gov/4031/", "page_type": "Visualization", "title": "First Earth-Directed CME of 2013", "description": "On Jan. 13, 2013, at 2:24 a.m. EST, the sun erupted with an Earth-directed coronal mass ejection or CME. Not to be confused with a solar flare, a CME is a solar phenomenon that can send solar particles into space and reach Earth one to three days later.Experimental NASA research models, based on observations from the Solar Terrestrial Relations Observatory (STEREO) and the ESA/NASA mission the Solar and Heliospheric Observatory, show that the CME left the sun at speeds of 275 miles per second. This is a fairly typical speed for CMEs, though much slower than the fastest ones, which can be almost ten times that speed.This visualization is constructed from a computer model run of the January 13, 2013 CME. The preliminary CME parameters were measured from instruments on the STEREO (the red and blue satellite icons) and SDO (in Earth orbit) satellites. The Enlil model was used to propagate those parameters through the solar system. From this model, they can estimate the strength and time of arrival of the CME at various locations around the solar system. This allows other missions to either safe-mode their satellites for protection, or allow them to conduct measurements to test the accuracy of the model.When Earth-directed, CMEs can cause a space weather phenomenon called a geomagnetic storm, which occurs when they successfully connect up with the outside of the Earth's magnetic envelope, the magnetosphere, for an extended period of time. In the past, CMEs of this speed have not caused substantial geomagnetic storms. They have caused auroras near the poles but are unlikely to affect electrical systems on Earth or interfere with GPS or satellite-based communications systems.Two active regions — named AR 11652 and AR 11654 by the National Oceanic and Atmospheric Administration (NOAA) — have produced four low-level M-class flares since Jan. 11. Solar flares are powerful bursts of light and radiation. Harmful radiation from a flare cannot pass through Earth's atmosphere to physically affect humans on the ground, however, when intense enough, they can disturb the atmosphere in the layer where GPS and communications signals travel. M-class flares are the weakest flares that can still cause some space weather effects near Earth. The recent flares caused weak radio blackouts and their effects have already subsided.NOAA's Space Weather Prediction Center is the United States Government official source for space weather forecasts. || ", "release_date": "2013-01-21T00:00:00-05:00", "update_date": "2023-05-03T13:52:28.029098-04:00", "main_image": { "id": 469036, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a004000/a004031/2013Jan13_high2AU.0014.jpg", "filename": "2013Jan13_high2AU.0014.jpg", "media_type": "Image", "alt_text": "Enlil model for the Jan. 13, 2013 coronal mass ejection, plotted out to ten astronomical units (beyond the orbit of Saturn). The top view slices the data in the plane of the Earth's orbit and projects the planetary orbits onto that. The side view is a cross-section through the Sun-Earth line. The wedge-shape of the side view is because the Enlil model only extends above and below the solar equator by 60 degrees.", "width": 1920, "height": 1080, "pixels": 2073600 } } }, { "id": 410449, "type": "details_page", "extra_data": null, "instance": { "id": 11201, "url": "https://svs.gsfc.nasa.gov/11201/", "page_type": "Produced Video", "title": "January 31, 2013 CME and Prominence Eruption", "description": "On Jan. 31, 2013 at 2:09am EST, the sun erupted with an Earth-directed coronal mass ejection or CME. Experimental NASA research models, based on observations from the Solar Terrestrial Relations Observatory (STEREO) and ESA/NASA's Solar and Heliospheric Observatory, show that the CME left the sun at speeds of around 575 miles per second, which is a fairly typical speed for CMEs. Historically, CMEs at this speed are mild.Not to be confused with a solar flare, a CME is a solar phenomenon that can send solar particles into space and reach Earth one to three days later.Earth-directed CMEs can cause a space weather phenomenon called a geomagnetic storm, which occurs when they connect with the outside of the Earth's magnetic envelope, the magnetosphere, for an extended period of time. In the past, CME's such as this have caused auroras near the poles but didn't disrupt electrical systems on Earth or interfere with GPS or satellite-based communications systems. || ", "release_date": "2013-01-31T12:00:00-05:00", "update_date": "2023-05-03T13:52:26.528702-04:00", "main_image": { "id": 468583, "url": "https://svs.gsfc.nasa.gov/vis/a010000/a011200/a011201/Ring_Prominence_Still_2.jpg", "filename": "Ring_Prominence_Still_2.jpg", "media_type": "Image", "alt_text": "The CME included a large prominence eruption most visible in light with a wavelength of 304 angstroms. SDO captured this footage from 3:00 to 9:00 Universal Time. In this video, the imaging cadence is one frame every 36 seconds.", "width": 1920, "height": 1080, "pixels": 2073600 } } }, { "id": 410450, "type": "details_page", "extra_data": null, "instance": { "id": 4090, "url": "https://svs.gsfc.nasa.gov/4090/", "page_type": "Visualization", "title": "Solar Prominence from SDO: July 1, 2013", "description": "A large solar prominence, caught in a tug-of-war between solar gravity pulling it downward and magnetic gradients lifting upward, hovers over the limb of the Sun (left) before eventually launching into space. || ", "release_date": "2014-02-11T10:00:00-05:00", "update_date": "2025-02-02T22:11:40.647957-05:00", "main_image": { "id": 463758, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a004000/a004090/July2013Prominence_stand.HD1080i.01200.jpg", "filename": "July2013Prominence_stand.HD1080i.01200.jpg", "media_type": "Image", "alt_text": "A large solar prominence (left limb of the Sun) hovers for hours before launching into space.", "width": 1920, "height": 1080, "pixels": 2073600 } } }, { "id": 410451, "type": "details_page", "extra_data": null, "instance": { "id": 11379, "url": "https://svs.gsfc.nasa.gov/11379/", "page_type": "Produced Video", "title": "Filament Eruption Creates 'Canyon of Fire' on the Sun", "description": "A magnetic filament of solar material erupted on the sun in late September, breaking the quiet conditions in a spectacular fashion. The 200,000 mile long filament ripped through the sun's atmosphere, the corona, leaving behind what looks like a canyon of fire. The glowing canyon traces the channel where magnetic fields held the filament aloft before the explosion. Visualizers at NASA's Goddard Space Flight Center in Greenbelt, Md. combined two days of satellite data to create a short movie of this gigantic event on the sun.In reality, the sun is not made of fire, but of something called plasma: particles so hot that their electrons have boiled off, creating a charged gas that is interwoven with magnetic fields. These images were captured on Sept. 29-30, 2013, by NASA's Solar Dynamics Observatory, or SDO, which constantly observes the sun in a variety of wavelengths. Different wavelengths help capture different aspect of events in the corona. The red images shown in the movie help highlight plasma at temperatures of 90,000° F and are good for observing filaments as they form and erupt. The yellow images, showing temperatures at 1,000,000° F, are useful for observing material coursing along the sun's magnetic field lines, seen in the movie as an arcade of loops across the area of the eruption. The browner images at the beginning of the movie show material at temperatures of 1,800,000° F, and it is here where the canyon of fire imagery is most obvious. By comparing this with the other colors, one sees that the two swirling ribbons moving farther away from each other are, in fact, the footprints of the giant magnetic field loops, which are growing and expanding as the filament pulls them upward. || ", "release_date": "2013-10-24T10:00:00-04:00", "update_date": "2023-05-03T13:51:37.825752-04:00", "main_image": { "id": 461871, "url": "https://svs.gsfc.nasa.gov/vis/a010000/a011300/a011379/Canyon_of_Fire171-304-screen-matte.jpg", "filename": "Canyon_of_Fire171-304-screen-matte.jpg", "media_type": "Image", "alt_text": "Short video with music. The image is a composite of SDO AIA 171 and 304, with the two wavelengths blended in the area of the canyon.Watch this video on the NASAexplorer YouTube channel.For complete transcript, click here.", "width": 1920, "height": 1080, "pixels": 2073600 } } }, { "id": 410452, "type": "details_page", "extra_data": null, "instance": { "id": 4089, "url": "https://svs.gsfc.nasa.gov/4089/", "page_type": "Visualization", "title": "June 2013's 'Busy Sun'", "description": "June of 2013, near the maximum of solar cycle 24, while not extremely active from a solar flare perspective, presented a range of diverse phenomena. We have a couple of solar 'tornadoes' (the twisted protrusions off the limb of the Sun in upper and lower left quadrants), which we eventually see erupt material into space. There are also a number of coronal loops in active regions which are incredibly stable but still exhibit much fine detail. || ", "release_date": "2014-02-11T10:00:00-05:00", "update_date": "2025-02-02T22:11:37.136272-05:00", "main_image": { "id": 463729, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a004000/a004089/June2013Busy_stand.HD1080i.04000.jpg", "filename": "June2013Busy_stand.HD1080i.04000.jpg", "media_type": "Image", "alt_text": "Movie of a serene but still active Sun.", "width": 1920, "height": 1080, "pixels": 2073600 } } }, { "id": 410453, "type": "details_page", "extra_data": null, "instance": { "id": 4066, "url": "https://svs.gsfc.nasa.gov/4066/", "page_type": "Visualization", "title": "SDO's Multi-wavelength View of a May 2013 Solar Flare", "description": "An active region on the left limb of the Sun launches a large flare and coronal material in this sequence from early May 2013. || ", "release_date": "2014-02-11T10:00:00-05:00", "update_date": "2025-02-02T22:10:52.532650-05:00", "main_image": { "id": 459251, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a004000/a004066/May2013Flare_304A_stand.HD1080i.00200.jpg", "filename": "May2013Flare_304A_stand.HD1080i.00200.jpg", "media_type": "Image", "alt_text": "In the 30.4nm wavelength of the helium ion, we can see both the flare, as well as some of the ejected solar material.", "width": 1920, "height": 1080, "pixels": 2073600 } } }, { "id": 410454, "type": "details_page", "extra_data": null, "instance": { "id": 4051, "url": "https://svs.gsfc.nasa.gov/4051/", "page_type": "Visualization", "title": "Boiling Solar Prominence from February 2013", "description": "A long-lived prominence (see Wikipedia) hovers over the limb of the Sun (about the 4-5 o'clock position) before breaking up. || ", "release_date": "2014-02-11T10:00:00-05:00", "update_date": "2025-02-02T22:10:42.012342-05:00", "main_image": { "id": 467683, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a004000/a004051/Feb2013Prominence_stand.HD1080i.00100.jpg", "filename": "Feb2013Prominence_stand.HD1080i.00100.jpg", "media_type": "Image", "alt_text": "HD movie of February 2013 prominence", "width": 1920, "height": 1080, "pixels": 2073600 } } }, { "id": 410455, "type": "details_page", "extra_data": null, "instance": { "id": 4136, "url": "https://svs.gsfc.nasa.gov/4136/", "page_type": "Visualization", "title": "More Solar Excitement - October 2013", "description": "Solar activity in October 2013 continues with several active regions, particularly on the limb, launching solar material into space. || ", "release_date": "2014-02-11T10:00:00-05:00", "update_date": "2023-05-03T13:51:13.867068-04:00", "main_image": { "id": 458925, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a004100/a004136/October2013Flare2_304A_stand.HD1080i.01000.jpg", "filename": "October2013Flare2_304A_stand.HD1080i.01000.jpg", "media_type": "Image", "alt_text": "Movie of continuing solar activity in October 2013.", "width": 1920, "height": 1080, "pixels": 2073600 } } }, { "id": 410456, "type": "details_page", "extra_data": null, "instance": { "id": 4133, "url": "https://svs.gsfc.nasa.gov/4133/", "page_type": "Visualization", "title": "February 2013: The Busy Sun", "description": "Even near solar maximum, with sunspots dotting the photosphere, the Sun can look tranquil and serene in visible light. In the case of these images from the HMI instrument on the Solar Dynamics Observatory, the only obvious changes are the constant shimmering of the solar disk due to the bubbling of solar granulation.But in ultraviolet light, in particular the 30.4 nanometer line of the helium ion, we see much more activity. Dark, wispy lines of cooler solar filaments (the term used for solar prominences when seen against the disk) stretch across the disk. The same structures, seen against the fainter glow of the solar corona, resemble slowly evolving flames on the limb of the Sun. Solar active regions surrounding the sunspots, appear bright in ultraviolet light. || ", "release_date": "2014-02-11T10:00:00-05:00", "update_date": "2023-05-03T13:51:13.715338-04:00", "main_image": { "id": 459129, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a004100/a004133/Feb2013Busy2_304A_stand.HD1080i.03600.jpg", "filename": "Feb2013Busy2_304A_stand.HD1080i.03600.jpg", "media_type": "Image", "alt_text": "The Sun in the light of singly-ionized helium at 30.4 nanometers.", "width": 1920, "height": 1080, "pixels": 2073600 } } }, { "id": 410457, "type": "details_page", "extra_data": null, "instance": { "id": 10785, "url": "https://svs.gsfc.nasa.gov/10785/", "page_type": "Produced Video", "title": "NASA's Heliophysics Fleet Captures May 1, 2013 Prominence Eruption and CME", "description": "On May 1, 2013, NASA's Solar Dynamics Observatory (SDO) watched as an active region just around the East limb (left edge) of the sun erupted with a huge cloud of solar material—a heated, charged gas called plasma. This eruption, called a coronal mass ejection, or CME, sent the plasma streaming out through the solar system. Viewing the sun in the extreme ultraviolet wavelength of 304 angstroms, SDO provided a beautiful view of the initial arc as it left the solar surface. Such eruptions soon leave SDO's field of view, but other satellites in NASA's Heliophysics fleet can pick them up, tracking such space weather to determine if they are headed toward Earth or spacecraft near other planets. With advance warning, many space assets can be put into safe mode and protect themselves from the effects of such particle radiation.In addition to the images captured by SDO, the May 1, 2013 CME was also observed by the ESA/NASA Solar and Heliospheric Observatory (SOHO). SOHO houses two overlapping coronagraphs—telescopes where the bright sun is blocked by a disk so it doesn't overpower the fainter solar atmosphere—and they both saw the CME continue outward. The LASCO C2 coronagraph shows the region out to about 2.5 million miles. The LASCO C3 coronagraph expands even farther out to around 13.5 million miles. Both of these instruments show the CME as it expands and becomes fainter on its trip away from the sun.NASA's Solar Terrestrial Relations Observatory (STEREO) Ahead satellite saw the eruption from a very different angle. It, along with its twin STEREO Behind, is orbiting at a similar distance as Earth. STEREO-A orbits slightly faster than Earth and STEREO-B orbits slightly slower. Currently, STEREO-A is more than two-thirds of the way to being directly behind the sun, and has a view of the far side of the sun. From this perspective, the CME came off the right side of the sun. STEREO has an extreme ultraviolet camera similar to SDO's, but it also has coronagraphs like SOHO. As a result, using its two inner coronagraphs, it was able to track the CME from the solar surface out to 6.3 million miles.Working together, such missions provide excellent coverage of a wide variety of solar events, a wealth of scientific data—and lots of beautiful imagery.Watch this video on YouTube. || ", "release_date": "2013-05-07T11:00:00-04:00", "update_date": "2023-05-03T13:52:11.042001-04:00", "main_image": { "id": 465754, "url": "https://svs.gsfc.nasa.gov/vis/a010000/a010700/a010785/Fleet_Still.jpg", "filename": "Fleet_Still.jpg", "media_type": "Image", "alt_text": "Several missions within NASA's Heliophysics System Observatory captured images of a gigantic eruption on the sun on May 1, 2013. Working together, such missions provide excellent coverage of a wide variety of solar events, a wealth of scientific data—and lots of beautiful imagery.For complete transcript, click here.", "width": 1920, "height": 1080, "pixels": 2073600 } } }, { "id": 410458, "type": "details_page", "extra_data": null, "instance": { "id": 11285, "url": "https://svs.gsfc.nasa.gov/11285/", "page_type": "Produced Video", "title": "First X-Class Solar Flares of 2013", "description": "On May 13, 2013, the sun emitted an X2.8-class flare, peaking at 12:05 p.m. EDT. This is the the strongest X-class flare of 2013 so far, surpassing in strength the X1.7-class flare that occurred 14 hours earlier. It is the 16th X-class flare of the current solar cycle and the third-largest flare of that cycle. The second-strongest was an X5.4 event on March 7, 2012. The strongest was an X6.9 on Aug. 9, 2011.On May 12, 2013, the sun emitted a significant solar flare, peaking at 10 p.m. EDT. This flare is classified as an X1.7, making it the first X-class flare of 2013. The flare was also associated with another solar phenomenon, called a coronal mass ejection (CME) that can send solar material out into space. This CME was not Earth-directed. The May 12 flare was also associated with a coronal mass ejection, another solar phenomenon that can send billions of tons of solar particles into space, which can affect electronic systems in satellites and on the ground. Experimental NASA research models show that the CME left the sun at 745 miles per second and is not Earth-directed, however its flank may pass by the STEREO-B and Spitzer spacecraft, and their mission operators have been notified. If warranted, operators can put spacecraft into safe mode to protect the instruments from solar material. There is some particle radiation associated with this event, which is what can concern operators of interplanetary spacecraft since the particles can trip computer electronics on board. || ", "release_date": "2013-05-13T10:30:00-04:00", "update_date": "2023-05-03T13:52:10.120221-04:00", "main_image": { "id": 465387, "url": "https://svs.gsfc.nasa.gov/vis/a010000/a011200/a011285/SDO_May_13_XFlare_131-171_Crop_web.jpg", "filename": "SDO_May_13_XFlare_131-171_Crop_web.jpg", "media_type": "Image", "alt_text": "The sun erupted with an X1.7-class solar flare on May 12, 2013. This is a blend of two images of the flare from NASA's Solar Dynamics Observatory (SDO) — one image shows light in the 171 angstrom wavelength, the other in 131 angstroms.Credit: NASA/SDO/AIA", "width": 319, "height": 298, "pixels": 95062 } } }, { "id": 410459, "type": "details_page", "extra_data": null, "instance": { "id": 4121, "url": "https://svs.gsfc.nasa.gov/4121/", "page_type": "Visualization", "title": "October 2013 X-Flare from Solar Dynamics Observatory", "description": "Another Halloween space weather fest? October-November 2003 of the previous solar cycle saw some of the most energetic solar events since space flight (see Halloween Solar Storms 2003: A Multi-Mission View. Halloween of 2013 has seen a similar round of high solar activity, with energetic flares and coronal mass ejections (CMEs). || ", "release_date": "2014-02-11T10:00:00-05:00", "update_date": "2025-02-02T22:12:27.512653-05:00", "main_image": { "id": 461136, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a004100/a004121/October2013Flare_304A_stand.HD1080i.00300.jpg", "filename": "October2013Flare_304A_stand.HD1080i.00300.jpg", "media_type": "Image", "alt_text": "A movie of October 2013 solar flares in the SDO/AIA 30.4 nm filter.", "width": 1920, "height": 1080, "pixels": 2073600 } } }, { "id": 410460, "type": "details_page", "extra_data": null, "instance": { "id": 11298, "url": "https://svs.gsfc.nasa.gov/11298/", "page_type": "Produced Video", "title": "Sun Emits a Solstice CME", "description": "On June 20, 2013, at 11:24 p.m., the sun erupted with an Earth-directed coronal mass ejection or CME, a solar phenomenon that can send billions of tons of particles into space that can reach Earth one to three days later. These particles cannot travel through the atmosphere to harm humans on Earth, but they can affect electronic systems in satellites and on the ground. Experimental NASA research models, based on observations from NASA's Solar Terrestrial Relations Observatory and ESA/NASA's Solar and Heliospheric Observatory show that the CME left the sun at speeds of around 1350 miles per second, which is a fast speed for CMEs. Earth-directed CMEs can cause a space weather phenomenon called a geomagnetic storm, which occurs when they funnel energy into Earth's magnetic envelope, the magnetosphere, for an extended period of time. The CME's magnetic fields peel back the outermost layers of Earth's fields changing their very shape. Magnetic storms can degrade communication signals and cause unexpected electrical surges in power grids. They also can cause aurora. Storms are rare during solar minimum, but as the sun's activity ramps up every 11 years toward solar maximum—currently expected in late 2013—large storms occur several times per year.In the past, geomagnetic storms caused by CMEs of this strength and direction have usually been mild. In addition, the CME may pass by additional spacecraft: Messenger, STEREO B, Spitzer, and their mission operators have been notified. If warranted, operators can put spacecraft into safe mode to protect the instruments from the solar material. || ", "release_date": "2013-06-28T00:00:00-04:00", "update_date": "2023-05-03T13:52:02.365119-04:00", "main_image": { "id": 464303, "url": "https://svs.gsfc.nasa.gov/vis/a010000/a011200/a011298/PE_Still.jpg", "filename": "PE_Still.jpg", "media_type": "Image", "alt_text": "Video of prominence eruption showing a blend of 304 and 171 angstrom light imaged by the Solar Dynamics Observatory's AIA instrument.Credit: NASA's Goddard Space Flight Center/SDO", "width": 1920, "height": 1080, "pixels": 2073600 } } }, { "id": 410461, "type": "details_page", "extra_data": null, "instance": { "id": 4101, "url": "https://svs.gsfc.nasa.gov/4101/", "page_type": "Visualization", "title": "August 2013: SDO Observes Large Coronal Hole", "description": "On the Sun, coronal holes represent regions where the solar magnetic field does not connect back to the Sun. In these cases, the magnetic field guides the charged particles of the solar wind into distant space, forming the fast solar wind. || ", "release_date": "2013-09-20T10:00:00-04:00", "update_date": "2025-02-02T22:11:59.237870-05:00", "main_image": { "id": 462497, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a004100/a004101/August2013Hole_stand.HD1080i.00700.jpg", "filename": "August2013Hole_stand.HD1080i.00700.jpg", "media_type": "Image", "alt_text": "This visualization shows the coronal hole over the course of 24 hours, sampled about once per minute.", "width": 1920, "height": 1080, "pixels": 2073600 } } }, { "id": 410462, "type": "details_page", "extra_data": null, "instance": { "id": 11387, "url": "https://svs.gsfc.nasa.gov/11387/", "page_type": "Produced Video", "title": "Five Days of Flares and CMEs", "description": "This movie shows 23 of the 26 M- and X-class flares on the sun between 18:00 UT Oct. 23 and 15:00 UT Oct. 28, 2013, as captured by NASA's Solar Dynamics Observatory. It also shows the coronal mass ejections — great clouds of solar material bursting off the sun into space — during that time as captured by the ESA/NASA Solar and Heliospheric Observatory. || ", "release_date": "2013-10-29T16:30:00-04:00", "update_date": "2023-05-03T13:51:33.389694-04:00", "main_image": { "id": 461578, "url": "https://svs.gsfc.nasa.gov/vis/a010000/a011300/a011387/October_Flares_Still.jpg", "filename": "October_Flares_Still.jpg", "media_type": "Image", "alt_text": "Credit: NASA/ESA/Goddard Space Flight CenterMusic: \"Stella Nova\" by Lars Leonhard, courtesy of the artist and Ultimae Records.Watch this video on the NASAexplorer YouTube channel.For complete transcript, click here.", "width": 1920, "height": 1080, "pixels": 2073600 } } } ], "extra_data": {} }, { "id": 371278, "url": "https://svs.gsfc.nasa.gov/gallery/sdo4k-content/#media_group_371278", "widget": "Tile gallery", "title": "2012", "caption": "", "description": "", "items": [ { "id": 410463, "type": "details_page", "extra_data": null, "instance": { "id": 4909, "url": "https://svs.gsfc.nasa.gov/4909/", "page_type": "Visualization", "title": "Monster Solar Filament Launch and CME", "description": "Launch of the filament at low cadence (36 seconds) as visible in the 304 Angstrom filter on SDO/AIA. || FilamentLaunch2012-Slow_304A_stand.HD1080i.00876_print.jpg (1024x576) [134.4 KB] || FilamentLaunch2012-Slow_304A_stand.HD1080i.00876_searchweb.png (320x180) [48.3 KB] || FilamentLaunch2012-Slow_304A_stand.HD1080i.00876_thm.png (80x40) [4.1 KB] || FilamentLaunch2012-Slow_304A (1920x1080) [0 Item(s)] || FilamentLaunch2012-Slow_304A_stand.HD1080i_p30.mp4 (1920x1080) [85.3 MB] || FilamentLaunch2012-Slow_304A_stand.HD1080i_p30.webm (1920x1080) [7.0 MB] || FilamentLaunch2012-Slow_304A.UHD (3840x2160) [0 Item(s)] || FilamentLaunch2012-Slow_304A_stand.UHD2160_p30.mp4 (3840x2160) [477.3 MB] || FilamentLaunch2012-Slow_304A_stand.HD1080i_p30.mp4.hwshow [212 bytes] || ", "release_date": "2021-06-18T11:00:00-04:00", "update_date": "2025-01-31T00:12:59.391282-05:00", "main_image": { "id": 378410, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a004900/a004909/FilamentLaunch2012-Slow_304A_stand.HD1080i.00876_print.jpg", "filename": "FilamentLaunch2012-Slow_304A_stand.HD1080i.00876_print.jpg", "media_type": "Image", "alt_text": "Launch of the filament at low cadence (36 seconds) as visible in the 304 Angstrom filter on SDO/AIA.", "width": 1024, "height": 576, "pixels": 589824 } } }, { "id": 410464, "type": "details_page", "extra_data": null, "instance": { "id": 3999, "url": "https://svs.gsfc.nasa.gov/3999/", "page_type": "Visualization", "title": "The View from SDO: The August 31, 2012 Filament Eruption", "description": "The Solar Dynamics Observatory (SDO) observed a large filament eruption on August 31, 2012. This visualization was generated using high time resolution (12 seconds) data from the Atmospheric Imaging Assembly (AIA). Two datasets are used, the SDO/AIA 304 Ångstrom wavelength (orange color table) and the 171 Ångstrom wavelength (gold color table). These are wavelengths in the ultraviolet band of the electromagnetic spectrum. They are not visible to the human eye or to ground-based telescopes so coded colors are used in presentation.It is the source material for \"August 31, 2012 Magnificent CME\" visualization. || ", "release_date": "2012-10-26T00:00:00-04:00", "update_date": "2025-02-02T22:09:12.832758-05:00", "main_image": { "id": 471365, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a003900/a003999/AIA171AugustCME.00800_web.png", "filename": "AIA171AugustCME.00800_web.png", "media_type": "Image", "alt_text": "SDO movie at 171Ångstroms of the filament eruption on August 31, 2012. 1Kx1K movie & 4Kx4K frames.", "width": 320, "height": 320, "pixels": 102400 } } }, { "id": 410465, "type": "details_page", "extra_data": null, "instance": { "id": 11095, "url": "https://svs.gsfc.nasa.gov/11095/", "page_type": "Produced Video", "title": "August 31, 2012 Magnificent CME", "description": "On August 31, 2012 a long filament of solar material that had been hovering in the sun's atmosphere, the corona, erupted out into space at 4:36 p.m. EDT. The coronal mass ejection, or CME, traveled at over 900 miles per second. The CME did not travel directly toward Earth, but did connect with Earth's magnetic environment, or magnetosphere, with a glancing blow. causing aurora to appear on the night of Monday, September 3. || ", "release_date": "2012-09-04T14:00:00-04:00", "update_date": "2023-05-03T13:52:48.922764-04:00", "main_image": { "id": 472497, "url": "https://svs.gsfc.nasa.gov/vis/a010000/a011000/a011095/304-171_Overlay_Blend_Crop.jpg", "filename": "304-171_Overlay_Blend_Crop.jpg", "media_type": "Image", "alt_text": "An overlay blended version of the 304 and 171 angstrom wavelengths. Cropped.", "width": 1920, "height": 1080, "pixels": 2073600 } } }, { "id": 410466, "type": "details_page", "extra_data": null, "instance": { "id": 4026, "url": "https://svs.gsfc.nasa.gov/4026/", "page_type": "Visualization", "title": "July 2012: Coronal Rain", "description": "A moderate solar flare was emitted by the sun on July 19, 2012. At 5:58 UTC it peaked at M7.7 on the flare scale, which makes it fairly powerful, but still much weaker than X-class flares, which are the largest. What made this particular event so noteworthy was the associated activity in the sun's corona. For the next day, hot plasma in corona cooled and condensed along the strong magnetic fields of the region that produced the flare. Magnetic fields are invisible, but the plasma is very obvious in the extreme ultraviolet wavelength of 304 angstroms, which highlights material at a temperature of about 50,000 Kelvin. This plasma is attracted to the magnetic fields and outlines them very clearly as it slowly falls back to the solar surface. This process of condensing plasma falling to the surface is called coronal rain.The footage in this video was collected by the Solar Dynamics Observatory's AIA instrument. SDO collected one frame every 12 seconds so each second in this video corresponds to 6 minutes of real time. The video covers 4:30 UTC on July 19th to 2:00 UTC on July 20th, a period of 21 hours and 30 minutes.Music—\"Thunderbolt\" by Lars Leonhard || ", "release_date": "2013-02-20T10:00:00-05:00", "update_date": "2025-02-02T22:09:50.215978-05:00", "main_image": { "id": 469747, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a004000/a004026/AIA304July2012rain_stand.HD1080i.03000.jpg", "filename": "AIA304July2012rain_stand.HD1080i.03000.jpg", "media_type": "Image", "alt_text": "An HD1080 movie of the coronal rain (right limb of sun) in the 304 Å wavelength.", "width": 1920, "height": 1080, "pixels": 2073600 } } }, { "id": 410467, "type": "details_page", "extra_data": null, "instance": { "id": 4761, "url": "https://svs.gsfc.nasa.gov/4761/", "page_type": "Visualization", "title": "New sites for magnetic reconnection", "description": "HD and UHD movie views of the plasma flowing along magnetic fields lines visible at 171Å. || May2012_Reconn_171A_stand.HD1080i.00951_print.jpg (1024x576) [52.0 KB] || May2012_Reconn_171A_stand.HD1080i.00951_searchweb.png (320x180) [43.5 KB] || May2012_Reconn_171A_stand.HD1080i.00951_thm.png (80x40) [4.2 KB] || AIA171A (1920x1080) [0 Item(s)] || May2012_Reconn_171A.HD1080i_p30.mp4 (1920x1080) [21.9 MB] || May2012_Reconn_171A.HD1080i_p30.webm (1920x1080) [7.0 MB] || AIA171A (3840x2160) [0 Item(s)] || May2012_Reconn_171A_2160p30.mp4 (3840x2160) [107.3 MB] || May2012_Reconn_171A.HD1080i_p30.mp4.hwshow [197 bytes] || ", "release_date": "2019-12-17T10:00:00-05:00", "update_date": "2025-01-06T00:15:05.590503-05:00", "main_image": { "id": 391680, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a004700/a004761/May2012_Reconn_171A.00951_print.jpg", "filename": "May2012_Reconn_171A.00951_print.jpg", "media_type": "Image", "alt_text": "4Kx4K frames of the plasma flowing along magnetic fields lines visible at 171Å.", "width": 1024, "height": 1024, "pixels": 1048576 } } }, { "id": 410468, "type": "details_page", "extra_data": null, "instance": { "id": 4038, "url": "https://svs.gsfc.nasa.gov/4038/", "page_type": "Visualization", "title": "Solar Prominence Dance - December 31, 2012", "description": "On the final day of 2012, the sun presented a beautiful twisting prominence that rose high into the corona for about 3 hours. It was most visible in extreme ultraviolet light with a wavelength of 304 angstroms. This wavelength highlights plasma with temperatures of around 50,000 Kelvin. The Atmospheric Imaging Assembly on NASA's Solar Dynamics Observatory captured the event at 4k resolution and a high imaging cadence of one image every 12 seconds. || ", "release_date": "2013-02-11T10:00:00-05:00", "update_date": "2025-02-02T22:10:19.680024-05:00", "main_image": { "id": 468796, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a004000/a004038/Dec2012SolarBallet_stand.HD1080i.00400.jpg", "filename": "Dec2012SolarBallet_stand.HD1080i.00400.jpg", "media_type": "Image", "alt_text": "HD movie of the prominence.", "width": 1920, "height": 1080, "pixels": 2073600 } } }, { "id": 410469, "type": "details_page", "extra_data": null, "instance": { "id": 11044, "url": "https://svs.gsfc.nasa.gov/11044/", "page_type": "Produced Video", "title": "Before the Flare: AR1520 and Shimmering Coronal Loops", "description": "The sun emitted a large flare on July 12, 2012, but earlier in the week it gave a demonstration of how gorgeous solar activity can be. This movie shows the sun from late July 8 to early July 10 shortly before it unleashed an X-class flare beginning at 12:11 PM EDT on July 12 as captured by the Solar Dynamics Observatory (SDO). || ", "release_date": "2012-07-16T17:00:00-04:00", "update_date": "2023-05-03T13:52:56.338438-04:00", "main_image": { "id": 474350, "url": "https://svs.gsfc.nasa.gov/vis/a010000/a011000/a011044/AR1520_Beauty_Still_1.jpg", "filename": "AR1520_Beauty_Still_1.jpg", "media_type": "Image", "alt_text": "VideoFor complete transcript, click here.", "width": 1920, "height": 1080, "pixels": 2073600 } } }, { "id": 410470, "type": "details_page", "extra_data": null, "instance": { "id": 4259, "url": "https://svs.gsfc.nasa.gov/4259/", "page_type": "Visualization", "title": "April 2012 Solar Flare & Eruption", "description": "Full disk movie of the flare and eruption, as seen through the 171angstrom filter. || April2012Eruption_171A_stand.HD1080i.00192_print.jpg (1024x576) [64.6 KB] || April2012Eruption_171AHD (1920x1080) [128.0 KB] || April2012Eruption_171A.HD1080i.mov (1920x1080) [57.8 MB] || April2012Eruption_171A_stand_1080.mp4 (1920x1080) [22.2 MB] || April2012Eruption_171A.HD1080i.webm (1920x1080) [6.5 MB] || ", "release_date": "2015-02-11T00:00:00-05:00", "update_date": "2023-05-03T13:50:02.067187-04:00", "main_image": { "id": 447152, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a004200/a004259/April2012Eruption_304A.00590_print.jpg", "filename": "April2012Eruption_304A.00590_print.jpg", "media_type": "Image", "alt_text": "4Kx4K full resolution frames of the flare and eruption, as seen through the 304 angstrom filter.", "width": 1024, "height": 1024, "pixels": 1048576 } } }, { "id": 410471, "type": "details_page", "extra_data": null, "instance": { "id": 3919, "url": "https://svs.gsfc.nasa.gov/3919/", "page_type": "Visualization", "title": "Solar Tornados as Seen by SDO (February 7, 2012)", "description": "A tornado-like structure is observed coming over the limb of the Sun (upper left quadrant) by SDO. || ", "release_date": "2012-03-07T00:00:00-05:00", "update_date": "2025-03-10T00:01:51.540413-04:00", "main_image": { "id": 478582, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a003900/a003919/SDO_2012-02_171_Tornado.02000_web.png", "filename": "SDO_2012-02_171_Tornado.02000_web.png", "media_type": "Image", "alt_text": "A movie of the tornado-like structure on the limb of the Sun.", "width": 320, "height": 320, "pixels": 102400 } } }, { "id": 410472, "type": "details_page", "extra_data": null, "instance": { "id": 4027, "url": "https://svs.gsfc.nasa.gov/4027/", "page_type": "Visualization", "title": "A July 2012 CME from SDO", "description": "On July 18, 2012, a fairly small explosion of light burst off the lower right limb of the sun. Such flares often come with an associated eruption of solar material, known as a coronal mass ejection or CME — but this one did not. Something interesting did happen, however. Magnetic field lines in this area of the sun's atmosphere, the corona, began to twist and kink, generating the hottest solar material — a charged gas called plasma — to trace out the newly-formed slinky shape. The plasma glowed brightly in extreme ultraviolet images from the Atmospheric Imaging Assembly (AIA) aboard NASA's Solar Dynamics Observatory (SDO) and scientists were able to watch for the first time the very formation of something they had long theorized was at the heart of many eruptive events on the sun: a flux rope.Eight hours later, on July 19, the same region flared again. This time the flux rope's connection to the sun was severed, and the magnetic fields escaped into space, dragging billions of tons of solar material along for the ride — a classic CME. || ", "release_date": "2013-01-31T13:00:00-05:00", "update_date": "2025-02-02T22:09:56.411063-05:00", "main_image": { "id": 469779, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a004000/a004027/AIA171July2012CME_stand.HD1080i.01000.jpg", "filename": "AIA171July2012CME_stand.HD1080i.01000.jpg", "media_type": "Image", "alt_text": "1080 HD movie of the CME launch in the 171angstrom AIA filter.", "width": 1920, "height": 1080, "pixels": 2073600 } } }, { "id": 410473, "type": "details_page", "extra_data": null, "instance": { "id": 3920, "url": "https://svs.gsfc.nasa.gov/3920/", "page_type": "Visualization", "title": "The Rising Solar Cycle: X5.4 Flare ('W' sunspot group) seen by SDO", "description": "Sunspot group 1429 of solar cycle 24 has launched an X5.4 flare can coronal mass ejection (CME) that is forecast to impact the EarthThis visualization has the full 4Kx4K frames from the 17.1 nm and 13.1 nm filters on the Solar Dynamics Observatory. 2Kx2K MPEG-4 movies are also available. || ", "release_date": "2012-03-07T14:00:00-05:00", "update_date": "2025-02-02T22:05:54.010075-05:00", "main_image": { "id": 478377, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a003900/a003920/SDO_2012-03-07_171_X5Flare.00400_web.png", "filename": "SDO_2012-03-07_171_X5Flare.00400_web.png", "media_type": "Image", "alt_text": "The solar flare in the 171A (17.1nm) filter", "width": 320, "height": 320, "pixels": 102400 } } }, { "id": 410474, "type": "details_page", "extra_data": null, "instance": { "id": 4034, "url": "https://svs.gsfc.nasa.gov/4034/", "page_type": "Visualization", "title": "September 23, 2012 Solar Prominence", "description": "On September 23, 2012 the sun emitted a large blast of plasma in the form of a prominence (see Wikipedia). This was most visible in extreme ultraviolet light with a wavelength of 304 angstroms. This wavelength highlights plasma with temperatures of around 50,000 Kelvin. The Atmospheric Imaging Assembly on NASA's Solar Dynamics Observatory captured the event at 4k resolution and a high imaging cadence of one image every 12 seconds. || ", "release_date": "2013-02-11T10:00:00-05:00", "update_date": "2025-02-02T22:10:13.739818-05:00", "main_image": { "id": 468995, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a004000/a004034/Sept2012prominence_stand.HD1080i.00500.jpg", "filename": "Sept2012prominence_stand.HD1080i.00500.jpg", "media_type": "Image", "alt_text": "HD movie of the prominence eruption", "width": 1920, "height": 1080, "pixels": 2073600 } } }, { "id": 410475, "type": "details_page", "extra_data": null, "instance": { "id": 4033, "url": "https://svs.gsfc.nasa.gov/4033/", "page_type": "Visualization", "title": "Monster Prominences with an Earth Eclipse (September 16, 2012)", "description": "On September 16, 2012 the sun had a beautiful prominence (see Wikipedia) that slowly twisted and dissipated over several hours. It was captured in 304 angstrom light by the Solar Dynamics Observatory's AIA instrument at 4k resolution and 12s imaging cadence. The prominence was immediately followed by one of the many eclipses that SDO experiences during September, when its orbit places the Earth between it and the sun. || ", "release_date": "2013-02-11T10:00:00-05:00", "update_date": "2025-02-02T22:10:11.755299-05:00", "main_image": { "id": 468983, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a004000/a004033/Sept2012eclipse.01000_web.png", "filename": "Sept2012eclipse.01000_web.png", "media_type": "Image", "alt_text": "Full colorized 4Kx4K frames of SDO data.", "width": 320, "height": 320, "pixels": 102400 } } }, { "id": 410476, "type": "details_page", "extra_data": null, "instance": { "id": 4037, "url": "https://svs.gsfc.nasa.gov/4037/", "page_type": "Visualization", "title": "Sunspot Growth in June 2012", "description": "Groups of sunspots grow and die over a matter of days. This is a movie built from images taken by the SDO/HMI instrument over the course of 13 days during the rise of solar cycle 24. || ", "release_date": "2013-02-11T10:00:00-05:00", "update_date": "2025-02-02T22:10:16.630430-05:00", "main_image": { "id": 468841, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a004000/a004037/June2012sunspots_stand.HD1080i.00500.jpg", "filename": "June2012sunspots_stand.HD1080i.00500.jpg", "media_type": "Image", "alt_text": "An HD movie of the sunspot evolution.", "width": 1920, "height": 1080, "pixels": 2073600 } } }, { "id": 410477, "type": "details_page", "extra_data": null, "instance": { "id": 4150, "url": "https://svs.gsfc.nasa.gov/4150/", "page_type": "Visualization", "title": "January 2012 - Arcade of Coronal Loops from SDO", "description": "An arcade of coronal loops forms and erupts - upper right quadrant of disk. || ", "release_date": "2014-03-14T00:00:00-04:00", "update_date": "2023-05-03T13:51:05.486243-04:00", "main_image": { "id": 457467, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a004100/a004150/Jan2012_171A_stand.HD1080i.00067.jpg", "filename": "Jan2012_171A_stand.HD1080i.00067.jpg", "media_type": "Image", "alt_text": "Movie of the formation and eruption of an arcade of coronal loops.", "width": 1920, "height": 1080, "pixels": 2073600 } } }, { "id": 410478, "type": "details_page", "extra_data": null, "instance": { "id": 3946, "url": "https://svs.gsfc.nasa.gov/3946/", "page_type": "Visualization", "title": "One-Two Solar Punch", "description": "Two dramatic solar eruptions on the limb of the Sun, a day apart. Neither of the events were directed towards the Earth. We processed them because they are just so visually spectacular. || ", "release_date": "2012-04-17T16:00:00-04:00", "update_date": "2025-02-02T22:06:55.273744-05:00", "main_image": { "id": 476574, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a003900/a003946/SDO_2012-04-16_304_PromB.00141_web.png", "filename": "SDO_2012-04-16_304_PromB.00141_web.png", "media_type": "Image", "alt_text": "The BIG eruption from April 16, 2012.", "width": 320, "height": 320, "pixels": 102400 } } }, { "id": 410479, "type": "details_page", "extra_data": null, "instance": { "id": 4309, "url": "https://svs.gsfc.nasa.gov/4309/", "page_type": "Visualization", "title": "Blast from the Past: A Flare from January 2012", "description": "A 1080 HD Full-Disk movie of the flare event. || Jan2012Flare_171A_stand.HD1080i.01500_print.jpg (1024x576) [69.7 KB] || Jan2012Flare_171A_stand.HD1080i.01500_searchweb.png (320x180) [47.1 KB] || Jan2012Flare_171A_stand.HD1080i.01500_thm.png (80x40) [4.3 KB] || 1920x1080_16x9_30p (1920x1080) [0 Item(s)] || Jan2012Flare_171A_stand_1080p30.mp4 (1920x1080) [33.7 MB] || Jan2012Flare_171A_stand_1080p30.mov (1920x1080) [86.4 MB] || Jan2012Flare_171A_stand_1080p30.webm (1920x1080) [9.4 MB] || Jan2012Flare_171A_stand_1080p30.mp4.hwshow [197 bytes] || ", "release_date": "2015-05-28T00:00:00-04:00", "update_date": "2025-01-05T22:46:17.680759-05:00", "main_image": { "id": 443116, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a004300/a004309/Jan2012Flare_171A.01900_print.jpg", "filename": "Jan2012Flare_171A.01900_print.jpg", "media_type": "Image", "alt_text": "4Kx4K frames of the flare from Solar Dynamics Observatory (SDO) AIA instrument.", "width": 1024, "height": 1024, "pixels": 1048576 } } }, { "id": 410480, "type": "details_page", "extra_data": null, "instance": { "id": 3941, "url": "https://svs.gsfc.nasa.gov/3941/", "page_type": "Visualization", "title": "Venus Transit 2012 Composited Visuals", "description": "These visualizations were generated by compositing the small field-of-view, high-cadence closeups of Venus with the full-disk, low-cadence imagery from Solar Dynamics Observatory (SDO). Two different instruments are used: the Helioseismic and Magnetic Imager (HMI) which sees light in the visible range, and the Atmospheric Imaging Assembly (AIA) which sees light in several wavelengths in the ultraviolet range. To find out more information about these instruments, check out The Atmospheric Imaging Assembly Tutorial.Some artifacts may be visible from the compositing, but you have to look pretty closely to see them.The color table threshold was raised for these images, reducing the amount of noise visible in the images. Note: There is an interesting artifact worthy of mention and clarification, and that is as Venus crosses the solar limb, the limb appears to be visible through the planet in some of the imagers (most notably the ultraviolet channels). Discussion with the scientists who built the imagers suggest this might be 'crosstalk' between the readouts of the four CCD panels that make up a complete image. It is an artifact of the imaging system. || ", "release_date": "2012-06-11T14:00:00-04:00", "update_date": "2025-02-02T22:06:49.677445-05:00", "main_image": { "id": 475498, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a003900/a003941/AIA171VenusTransit_stand.HD1080i.00500.jpg", "filename": "AIA171VenusTransit_stand.HD1080i.00500.jpg", "media_type": "Image", "alt_text": "A high-cadence view of Venus Transit in AIA 171 angstroms.", "width": 1920, "height": 1080, "pixels": 2073600 } } }, { "id": 410481, "type": "details_page", "extra_data": null, "instance": { "id": 3940, "url": "https://svs.gsfc.nasa.gov/3940/", "page_type": "Visualization", "title": "Venus Transit 2012 from Solar Dynamics Observatory", "description": "Full disk and Tracking views of Venus Transit from Solar Dynamics Observatory (SDO). It includes images taken by the Helioseismic and Magnetic Imager (HMI) and the Atmospheric Imaging Assembly (AIA).These are the basic images, collected from the telemetry. To see the insets composited, see Venus Transit 2012 Composited Visuals. || ", "release_date": "2012-06-12T00:00:00-04:00", "update_date": "2025-01-02T13:27:41.189924-05:00", "main_image": { "id": 475538, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a003900/a003940/AIA171A_Track.00100_print.jpg", "filename": "AIA171A_Track.00100_print.jpg", "media_type": "Image", "alt_text": "Full disk and tracking view from AIA 171 Ångstroms.", "width": 854, "height": 480, "pixels": 409920 } } }, { "id": 410482, "type": "details_page", "extra_data": null, "instance": { "id": 11034, "url": "https://svs.gsfc.nasa.gov/11034/", "page_type": "Produced Video", "title": "AR1515 Releases X1.1 Class Flare", "description": "Active Region 1515 released an X1.1 class flare from the lower right of the sun on July 6, 2012, peaking at 7:08 PM EDT. This flare caused a radio blackout, labeled as an R3 on the National Oceanic and Atmospheric Administrations scale that goes from R1 to R5. Such blackouts can cause disruption to both high and low level radio frequencies.Earth's magnetosphere also underwent a minor geomagnetic storm on the evening of July 6 in response to relatively slow coronal mass ejections (CMEs) that have erupted from other regions on the sun since July 4. || ", "release_date": "2012-07-09T17:00:00-04:00", "update_date": "2023-05-03T13:52:57.182915-04:00", "main_image": { "id": 474575, "url": "https://svs.gsfc.nasa.gov/vis/a010000/a011000/a011034/July_6_flare_crop_web.jpg", "filename": "July_6_flare_crop_web.jpg", "media_type": "Image", "alt_text": "Video and still image of flare.", "width": 320, "height": 181, "pixels": 57920 } } }, { "id": 410483, "type": "details_page", "extra_data": null, "instance": { "id": 3963, "url": "https://svs.gsfc.nasa.gov/3963/", "page_type": "Visualization", "title": "Active Region 1520 from SDO", "description": "This is source material for the SDO view of Active Region 1520 in July of 2012. || ", "release_date": "2012-07-17T00:00:00-04:00", "update_date": "2025-02-02T22:07:31.994800-05:00", "main_image": { "id": 474541, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a003900/a003963/SDO_SDO_AR1520_171.00500_web.png", "filename": "SDO_SDO_AR1520_171.00500_web.png", "media_type": "Image", "alt_text": "This is 4Kx4K source frames and 1Kx1K movie of Active Region 1520.", "width": 320, "height": 320, "pixels": 102400 } } }, { "id": 410484, "type": "details_page", "extra_data": null, "instance": { "id": 3922, "url": "https://svs.gsfc.nasa.gov/3922/", "page_type": "Visualization", "title": "Growing Active Regions: January 2012", "description": "A group of active regions appear during the rise of solar cycle 25. This is a view from SDO, 171 Angstrom filter. || ", "release_date": "2012-03-31T00:00:00-04:00", "update_date": "2025-02-02T22:05:58.321026-05:00", "main_image": { "id": 477815, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a003900/a003922/SDO_Cascade_Jan2012.00500_web.png", "filename": "SDO_Cascade_Jan2012.00500_web.png", "media_type": "Image", "alt_text": "Full resolution 4Kx4K frames at 2 minutes per frame cadence.", "width": 320, "height": 320, "pixels": 102400 } } } ], "extra_data": {} }, { "id": 371279, "url": "https://svs.gsfc.nasa.gov/gallery/sdo4k-content/#media_group_371279", "widget": "Tile gallery", "title": "2011", "caption": "", "description": "", "items": [ { "id": 410485, "type": "details_page", "extra_data": null, "instance": { "id": 3955, "url": "https://svs.gsfc.nasa.gov/3955/", "page_type": "Visualization", "title": "Wispy 'Plasma Dancer' on the limb of the Sun", "description": "This movie actually exhibits a number of interesting solar phenomena.The primary feature of interest was the whirrling tower of plasma on the lower right limb. || ", "release_date": "2012-05-17T00:00:00-04:00", "update_date": "2025-02-02T22:07:04.949704-05:00", "main_image": { "id": 475949, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a003900/a003955/SDO_2011-09-25_171_Wispy.01000_web.png", "filename": "SDO_2011-09-25_171_Wispy.01000_web.png", "media_type": "Image", "alt_text": "Half resolution (2Kx2K) movies from SDO.", "width": 320, "height": 320, "pixels": 102400 } } }, { "id": 410486, "type": "details_page", "extra_data": null, "instance": { "id": 3945, "url": "https://svs.gsfc.nasa.gov/3945/", "page_type": "Visualization", "title": "Plasma 'Dance' on the Sun!", "description": "Full resolution 4Kx4K SDO images || SDO_2011-09-25_171_Wispy.00900.jpg (4096x4096) [2.2 MB] || SDO_2011-09-25_171_Wispy.00900_web.png (320x320) [100.9 KB] || SDO_2011-09-25_171_Wispy.00900_thm.png (80x40) [6.1 KB] || SDO_2011-09-25_171_Wispy.00900_searchweb.png (320x180) [96.0 KB] || SDO_2011-09-25_171_Wispy_1Kx1K.mp4 (1024x1024) [27.4 MB] || SDO_2011-09-25_171_Wispy_1Kx1K.mov (1024x1024) [27.4 MB] || SDO_2011-09-25_171_Wispy_2Kx2K.webmhd.webm (960x540) [8.1 MB] || SDO_2011-09-25_171_Wispy_2Kx2K.mp4 (2048x2048) [207.3 MB] || 4096x4096_1x1_30p (4096x4096) [0 Item(s)] || SDO_2011-09-25_171_Wispy.mp4 (4096x4096) [651.1 KB] || SDO_2011-09-25_171_Wispy_iPod.m4v (480x480) [11.3 MB] || ", "release_date": "2012-04-20T00:00:00-04:00", "update_date": "2025-02-02T22:06:53.878293-05:00", "main_image": { "id": 476615, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a003900/a003945/SDO_2011-09-25_171_Wispy.00900_web.png", "filename": "SDO_2011-09-25_171_Wispy.00900_web.png", "media_type": "Image", "alt_text": "Full resolution 4Kx4K SDO images", "width": 320, "height": 320, "pixels": 102400 } } }, { "id": 410487, "type": "details_page", "extra_data": null, "instance": { "id": 4128, "url": "https://svs.gsfc.nasa.gov/4128/", "page_type": "Visualization", "title": "Solar Dynamics Observatory - Argo view - Slices of SDO", "description": "Argos (or Argus Panoptes) was the 100-eyed giant in Greek mythology (wikipedia).While the Solar Dynamics Observatory (SDO) has significantly less than 100 eyes, (see \"SDO Jewelbox: The Many Eyes of SDO\"), seeing connections in the solar atmosphere through the many filters of SDO presents a number of interesting challenges. This visualization experiment illustrates a mechanism for highlighting these connections. This visualization is a variation of the original Solar Dynamics Observatory - Argo view. In this case, the different wavelength filters are presented in three sets around the Sun at full 4Kx4K resolution. This enables monitoring of changes in time over all wavelengths at any location around the limb of the Sun. The wavelengths presented are: 617.3nm optical light from SDO/HMI. From SDO/AIA we have 170nm (pink), then 160nm (green), 33.5nm (blue), 30.4nm (orange), 21.1nm (violet), 19.3nm (bronze), 17.1nm (gold), 13.1nm (aqua) and 9.4nm (green).We've locked the camera to rotate the view of the Sun so each wedge-shaped wavelength filter passes over a region of the Sun. As the features pass from one wavelength to the next, we can see dramatic differences in solar structures that appear in different wavelengths.Filaments extending off the limb of the Sun which are bright in 30.4 nanometers, appear dark in many other wavelengths.Sunspots which appear dark in optical wavelengths, are festooned with glowing ribbons in ultraviolet wavelengths.small flares, invisible in optical wavelengths, are bright ribbons in ultraviolet wavelengths.if we compare the visible light limb of the Sun with the 170 nanometer filter on the left, with the visible light limb and the 9.4 nanometer filter on the right, we see that the 'edge' is at different heights. This effect is due to the different amounts of absorption, and emission, of the solar atmosphere in ultraviolet light.in far ultraviolet light, the photosphere is dark since the black-body spectrum at a temperature of 5700 Kelvin emits very little light in this wavelength. || ", "release_date": "2013-12-24T00:00:00-05:00", "update_date": "2025-02-02T22:12:40.795314-05:00", "main_image": { "id": 461559, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a004100/a004128/SlicesOfSDO_rotor_stand.4Kx4K.02000_web.png", "filename": "SlicesOfSDO_rotor_stand.4Kx4K.02000_web.png", "media_type": "Image", "alt_text": "1/4 resolution full-disk movie illustrating how the different wavelength filters move around the solar image.", "width": 320, "height": 320, "pixels": 102400 } } }, { "id": 410488, "type": "details_page", "extra_data": null, "instance": { "id": 4117, "url": "https://svs.gsfc.nasa.gov/4117/", "page_type": "Visualization", "title": "Solar Dynamics Observatory - Argo view", "description": "Argos (or Argus Panoptes) was the 100-eyed giant in Greek mythology (wikipedia).While the Solar Dynamics Observatory (SDO) has significantly less than 100 eyes, (see \"SDO Jewelbox: The Many Eyes of SDO\"), seeing connections in the solar atmosphere through the many filters of SDO presents a number of interesting challenges. This visualization experiment illustrates a mechanism for highlighting these connections.The wavelengths presented are: 617.3nm optical light from SDO/HMI. From SDO/AIA we have 170nm (pink), then 160nm (green), 33.5nm (blue), 30.4nm (orange), 21.1nm (violet), 19.3nm (bronze), 17.1nm (gold), 13.1nm (aqua) and 9.4nm (green).We've locked the camera to rotate the view of the Sun so each wedge-shaped wavelength filter passes over a region of the Sun. As the features pass from one wavelength to the next, we can see dramatic differences in solar structures that appear in different wavelengths.Filaments extending off the limb of the Sun which are bright in 30.4 nanometers, appear dark in many other wavelengths.Sunspots which appear dark in optical wavelengths, are festooned with glowing ribbons in ultraviolet wavelengths.Small flares, invisible in optical wavelengths, are bright ribbons in ultraviolet wavelengths.If we compare the visible light limb of the Sun with the 170 nanometer filter on the left, with the visible light limb and the 9.4 nanometer filter on the right, we see that the 'edge' is at different heights. This effect is due to the different amounts of absorption, and emission, of the solar atmosphere in ultraviolet light.In far ultraviolet light, the photosphere is dark since the black-body spectrum at a temperature of 5700 Kelvin emits very little light in this wavelength. || ", "release_date": "2013-12-17T10:00:00-05:00", "update_date": "2025-02-02T00:04:57.026482-05:00", "main_image": { "id": 461378, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a004100/a004117/SDOargoFD_rotorzoom_stand.HD1080i.01800.jpg", "filename": "SDOargoFD_rotorzoom_stand.HD1080i.01800.jpg", "media_type": "Image", "alt_text": "The movie opens with a full-disk view of the Sun in visible wavelengths. Then the filters are applied to small pie-shaped wedges of the Sun, starting with 170nm (pink), then 160nm (green), 33.5nm (blue), 30.4nm (orange), 21.1nm (violet), 19.3nm (bronze), 17.1nm (gold), 13.1nm (aqua) and 9.4nm (green). We let the set of filters sweep around the solar disk and then zoom and rotate the camera to rotate with the filters as the solar image is rotate underneath. This video is also available on our YouTube channel.", "width": 1920, "height": 1080, "pixels": 2073600 } } }, { "id": 410489, "type": "details_page", "extra_data": null, "instance": { "id": 4049, "url": "https://svs.gsfc.nasa.gov/4049/", "page_type": "Visualization", "title": "'X' Marks the Spot: SDO Observes a Reconnection Event", "description": "This is the source data material for the main release of X Marks the Spot: SDO Sees Reconnection.Frames were generated using the standard SDO AIA 131 Å color table and an enhanced version to reveal the finer details of the coronal loops, which are overly saturated in the standard color table ranges. || ", "release_date": "2013-07-15T10:00:00-04:00", "update_date": "2023-05-03T13:52:00.385779-04:00", "main_image": { "id": 467815, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a004000/a004049/ReconnAIA131_stand.HD1080i.00108.jpg", "filename": "ReconnAIA131_stand.HD1080i.00108.jpg", "media_type": "Image", "alt_text": "A standard HD movie of the SDO/AIA 131 Å dataset.", "width": 1920, "height": 1080, "pixels": 2073600 } } }, { "id": 410490, "type": "details_page", "extra_data": null, "instance": { "id": 4151, "url": "https://svs.gsfc.nasa.gov/4151/", "page_type": "Visualization", "title": "Looking Back: The Record Flare for Solar Cycle 24", "description": "On August 9, 2011 at 3:48 a.m. EDT, the sun emitted an Earth-directed X6.9 flare, as measured by the NOAA GOES satellite. These gigantic bursts of radiation cannot pass through Earth's atmosphere to harm humans on the ground, however they can disrupt the atmosphere and disrupt GPS and communications signals. In this case, it appears the flare is strong enough to potentially cause some radio communication blackouts. It also produced increased solar energetic proton radiation — enough to affect humans in space if they do not protect themselves.As of March 2014, this flare is the largest of solar cycle 24.Here are the raw images used in creating the components in Sun Unleashes X6.9 Class Flare on August 9, 2011 || ", "release_date": "2014-05-16T00:00:00-04:00", "update_date": "2023-05-03T13:50:54.552822-04:00", "main_image": { "id": 457394, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a004100/a004151/Aug2011X6Flare_131A_stand.HD1080i.00050.jpg", "filename": "Aug2011X6Flare_131A_stand.HD1080i.00050.jpg", "media_type": "Image", "alt_text": "The X6.9 flare as seen by SDO/AIA in 13.1nm filter.", "width": 1920, "height": 1080, "pixels": 2073600 } } }, { "id": 410491, "type": "details_page", "extra_data": null, "instance": { "id": 3897, "url": "https://svs.gsfc.nasa.gov/3897/", "page_type": "Visualization", "title": "Growing Sunspots - A Full Disk View: February 2011", "description": "Here is a leisurely view of SDO/HMI data, sampled every hour, covering two weeks in the middle of February 2011. While the solar disk starts out featureless, eventually small groups of sunspots (the darker regions) emerge, grow, and then rotate out of view.For a closeup view of of one of these sunspot groups, see animation 3898, Growing Sunspots - Tracking Closeup: February 2011 || ", "release_date": "2012-01-27T00:00:00-05:00", "update_date": "2025-02-02T22:05:10.147776-05:00", "main_image": { "id": 480148, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a003800/a003897/SDOHMIFullSun2011Feb_stand.HD1080i.01000.jpg", "filename": "SDOHMIFullSun2011Feb_stand.HD1080i.01000.jpg", "media_type": "Image", "alt_text": "This movie plays a two-week long view of the Sun, sampled every hour.", "width": 1920, "height": 1080, "pixels": 2073600 } } }, { "id": 410492, "type": "details_page", "extra_data": null, "instance": { "id": 4352, "url": "https://svs.gsfc.nasa.gov/4352/", "page_type": "Visualization", "title": "Incredible Solar Flare, Prominence Eruption and CME Event (SDO/HMI visible light)", "description": "These movies present the six hour interval around the event, a one minute per animation frame. || MonsterFilament_HMI_stand.HD1080i.00100_print.jpg (1024x576) [40.8 KB] || MonsterFilament_HMI_stand.HD1080i.00100_searchweb.png (320x180) [21.8 KB] || MonsterFilament_HMI_stand.HD1080i.00100_thm.png (80x40) [2.7 KB] || MonsterFilament_HMI_stand.HD1080i.00100_web.png (320x180) [21.8 KB] || 1920x1080_16x9_30p (1920x1080) [0 Item(s)] || MonsterFilament_HMI.HD1080i_p30.mp4 (1920x1080) [12.1 MB] || MonsterFilament_HMI.HD1080i_p30.webm (1920x1080) [1.2 MB] || MonsterFilament_HMI.HD1080i_p30.mp4.hwshow [197 bytes] || ", "release_date": "2017-08-20T10:00:00-04:00", "update_date": "2025-02-02T22:22:15.115122-05:00", "main_image": { "id": 412328, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a004300/a004352/MonsterFilament_HMI.00100_print.jpg", "filename": "MonsterFilament_HMI.00100_print.jpg", "media_type": "Image", "alt_text": "These are 4Kx4K frames with coded colors.", "width": 1024, "height": 1024, "pixels": 1048576 } } }, { "id": 410493, "type": "details_page", "extra_data": null, "instance": { "id": 3838, "url": "https://svs.gsfc.nasa.gov/3838/", "page_type": "Visualization", "title": "Incredible Solar Flare, Prominence Eruption and CME Event (304 angstroms)", "description": "On June 7, 2011, an M-2 flare occurred on the Sun which released a very large coronal mass ejection (CME). Much of the ejected material is much cooler (less than about 80,000K) and therefore appears dark against the brighter solar disk.Material which does not reach solar escape velocity can be seen falling back and striking the solar surface, sometimes triggering smaller events.This image sequence is captured at one minute intervals and designed to play synchronously with animations 3839 (171 Ångstroms), 3840 (211 Ångstroms) and 3841 (1700 Ångstroms). || ", "release_date": "2011-07-01T10:00:00-04:00", "update_date": "2025-03-09T00:00:56.850075-05:00", "main_image": { "id": 484932, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a003800/a003838/SDO304FullDisk_1080HD_web.png", "filename": "SDO304FullDisk_1080HD_web.png", "media_type": "Image", "alt_text": "These movies present the six hour interval around the event, a one minute per animation frame.", "width": 320, "height": 180, "pixels": 57600 } } }, { "id": 410494, "type": "details_page", "extra_data": null, "instance": { "id": 3839, "url": "https://svs.gsfc.nasa.gov/3839/", "page_type": "Visualization", "title": "Incredible Solar Flare, Prominence Eruption and CME Event (171 angstroms)", "description": "On June 7, 2011, an M-2 flare occurred on the Sun which released a very large coronal mass ejection (CME). Much of the ejected material is much cooler (less than about 80,000K) and therefore appears dark against the brighter solar disk.Material which does not reach solar escape velocity can be seen falling back and striking the solar surface, sometimes triggering smaller events.This image sequence is captured at one minute intervals and designed to play synchronously with animations 3838 (304 Ångstroms), 3840 (211 Ångstroms) and 3841 (1700 Ångstroms). || ", "release_date": "2011-07-01T10:00:00-04:00", "update_date": "2025-02-02T00:01:24.120933-05:00", "main_image": { "id": 484965, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a003800/a003839/SDO171Full_stand.HD1080i.00100.jpg", "filename": "SDO171Full_stand.HD1080i.00100.jpg", "media_type": "Image", "alt_text": "These movies present the six hour interval around the event, a one minute per animation frame.", "width": 1920, "height": 1080, "pixels": 2073600 } } }, { "id": 410495, "type": "details_page", "extra_data": null, "instance": { "id": 3840, "url": "https://svs.gsfc.nasa.gov/3840/", "page_type": "Visualization", "title": "Incredible Solar Flare, Prominence Eruption and CME Event (211 angstroms)", "description": "On June 7, 2011, an M-2 flare occurred on the Sun which released a very large coronal mass ejection (CME). Much of the ejected material is much cooler (less than about 80,000K) and therefore appears dark against the brighter solar disk.Material which does not reach solar escape velocity can be seen falling back and striking the solar surface, sometimes triggering smaller events.This image sequence is captured at one minute intervals and designed to play synchronously with animations 3839 (171 Ångstroms), 3838 (304 Ångstroms) and 3841 (1700 Ångstroms). || ", "release_date": "2011-07-01T10:00:00-04:00", "update_date": "2025-02-02T22:02:50.495232-05:00", "main_image": { "id": 484994, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a003800/a003840/SDO211Full_stand.HD1080i.00100.jpg", "filename": "SDO211Full_stand.HD1080i.00100.jpg", "media_type": "Image", "alt_text": "These movies present the six hour interval around the event, a one minute per animation frame.", "width": 1920, "height": 1080, "pixels": 2073600 } } }, { "id": 410496, "type": "details_page", "extra_data": null, "instance": { "id": 4250, "url": "https://svs.gsfc.nasa.gov/4250/", "page_type": "Visualization", "title": "Trebuchet Solar Eruption of February 2011", "description": "The Trebuchet eruption (upper left) as seen in the SDO AIA 304 angstrom filter. This is probably one of the more popular views of the event. || Feb2011Trebuchet_304A_stand.HD1080i.00460_print.jpg (1024x576) [101.4 KB] || Feb2011Trebuchet_304A_stand.HD1080i.00460_searchweb.png (320x180) [53.5 KB] || Feb2011Trebuchet_304A_stand.HD1080i.00460_thm.png (80x40) [4.1 KB] || Feb2011Trebuchet_304A_stand.HD1080i.00460_web.png (320x180) [53.5 KB] || AIA0304A (1920x1080) [128.0 KB] || Feb2011Trebuchet_304A_HD1080.mp4 (1920x1080) [80.6 MB] || Feb2011Trebuchet_304A_HD1080.webm (1920x1080) [7.1 MB] || ", "release_date": "2015-02-11T00:00:00-05:00", "update_date": "2023-05-03T13:50:01.955925-04:00", "main_image": { "id": 447983, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a004200/a004250/Feb2011Trebuchet_304A.00460_print.jpg", "filename": "Feb2011Trebuchet_304A.00460_print.jpg", "media_type": "Image", "alt_text": "Full resolution 4Kx4K imagery for the 304 angstrom filter.", "width": 1024, "height": 1024, "pixels": 1048576 } } }, { "id": 410497, "type": "details_page", "extra_data": null, "instance": { "id": 3841, "url": "https://svs.gsfc.nasa.gov/3841/", "page_type": "Visualization", "title": "Incredible Solar Flare, Prominence Eruption and CME Event (1700 angstroms)", "description": "On June 7, 2011, an M-2 flare occurred on the Sun which released a very large coronal mass ejection (CME). At this wavelength, very little of the ejected material is visible. However, it is possible to see locations where some of the material is falling back and striking the solar surface.This image sequence is captured at one minute intervals and designed to play synchronously with animations 3839 (171 Ångstroms), 3840 (211 Ångstroms) and 3838 (304 Ångstroms). || ", "release_date": "2011-07-01T10:00:00-04:00", "update_date": "2025-02-02T22:02:51.740327-05:00", "main_image": { "id": 485027, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a003800/a003841/SDO1700Full_stand.HD1080i.00100.jpg", "filename": "SDO1700Full_stand.HD1080i.00100.jpg", "media_type": "Image", "alt_text": "These movies present the six hour interval around the event, a one minute per animation frame.", "width": 1920, "height": 1080, "pixels": 2073600 } } }, { "id": 410498, "type": "details_page", "extra_data": null, "instance": { "id": 3828, "url": "https://svs.gsfc.nasa.gov/3828/", "page_type": "Visualization", "title": "Solar Dynamics Observatory - Atmospheric Imaging Assembly", "description": "The Sun's activity increases as we enter solar cycle 24. But even several years away from the peak, the Sun in ultraviolet light shows a variety of activity.This visualization consists of eight hours of SDO AIA imagery from the 30.4 nanometer filter (304 Ångstroms). This sequence plays at the full time cadence of the AIA instrument - one image every twelve seconds of real time - and showing thirty images per second on playback. || ", "release_date": "2011-12-07T00:00:00-05:00", "update_date": "2025-02-02T22:02:39.479466-05:00", "main_image": { "id": 486460, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a003800/a003828/SDO304Full_stand.HD1080i.01500.jpg", "filename": "SDO304Full_stand.HD1080i.01500.jpg", "media_type": "Image", "alt_text": "This is a movie of the active Sun as visible in the ultraviolet 30.4 nanometers wavelength. The 4096x4096 images in the Frames area are the FULL RESOLUTION SDO images with coded colors installed.", "width": 1920, "height": 1080, "pixels": 2073600 } } }, { "id": 410499, "type": "details_page", "extra_data": null, "instance": { "id": 3933, "url": "https://svs.gsfc.nasa.gov/3933/", "page_type": "Visualization", "title": "Sunspots on the Move: August 22, 2011", "description": "SDO/HMI movie of sunspots evolving across the solar disk. || HMI_IcChangingSpots.00300.jpg (4096x4096) [3.3 MB] || HMI_IcChangingSpots.00300_web.png (320x320) [89.7 KB] || HMI_IcChangingSpots.00300_thm.png (80x40) [3.8 KB] || HMI_IcChangingSpots.00300_searchweb.png (320x180) [57.8 KB] || HMI_Ic_ChangingSpots_1Kx1K.mov (1024x1024) [28.6 MB] || HMI_Ic_ChangingSpots_4Kx4K.webmhd.webm (960x540) [3.0 MB] || HMI_Ic_ChangingSpots_2Kx2K.mov (2048x2048) [168.7 MB] || 4096x4096_1x1_30p (4096x4096) [0 Item(s)] || HMI_Ic_ChangingSpots_4Kx4K.mov (4096x4096) [17.8 GB] || ", "release_date": "2012-03-31T00:00:00-04:00", "update_date": "2025-02-02T22:06:31.734231-05:00", "main_image": { "id": 477113, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a003900/a003933/HMI_IcChangingSpots.00300_web.png", "filename": "HMI_IcChangingSpots.00300_web.png", "media_type": "Image", "alt_text": "SDO/HMI movie of sunspots evolving across the solar disk.", "width": 320, "height": 320, "pixels": 102400 } } }, { "id": 410500, "type": "details_page", "extra_data": null, "instance": { "id": 3932, "url": "https://svs.gsfc.nasa.gov/3932/", "page_type": "Visualization", "title": "Survivor 2011: Comet Lovejoy vs. The Sun", "description": "Comet Lovejoy makes a close pass to the Sun, and survives.The Solar Dynamics Observatory (SDO) is actually repointed to better observe the comet's approach to the Sun. || ", "release_date": "2012-03-31T00:00:00-04:00", "update_date": "2025-03-10T00:02:02.274996-04:00", "main_image": { "id": 477376, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a003900/a003932/LovejoyCloseup_stand.HD1080i.00600.jpg", "filename": "LovejoyCloseup_stand.HD1080i.00600.jpg", "media_type": "Image", "alt_text": "This movie zooms in for the comet approach and departure.", "width": 1920, "height": 1080, "pixels": 2073600 } } }, { "id": 410501, "type": "details_page", "extra_data": null, "instance": { "id": 3931, "url": "https://svs.gsfc.nasa.gov/3931/", "page_type": "Visualization", "title": "Launching Filament: November 14, 2011", "description": "A large filament launches from the Sun in this sequence of 304 Ångstrom imagery from Solar Dynamics Observatory. || ", "release_date": "2012-03-31T00:00:00-04:00", "update_date": "2025-02-02T22:06:28.207119-05:00", "main_image": { "id": 477362, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a003900/a003931/AIA304filament.00500_web.png", "filename": "AIA304filament.00500_web.png", "media_type": "Image", "alt_text": "Full resolution 4Kx4K frames", "width": 320, "height": 320, "pixels": 102400 } } }, { "id": 410502, "type": "details_page", "extra_data": null, "instance": { "id": 3929, "url": "https://svs.gsfc.nasa.gov/3929/", "page_type": "Visualization", "title": "A Comet's Demise: July 6, 2011", "description": "A small comet evaporates away in its flyby of the Sun. || Full resolution 4Kx4K frames || AIA171CometDemise.00390_print.jpg (4096x4096) [2.2 MB] || AIA171CometDemise.00390_web.png (320x320) [90.6 KB] || AIA171CometDemise.mp4 (1080x1080) [9.6 MB] || AIA171CometDemise.webm (1080x1080) [2.5 MB] || 4096x4096_1x1_30p (4096x4096) [0 Item(s)] || AIA171CometDemise-1.mp4 (4096x4096) [198.3 MB] || ", "release_date": "2012-03-31T00:00:00-04:00", "update_date": "2025-02-02T22:06:14.082808-05:00", "main_image": { "id": 477393, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a003900/a003929/Death2Snowball_stand.HD1080i.00390.jpg", "filename": "Death2Snowball_stand.HD1080i.00390.jpg", "media_type": "Image", "alt_text": "This movie zooms into the location where the comet is visible as it passes in front of the Sun.", "width": 1920, "height": 1080, "pixels": 2073600 } } }, { "id": 410503, "type": "details_page", "extra_data": null, "instance": { "id": 3924, "url": "https://svs.gsfc.nasa.gov/3924/", "page_type": "Visualization", "title": "Solar Prominences and Filaments: June 16, 2011", "description": "Full resolution 4Kx4K frames || AIA304flames.01600.jpg (4096x4096) [4.2 MB] || AIA304flames.01600_web.png (320x320) [118.5 KB] || AIA304flames.01600_thm.png (80x40) [5.6 KB] || AIA304flames.01600_searchweb.png (320x180) [95.8 KB] || SDOAIA304_Flames.1Kx1K.mp4 (1024x1024) [42.1 MB] || SDOAIA304_Flames.2Kx2K.webmhd.webm (960x540) [10.4 MB] || SDOAIA304_Flames.2Kx2K.mp4 (2048x2048) [215.4 MB] || 4096x4096_1x1_30p (4096x4096) [0 Item(s)] || SDOAIA304_Flames.iPod.m4v (480x480) [11.9 MB] || AIA304flames.mp4 (4096x4096) [1.0 GB] || ", "release_date": "2012-03-31T00:00:00-04:00", "update_date": "2025-02-02T22:06:04.392963-05:00", "main_image": { "id": 477833, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a003900/a003924/AIA304flames.01600_web.png", "filename": "AIA304flames.01600_web.png", "media_type": "Image", "alt_text": "Full resolution 4Kx4K frames", "width": 320, "height": 320, "pixels": 102400 } } }, { "id": 410504, "type": "details_page", "extra_data": null, "instance": { "id": 3923, "url": "https://svs.gsfc.nasa.gov/3923/", "page_type": "Visualization", "title": "The Active Region Trio: October 2011", "description": "A group of solar active regions, observed in October 2011 by SDO in the 171 Angstrom filter. || ", "release_date": "2012-03-31T00:00:00-04:00", "update_date": "2025-02-02T22:05:59.673731-05:00", "main_image": { "id": 477823, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a003900/a003923/SDO_SDO3energized.02500_web.png", "filename": "SDO_SDO3energized.02500_web.png", "media_type": "Image", "alt_text": "4K by 4K frames", "width": 320, "height": 320, "pixels": 102400 } } }, { "id": 410505, "type": "details_page", "extra_data": null, "instance": { "id": 4277, "url": "https://svs.gsfc.nasa.gov/4277/", "page_type": "Visualization", "title": "July 12, 2011: A Bright Limb Prominence from Solar Dynamics Observatory", "description": "HD movie of solar prominence launch in the AIA 304 angstrom filter (upper left limb of Sun). || July2011Prominence_304A_stand.HD1080i.00600_print.jpg (1024x576) [92.4 KB] || July2011Prominence_304A_stand.HD1080i.00600_searchweb.png (320x180) [45.8 KB] || July2011Prominence_304A_stand.HD1080i.00600_thm.png (80x40) [3.8 KB] || July2011Prominence_304A.HD1080.webm (1920x1080) [4.7 MB] || July2011Prominence_304A.HD1080.mov (1920x1080) [128.8 MB] || July2011Prominence_304AHD (1920x1080) [128.0 KB] || July2011Prominence_304A_stand_HD1080.mp4 (1920x1080) [45.4 MB] || ", "release_date": "2015-03-03T00:00:00-05:00", "update_date": "2023-05-03T13:49:55.252810-04:00", "main_image": { "id": 445985, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a004200/a004277/July2011Prominence_304A.00400_print.jpg", "filename": "July2011Prominence_304A.00400_print.jpg", "media_type": "Image", "alt_text": "Full resolution 4Kx4K image sequence of solar prominence launch in the AIA 304 angstrom filter (upper left limb of Sun).", "width": 1024, "height": 1024, "pixels": 1048576 } } }, { "id": 410506, "type": "details_page", "extra_data": null, "instance": { "id": 3957, "url": "https://svs.gsfc.nasa.gov/3957/", "page_type": "Visualization", "title": "Solar Flare from SDO, April 2011 (AIA 94 Å)", "description": "The Solar Dynamics Observatory (SDO) observed a large solar flare in April 2011.This visualization was generated using quick-look time resolution (36 seconds) data from the Atmospheric Imaging Assembly (AIA). Two datasets are used, the SDO/AIA 94 Ångstrom wavelength (green color table). This wavelength is in the ultraviolet band of the electromagnetic spectrum. It is not visible to the human eye or to ground-based telescopes so coded colors are used in presentation.It is the source material for \"SDO Year 2 video\". || ", "release_date": "2012-08-24T00:00:00-04:00", "update_date": "2025-02-02T22:07:09.323098-05:00", "main_image": { "id": 473262, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a003900/a003957/SDO_Flare_94_April2011.01000_web.png", "filename": "SDO_Flare_94_April2011.01000_web.png", "media_type": "Image", "alt_text": "Movie of the solar flare from April 2011. 4Kx4K source frames and 1Kx1K movies", "width": 320, "height": 320, "pixels": 102400 } } }, { "id": 410507, "type": "details_page", "extra_data": null, "instance": { "id": 3978, "url": "https://svs.gsfc.nasa.gov/3978/", "page_type": "Visualization", "title": "The Active Sun from SDO: 94 Ångstroms", "description": "The Solar Dynamics Observatory (SDO) observes the Sun with many different instruments, in many different wavelengths of light. Many of these capabilities are not possible for ground-based observatories - hence the need for a space-based observing platform.This movie is generated for a wavelength of 94 Ångstroms (9.4 nanometers) which highlights a spectral line emitted by iron atoms that have lost 17 electrons (also known as iron-18 or Fe XVIII) at temperatures of 6,000,000 K. Temperatures like this represent regions of the corona during a solar flare.This visualization is one of a set of visualizations (others linked below) covering the same time span of 17 hours over the full wavelength range of the instruments. They are setup to play synchronously on a Hyperwall, or can be run individually.The images are sampled every 36 seconds, 1/3 of the standard 12 second time-cadence for SDO. This visualization is useful for illustrating how different solar phenomena, such as sunspots and active regions, look very different in different wavelengths of light. These differences enable scientists to study them more completely, with an eventual goal of improving Space Weather forecasting. || ", "release_date": "2012-11-20T09:00:00-05:00", "update_date": "2025-02-02T22:08:03.275956-05:00", "main_image": { "id": 472643, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a003900/a003978/SDOAIA094A_Jewelbox_stand.HD1080i.01000.jpg", "filename": "SDOAIA094A_Jewelbox_stand.HD1080i.01000.jpg", "media_type": "Image", "alt_text": "Stand-alone full-disk movies of AIA 94Ångstrom imagery.", "width": 1920, "height": 1080, "pixels": 2073600 } } }, { "id": 410508, "type": "details_page", "extra_data": null, "instance": { "id": 3979, "url": "https://svs.gsfc.nasa.gov/3979/", "page_type": "Visualization", "title": "The Active Sun from SDO: 131 Ångstroms", "description": "The Solar Dynamics Observatory (SDO) observes the Sun with many different instruments, in many different wavelengths of light. Many of these capabilities are not possible for ground-based observatories - hence the need for a space-based observing platform.This movie is generated for a wavelength of 131 Ångstroms (13.1 nanometers) which highlights a spectral line emitted by iron atoms that have lost 19 and 22 electrons (also known as iron-20 or Fe XX; and iron-23 or FeXXIII) at temperatures of 10,000,000 K. Temperatures like this represent material in a solar flare.This visualization is one of a set of visualizations (others linked below) covering the same time span of 17 hours over the full wavelength range of the mission. They are setup to play synchronously on a Hyperwall, or can be run individually.The images are sampled every 36 seconds, 1/3 of the standard time-cadence for SDO. This visualization is useful for illustrating how different solar phenomena, such as sunspots and active regions, look very different in different wavelengths of light. These differences enable scientists to study them more completely, with an eventual goal of improving Space Weather forecasting. || ", "release_date": "2012-11-20T09:00:00-05:00", "update_date": "2025-02-02T22:08:07.040171-05:00", "main_image": { "id": 472601, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a003900/a003979/SDOAIA131A_Jewelbox_stand.HD1080i.00100.jpg", "filename": "SDOAIA131A_Jewelbox_stand.HD1080i.00100.jpg", "media_type": "Image", "alt_text": "Stand-alone HD1080 Movie of AIA 131Å imagery.", "width": 1920, "height": 1080, "pixels": 2073600 } } }, { "id": 410509, "type": "details_page", "extra_data": null, "instance": { "id": 3980, "url": "https://svs.gsfc.nasa.gov/3980/", "page_type": "Visualization", "title": "The Active Sun from SDO: 171 Ångstroms", "description": "The Solar Dynamics Observatory (SDO) observes the Sun with many different instruments, in many different wavelengths of light. Many of these capabilities are not possible for ground-based observatories - hence the need for a space-based observing platform.This movie is generated for a wavelength of 171 Ångstroms (17.1 nanometers) which highlights a spectral line emitted by iron atoms that have lost 8 electrons (also known as iron-9 or Fe IX) at temperatures of 600,000 K. Temperatures like this show the quiet corona and magnetic structures like coronal loops.This visualization is one of a set of visualizations (others linked below) covering the same time span of 17 hours over the full wavelength range of the mission. They are setup to play synchronously on a Hyperwall, or can be run individually.The images are sampled every 36 seconds, 1/3 of the standard time-cadence for SDO. This visualization is useful for illustrating how different solar phenomena, such as sunspots and active regions, look very different in different wavelengths of light. These differences enable scientists to study them more completely, with an eventual goal of improving Space Weather forecasting. || ", "release_date": "2012-11-20T09:00:00-05:00", "update_date": "2025-02-02T22:08:10.685348-05:00", "main_image": { "id": 472653, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a003900/a003980/SDOAIA171A_Jewelbox_stand.HD1080i.00100.jpg", "filename": "SDOAIA171A_Jewelbox_stand.HD1080i.00100.jpg", "media_type": "Image", "alt_text": "Stand-alone HD1080 movie of AIA 171Å imagery.", "width": 1920, "height": 1080, "pixels": 2073600 } } }, { "id": 410510, "type": "details_page", "extra_data": null, "instance": { "id": 3981, "url": "https://svs.gsfc.nasa.gov/3981/", "page_type": "Visualization", "title": "The Active Sun from SDO: 193 Ångstroms", "description": "The Solar Dynamics Observatory (SDO) observes the Sun with many different instruments, in many different wavelengths of light. Many of these capabilities are not possible for ground-based observatories - hence the need for a space-based observing platform.This movie is generated for a wavelength of 193 Ångstroms (19.3 nanometers) which highlights a spectral line emitted by iron atoms that have lost 11 electrons (also known as iron-12 or Fe XII) at temperatures of 1,000,000 K as well as iron atoms that have lost 23 electrons (also known as iron-24 or FeXXIV) at temperatures of 20,000,000K. The former represents a slightly higher region of the corona and the latter represents the much hotter material of a solar flare. This wavelength also makes coronal holes (which appear as dark regions near the solar surface) more visible.This visualization is one of a set of visualizations (others linked below) covering the same time span of 17 hours over the full wavelength range of the mission. They are setup to play synchronously on a Hyperwall, or can be run individually.The images are sampled every 36 seconds, 1/3 of the standard time-cadence for SDO. This visualization is useful for illustrating how different solar phenomena, such as sunspots and active regions, look very different in different wavelengths of light. These differences enable scientists to study them more completely, with an eventual goal of improving Space Weather forecasting. || ", "release_date": "2012-11-20T09:00:00-05:00", "update_date": "2025-02-02T22:08:14.324768-05:00", "main_image": { "id": 472670, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a003900/a003981/SDOAIA193A_Jewelbox_stand.HD1080i.00100.jpg", "filename": "SDOAIA193A_Jewelbox_stand.HD1080i.00100.jpg", "media_type": "Image", "alt_text": "Stand-alone HD1080 movie of AIA 193 Å imagery.", "width": 1920, "height": 1080, "pixels": 2073600 } } }, { "id": 410511, "type": "details_page", "extra_data": null, "instance": { "id": 3982, "url": "https://svs.gsfc.nasa.gov/3982/", "page_type": "Visualization", "title": "The Active Sun from SDO: 211 Ångstroms", "description": "The Solar Dynamics Observatory (SDO) observes the Sun with many different instruments, in many different wavelengths of light. Many of these capabilities are not possible for ground-based observatories - hence the need for a space-based observing platform.This movie is generated for a wavelength of 211 Ångstroms (21.1 nanometers) which highlights a spectral line emitted by iron atoms that have lost 13 electrons (also known as iron-14 or Fe XIV) at temperatures of 2,000,000 K. These images show hotter, active regions in the sun's corona.This visualization is one of a set of visualizations (others linked below) covering the same time span of 17 hours over the full wavelength range of the mission. They are setup to play synchronously on a Hyperwall, or can be run individually.The images are sampled every 36 seconds, 1/3 of the standard time-cadence for SDO. This visualization is useful for illustrating how different solar phenomena, such as sunspots and active regions, look very different in different wavelengths of light. These differences enable scientists to study them more completely, with an eventual goal of improving Space Weather forecasting. || ", "release_date": "2012-11-20T09:00:00-05:00", "update_date": "2025-02-02T22:08:17.979816-05:00", "main_image": { "id": 472618, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a003900/a003982/SDOAIA211A_Jewelbox_stand.HD1080i.00100.jpg", "filename": "SDOAIA211A_Jewelbox_stand.HD1080i.00100.jpg", "media_type": "Image", "alt_text": "Stand-alone HD1080 movie of AIA 211 Å imagery", "width": 1920, "height": 1080, "pixels": 2073600 } } }, { "id": 410512, "type": "details_page", "extra_data": null, "instance": { "id": 3983, "url": "https://svs.gsfc.nasa.gov/3983/", "page_type": "Visualization", "title": "The Active Sun from SDO: 304 Ångstroms", "description": "The Solar Dynamics Observatory (SDO) observes the Sun with many different instruments, in many different wavelengths of light. Many of these capabilities are not possible for ground-based observatories - hence the need for a space-based observing platform.This movie is generated for a wavelength of 304 Ångstroms (30.4 nanometers) which highlights a spectral line emitted by helium atoms that have lost 1 electron (also known as helium-2 or He II) at temperatures of 50,000 K. This light is emitted from the upper transition region and the chromosphere. Solar prominences are readily visible at this wavelength.This visualization is one of a set of visualizations (others linked below) covering the same time span of 17 hours over the full wavelength range of the mission. They are setup to play synchronously on a Hyperwall, or can be run individually.The images are sampled every 36 seconds, 1/3 of the standard time-cadence for SDO. This visualization is useful for illustrating how different solar phenomena, such as sunspots and active regions, look very different in different wavelengths of light. These differences enable scientists to study them more completely, with an eventual goal of improving Space Weather forecasting. || ", "release_date": "2012-11-20T09:00:00-05:00", "update_date": "2025-02-02T22:08:21.663673-05:00", "main_image": { "id": 472687, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a003900/a003983/SDOAIA304A_Jewelbox_stand.HD1080i.00100.jpg", "filename": "SDOAIA304A_Jewelbox_stand.HD1080i.00100.jpg", "media_type": "Image", "alt_text": "Stand-alone HD1080 movie of AIA 304 ", "width": 1920, "height": 1080, "pixels": 2073600 } } }, { "id": 410513, "type": "details_page", "extra_data": null, "instance": { "id": 3984, "url": "https://svs.gsfc.nasa.gov/3984/", "page_type": "Visualization", "title": "The Active Sun from SDO: 335 Ångstroms", "description": "The Solar Dynamics Observatory (SDO) observes the Sun with many different instruments, in many different wavelengths of light. Many of these capabilities are not possible for ground-based observatories - hence the need for a space-based observing platform.This movie is generated for a wavelength of 335 Ångstroms (33.5 nanometers) which highlights a spectral line of iron that has lost 15 electrons (also known as iron-16 or Fe XVI) at temperatures of 2,500,000 K. These images show active regions in the corona.This visualization is one of a set of visualizations (others linked below) covering the same time span of 17 hours over the full wavelength range of the mission. They are setup to play synchronously on a Hyperwall, or can be run individually.The images are sampled every 36 seconds, 1/3 of the standard time-cadence for SDO. This visualization is useful for illustrating how different solar phenomena, such as sunspots and active regions, look very different in different wavelengths of light. These differences enable scientists to study them more completely, with an eventual goal of improving Space Weather forecasting. || ", "release_date": "2012-11-20T09:00:00-05:00", "update_date": "2025-02-02T22:08:25.435603-05:00", "main_image": { "id": 472584, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a003900/a003984/SDOAIA335A_Jewelbox_stand.HD1080i.00100.jpg", "filename": "SDOAIA335A_Jewelbox_stand.HD1080i.00100.jpg", "media_type": "Image", "alt_text": "Stand-alone HD1080 movie of AIA 335 Å imagery", "width": 1920, "height": 1080, "pixels": 2073600 } } }, { "id": 410514, "type": "details_page", "extra_data": null, "instance": { "id": 3985, "url": "https://svs.gsfc.nasa.gov/3985/", "page_type": "Visualization", "title": "The Active Sun from SDO: 1600 Ångstroms", "description": "The Solar Dynamics Observatory (SDO) observes the Sun with many different instruments, in many different wavelengths of light. Many of these capabilities are not possible for ground-based observatories - hence the need for a space-based observing platform.This movie is generated for a wavelength of 1600 Ångstroms (160.0 nanometers) which highlights a spectral line of carbon that has lost 3 electrons (also known as carbon-4 or C-IV) at temperatures of 10,000 K. C IV at these temperatures is present in what's called the transition region between the sun's surface and the lowest levels of the sun's atmosphere, the chromosphere.This visualization is one of a set of visualizations (others linked below) covering the same time span of 17 hours over the full wavelength range of the mission. They are setup to play synchronously on a Hyperwall, or can be run individually.The images are sampled every 36 seconds, 1/3 of the standard time-cadence for SDO. This visualization is useful for illustrating how different solar phenomena, such as sunspots and active regions, look very different in different wavelengths of light. These differences enable scientists to study them more completely, with an eventual goal of improving Space Weather forecasting. || ", "release_date": "2012-11-20T09:00:00-05:00", "update_date": "2025-02-02T22:08:29.329987-05:00", "main_image": { "id": 472704, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a003900/a003985/SDOAIA1600A_Jewelbox_stand.HD1080i.00100.jpg", "filename": "SDOAIA1600A_Jewelbox_stand.HD1080i.00100.jpg", "media_type": "Image", "alt_text": "Stand-alone HD1080 movie of AIA 1600 Å imagery", "width": 1920, "height": 1080, "pixels": 2073600 } } }, { "id": 410515, "type": "details_page", "extra_data": null, "instance": { "id": 3986, "url": "https://svs.gsfc.nasa.gov/3986/", "page_type": "Visualization", "title": "The Active Sun from SDO: 1700 Ångstroms", "description": "The Solar Dynamics Observatory (SDO) observes the Sun with many different instruments, in many different wavelengths of light. Many of these capabilities are not possible for ground-based observatories - hence the need for a space-based observing platform.This movie is generated for a wavelength of 1700 Ånstroms (170.0 nanometers) which is in the ultraviolet band showing the lower level of the Sun's atmosphere, called the chromosphere.This visualization is one of a set of visualizations (others linked below) covering the same time span of 17 hours over the full wavelength range of the mission. They are setup to play synchronously on a Hyperwall, or can be run individually.The images are sampled every 36 seconds, 1/3 of the standard time-cadence for SDO. This visualization is useful for illustrating how different solar phenomena, such as sunspots and active regions, look very different in different wavelengths of light. These differences enable scientists to study them more completely, with an eventual goal of improving Space Weather forecasting. || ", "release_date": "2012-11-20T09:00:00-05:00", "update_date": "2025-02-02T22:08:33.314242-05:00", "main_image": { "id": 472721, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a003900/a003986/SDOAIA1700A_Jewelbox_stand.HD1080i.00100.jpg", "filename": "SDOAIA1700A_Jewelbox_stand.HD1080i.00100.jpg", "media_type": "Image", "alt_text": "Stand-alone HD1080 movie of AIA 1700 Å imagery", "width": 1920, "height": 1080, "pixels": 2073600 } } }, { "id": 410516, "type": "details_page", "extra_data": null, "instance": { "id": 3987, "url": "https://svs.gsfc.nasa.gov/3987/", "page_type": "Visualization", "title": "The Active Sun from SDO: 4500 Ångstroms", "description": "The Solar Dynamics Observatory (SDO) observes the Sun with many different instruments, in many different wavelengths of light. Many of these capabilities are not possible for ground-based observatories - hence the need for a space-based observing platform.This movie is generated for a wavelength of 4500 Ångstroms (450.0 nanometers) which corresponds to visible light, showing the Sun's visible surface, or photosphere. This wavelength can also be seen from the surface of the Earth, though not with the clarity possible from SDO. The dark regions on the left side are sunspots (Wikipedia) - essentially magnetic storms in the photosphere.This visualization is one of a set of visualizations (others linked below) covering the same time span of 17 hours over the full wavelength range of the mission. They are setup to play synchronously on a Hyperwall, or can be run individually.The images are sampled every 36 seconds, 1/3 of the standard time-cadence for SDO. This visualization is useful for illustrating how different solar phenomena, such as sunspots and active regions, look very different in different wavelengths of light. These differences enable scientists to study them more completely, with an eventual goal of improving Space Weather forecasting. || ", "release_date": "2012-11-20T09:00:00-05:00", "update_date": "2025-02-02T22:08:37.201367-05:00", "main_image": { "id": 472738, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a003900/a003987/SDOAIA4500A_Jewelbox_stand.HD1080i.00100.jpg", "filename": "SDOAIA4500A_Jewelbox_stand.HD1080i.00100.jpg", "media_type": "Image", "alt_text": "Stand-alone HD1080 movie of AIA 4500 Å imagery", "width": 1920, "height": 1080, "pixels": 2073600 } } }, { "id": 410517, "type": "details_page", "extra_data": null, "instance": { "id": 3989, "url": "https://svs.gsfc.nasa.gov/3989/", "page_type": "Visualization", "title": "The Active Sun from SDO: HMI Magnetogram", "description": "The Solar Dynamics Observatory (SDO) observes the Sun with many different instruments, in many different wavelengths of light. Many of these capabilities are not possible for ground-based observatories - hence the need for a space-based observing platform.The Helioseismic Magnetic Imager (HMI) aboard the Solar Dynamics Observatory takes a series of images every 45 seconds in a very narrow range of wavelengths in visible light of the solar photosphere. The wavelengths correspond to a region around the 6173 Ångstroms (617.3 nanometers) spectral line of neutral iron (Fe I). From this series of images, it constructs a set of images which extract other characteristics of the photosphere. For this dataset, it measures the splitting of the spectral lines to determine the intensity of the magnetic field on the solar surface. White represents north magnetic polarity and black represents south magnetic polarity.This visualization is one of a set of visualizations (others linked below) covering the same time span of 17 hours over the full wavelength range of the mission. They are setup to play synchronously on a Hyperwall, or can be run individually.The images are sampled every 36 seconds, 1/3 of the standard time-cadence for SDO. This visualization is useful for illustrating how different solar phenomena, such as sunspots and active regions, look very different in different wavelengths of light. These differences enable scientists to study them more completely, with an eventual goal of improving Space Weather forecasting. || ", "release_date": "2012-11-20T09:00:00-05:00", "update_date": "2025-02-02T22:08:45.089433-05:00", "main_image": { "id": 472772, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a003900/a003989/SDOHMImagnetogram_Jewelbox_stand.HD1080i.00100.jpg", "filename": "SDOHMImagnetogram_Jewelbox_stand.HD1080i.00100.jpg", "media_type": "Image", "alt_text": "Stand-alone HD1080 movie of the HMI magnetograms.", "width": 1920, "height": 1080, "pixels": 2073600 } } }, { "id": 410518, "type": "details_page", "extra_data": null, "instance": { "id": 3990, "url": "https://svs.gsfc.nasa.gov/3990/", "page_type": "Visualization", "title": "The Active Sun from SDO: HMI Dopplergram", "description": "The Solar Dynamics Observatory (SDO) observes the Sun with many different instruments, in many different wavelengths of light. Many of these capabilities are not possible for ground-based observatories - hence the need for a space-based observing platform.The Helioseismic Magnetic Imager (HMI) aboard the Solar Dynamics Observatory takes a series of images every 45 seconds in a very narrow range of wavelengths in visible light of the solar photosphere. The wavelengths correspond to a region around the 6173 Ångstroms (617.3 nanometers) spectral line of neutral iron (Fe I). From this series of images, it constructs a set of images which extract other characteristics of the photosphere. For this dataset, it measures the shifting of the spectral lines to determine the velocity of gas flows on the solar surface. This spectral line shift is due to the Doppler effect (Wikipedia). Blue represents motion towards the observer. Red indicates motion away from the observer. For the images below, the color is dominated by the solar rotation, so the solar limb on the right is moving away from us (and therefore red) while the left limb is moving towards us (and therefore blue). Motions on the solar surface generate the rippling in the color and you can see evidence of surface flows around the sunspot near the left limb. This visualization is one of a set of visualizations (others linked below) covering the same time span of 17 hours over the full wavelength range of the mission. They are setup to play synchronously on a Hyperwall, or can be run individually.The images are sampled every 36 seconds, 1/3 of the standard time-cadence for SDO. This visualization is useful for illustrating how different solar phenomena, such as sunspots and active regions, look very different in different wavelengths of light. These differences enable scientists to study them more completely, with an eventual goal of improving Space Weather forecasting. || ", "release_date": "2012-11-20T09:00:00-05:00", "update_date": "2025-02-02T22:08:49.145735-05:00", "main_image": { "id": 472789, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a003900/a003990/SDOHMIdoppler_Jewelbox_stand.HD1080i.00100.jpg", "filename": "SDOHMIdoppler_Jewelbox_stand.HD1080i.00100.jpg", "media_type": "Image", "alt_text": "Stand-alone movie of the HMI dopplergrams", "width": 1920, "height": 1080, "pixels": 2073600 } } }, { "id": 410519, "type": "details_page", "extra_data": null, "instance": { "id": 3988, "url": "https://svs.gsfc.nasa.gov/3988/", "page_type": "Visualization", "title": "The Active Sun from SDO: HMI Intensity", "description": "The Solar Dynamics Observatory (SDO) observes the Sun with many different instruments, in many different wavelengths of light. Many of these capabilities are not possible for ground-based observatories - hence the need for a space-based observing platform.The Helioseismic Magnetic Imager (HMI) aboard the Solar Dynamics Observatory takes a series of images every 45 seconds in a very narrow range of wavelengths in visible light of the solar photosphere. The wavelengths correspond to a region around the 6173 Ångstroms (617.3 nanometers) spectral line of neutral iron (Fe I). From this series of images, it constructs a set of images which extract other characteristics of the photosphere. For this dataset, it shows the solar photosphere in visible light.This visualization is one of a set of visualizations (others linked below) covering the same time span of 17 hours over the full wavelength range of the mission. They are setup to play synchronously on a Hyperwall, or can be run individually.The images are sampled every 36 seconds, 1/3 of the standard time-cadence for SDO. This visualization is useful for illustrating how different solar phenomena, such as sunspots and active regions, look very different in different wavelengths of light. These differences enable scientists to study them more completely, with an eventual goal of improving Space Weather forecasting. || ", "release_date": "2012-11-20T09:00:00-05:00", "update_date": "2025-02-02T22:08:41.109953-05:00", "main_image": { "id": 472755, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a003900/a003988/SDOHMIintensity_Jewelbox_stand.HD1080i.00100.jpg", "filename": "SDOHMIintensity_Jewelbox_stand.HD1080i.00100.jpg", "media_type": "Image", "alt_text": "Stand-alone movies of HMI intensity imagery.", "width": 1920, "height": 1080, "pixels": 2073600 } } } ], "extra_data": {} }, { "id": 371280, "url": "https://svs.gsfc.nasa.gov/gallery/sdo4k-content/#media_group_371280", "widget": "Card gallery", "title": "2010", "caption": "", "description": "", "items": [ { "id": 410520, "type": "details_page", "extra_data": null, "instance": { "id": 3965, "url": "https://svs.gsfc.nasa.gov/3965/", "page_type": "Visualization", "title": "Impressionist Sun: SDO Source Images", "description": "A set of multi-wavelength views of the Sun from SDO provided source and context imagery for the Van Gogh Sun video. This video illustrates how imagery is converted into physical parameters teaching us more about the physical processes taking place in the solar atmosphere. || ", "release_date": "2012-07-20T00:00:00-04:00", "update_date": "2023-05-03T13:52:55.046495-04:00", "main_image": { "id": 474307, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a003900/a003965/AIA094_Impressions.00001.jpg", "filename": "AIA094_Impressions.00001.jpg", "media_type": "Image", "alt_text": "Input data for the Van Gogh Sun, 94Å.", "width": 4096, "height": 4096, "pixels": 16777216 } } }, { "id": 410521, "type": "details_page", "extra_data": null, "instance": { "id": 4075, "url": "https://svs.gsfc.nasa.gov/4075/", "page_type": "Visualization", "title": "Lunar Transit from Solar Dynamics Observatory (2010)", "description": "Just as we do on Earth, the Solar Dynamics Observatory satellite periodically crosses the Moon's shadow and experiences a solar eclipse. During the eclipse witnessed by SDO on October 7, 2010, the southern hemisphere of the Moon was silhouetted against the solar disk, revealing some especially prominent mountain peaks near the Moon's south pole. By using elevation data from Lunar Reconnaissance Orbiter to visualize the Moon from SDO's point of view, it's possible to identify these peaks. Although all of these are well-known features, all but one of them have no official names. The following list corresponds to the labels in the animation, from left to right.In his 1954 sketch of the lunar south pole, astronomer Ewen Whitaker labeled this feature \"M3.\" It's a mountain about halfway between the craters Cabeus and Drygalski, at 83.2°S 68°W.Whitaker's \"M1,\" a mountain on the northern rim of Cabeus, 83.4°S 33°W.A mountain on the southern rim of Malapert crater, about halfway between the centers of Malapert and Haworth. Whitaker labels this Malapert Alpha. It's also known as Mons Malapert or Malapert Peak. 85.8°S 0°E.Labeled Leibnitz Beta by Whitaker and now officially named Mons Mouton, this is part of the highlands adjacent to the northern rim of Nobile crater. 84°S 37°E. Part of the Leibnitz mountain range first identified by Johann Schröter in the late 1700s, unrelated to Leibnitz Crater on the lunar far side.A mountain near Amundsen crater, on the western (Earthward) rim of Hédervári crater, 82.2°S 75°E. Whitaker tentatively labels this Leibnitz Epsilon in his sketch.The Moon visualization uses the latest albedo and elevation maps from Lunar Reconnaissance Orbiter (LRO). || ", "release_date": "2013-06-12T10:00:00-04:00", "update_date": "2025-02-02T22:11:14.692179-05:00", "main_image": { "id": 465571, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a004000/a004075/sdomoon.0230_print.jpg", "filename": "sdomoon.0230_print.jpg", "media_type": "Image", "alt_text": "The southern limb of the Moon transits across the Sun in this sequence of images from Solar Dynamics Observatory on October 7, 2010. Five peaks near the lunar south pole, visible in silhouette, are identified. A visualization of the Moon using Lunar Reconnaissance Orbiter data is precisely aligned with the SDO image, then rotated to show these five peaks on a false-color global elevation map.This video is also available on our YouTube channel.", "width": 1024, "height": 576, "pixels": 589824 } } } ], "extra_data": {} } ] }