To have a record of such an intense flare from so many observatories is unprecedented. Such research can help scientists better understand what catalyst sets off these large explosions on the sun. Perhaps we may even some day be able to predict their onset and forewarn of the radio blackouts solar flares can cause near Earth – blackouts that can interfere with airplane, ship and military communications.", "items": [], "extra_data": {} }, { "id": 344764, "url": "https://svs.gsfc.nasa.gov/11522/#media_group_344764", "widget": "Video player", "title": "", "caption": "", "description": "A web short about the multi-spacecraft observations of the March 29, 2014 X-class flare.
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Credit: NASA/SDO/HMI
", "items": [ { "id": 304752, "type": "media", "extra_data": null, "title": null, "caption": null, "instance": { "id": 455496, "url": "https://svs.gsfc.nasa.gov/vis/a010000/a011500/a011522/C_SDO_HMI_magnetogram_20140329_17_48.png", "filename": "C_SDO_HMI_magnetogram_20140329_17_48.png", "media_type": "Image", "alt_text": "NASA's Solar Dynamics Observatory captures magnetic information about the surface of the sun. Dark areas in this image from 1:48 p.m. EDT on March 29, 2014, show where magnetic field lines point into the surface during the X-class flare. The white areas show where the field lines point out. This information helps unravel the complex magnetic system on and around the sun, which can lead to large eruptive events like solar flares.Credit: NASA/SDO/HMI", "width": 1362, "height": 808, "pixels": 1100496 } }, { "id": 304753, "type": "media", "extra_data": null, "title": null, "caption": null, "instance": { "id": 455495, "url": "https://svs.gsfc.nasa.gov/vis/a010000/a011500/a011522/C_SDO_HMI_magnetogram_20140329_17_48_web.jpg", "filename": "C_SDO_HMI_magnetogram_20140329_17_48_web.jpg", "media_type": "Image", "alt_text": "NASA's Solar Dynamics Observatory captures magnetic information about the surface of the sun. Dark areas in this image from 1:48 p.m. EDT on March 29, 2014, show where magnetic field lines point into the surface during the X-class flare. The white areas show where the field lines point out. This information helps unravel the complex magnetic system on and around the sun, which can lead to large eruptive events like solar flares.Credit: NASA/SDO/HMI", "width": 319, "height": 189, "pixels": 60291 } }, { "id": 304754, "type": "media", "extra_data": null, "title": null, "caption": null, "instance": { "id": 455494, "url": "https://svs.gsfc.nasa.gov/vis/a010000/a011500/a011522/C_SDO_HMI_magnetogram_20140329_17_48_web.png", "filename": "C_SDO_HMI_magnetogram_20140329_17_48_web.png", "media_type": "Image", "alt_text": "NASA's Solar Dynamics Observatory captures magnetic information about the surface of the sun. Dark areas in this image from 1:48 p.m. EDT on March 29, 2014, show where magnetic field lines point into the surface during the X-class flare. The white areas show where the field lines point out. This information helps unravel the complex magnetic system on and around the sun, which can lead to large eruptive events like solar flares.Credit: NASA/SDO/HMI", "width": 320, "height": 189, "pixels": 60480 } }, { "id": 304755, "type": "media", "extra_data": null, "title": null, "caption": null, "instance": { "id": 455493, "url": "https://svs.gsfc.nasa.gov/vis/a010000/a011500/a011522/C_SDO_HMI_magnetogram_20140329_17_48_thm.png", "filename": "C_SDO_HMI_magnetogram_20140329_17_48_thm.png", "media_type": "Image", "alt_text": "NASA's Solar Dynamics Observatory captures magnetic information about the surface of the sun. Dark areas in this image from 1:48 p.m. EDT on March 29, 2014, show where magnetic field lines point into the surface during the X-class flare. The white areas show where the field lines point out. This information helps unravel the complex magnetic system on and around the sun, which can lead to large eruptive events like solar flares.Credit: NASA/SDO/HMI", "width": 80, "height": 40, "pixels": 3200 } } ], "extra_data": {} }, { "id": 344768, "url": "https://svs.gsfc.nasa.gov/11522/#media_group_344768", "widget": "Single image", "title": "", "caption": "", "description": "In these images of the solar corona showing light in the 171 angstrom wavelength, the March 29, 2014, flare can barely be seen. However light in this wavelength does clearly show the beautiful loops of charged particles – tracing out the sun's magnetic field lines — that can clearly be seen rising up on the sun's horizon.
Credit: NASA/SDO/AIA\r", "items": [ { "id": 304756, "type": "media", "extra_data": null, "title": null, "caption": null, "instance": { "id": 455500, "url": "https://svs.gsfc.nasa.gov/vis/a010000/a011500/a011522/O_SDO_AIA_171_20140329_17_48.jpg", "filename": "O_SDO_AIA_171_20140329_17_48.jpg", "media_type": "Image", "alt_text": "In these images of the solar corona showing light in the 171 angstrom wavelength, the March 29, 2014, flare can barely be seen. However light in this wavelength does clearly show the beautiful loops of charged particles – tracing out the sun's magnetic field lines — that can clearly be seen rising up on the sun's horizon.Credit: NASA/SDO/AIA\r", "width": 1362, "height": 808, "pixels": 1100496 } }, { "id": 304757, "type": "media", "extra_data": null, "title": null, "caption": null, "instance": { "id": 455499, "url": "https://svs.gsfc.nasa.gov/vis/a010000/a011500/a011522/O_SDO_AIA_171_20140329_17_48_web.jpg", "filename": "O_SDO_AIA_171_20140329_17_48_web.jpg", "media_type": "Image", "alt_text": "In these images of the solar corona showing light in the 171 angstrom wavelength, the March 29, 2014, flare can barely be seen. However light in this wavelength does clearly show the beautiful loops of charged particles – tracing out the sun's magnetic field lines — that can clearly be seen rising up on the sun's horizon.Credit: NASA/SDO/AIA\r", "width": 319, "height": 189, "pixels": 60291 } }, { "id": 304758, "type": "media", "extra_data": null, "title": null, "caption": null, "instance": { "id": 455498, "url": "https://svs.gsfc.nasa.gov/vis/a010000/a011500/a011522/O_SDO_AIA_171_20140329_17_48_web.png", "filename": "O_SDO_AIA_171_20140329_17_48_web.png", "media_type": "Image", "alt_text": "In these images of the solar corona showing light in the 171 angstrom wavelength, the March 29, 2014, flare can barely be seen. However light in this wavelength does clearly show the beautiful loops of charged particles – tracing out the sun's magnetic field lines — that can clearly be seen rising up on the sun's horizon.Credit: NASA/SDO/AIA\r", "width": 320, "height": 189, "pixels": 60480 } }, { "id": 304759, "type": "media", "extra_data": null, "title": null, "caption": null, "instance": { "id": 455497, "url": "https://svs.gsfc.nasa.gov/vis/a010000/a011500/a011522/O_SDO_AIA_171_20140329_17_48_thm.png", "filename": "O_SDO_AIA_171_20140329_17_48_thm.png", "media_type": "Image", "alt_text": "In these images of the solar corona showing light in the 171 angstrom wavelength, the March 29, 2014, flare can barely be seen. However light in this wavelength does clearly show the beautiful loops of charged particles – tracing out the sun's magnetic field lines — that can clearly be seen rising up on the sun's horizon.Credit: NASA/SDO/AIA\r", "width": 80, "height": 40, "pixels": 3200 } } ], "extra_data": {} }, { "id": 344769, "url": "https://svs.gsfc.nasa.gov/11522/#media_group_344769", "widget": "Single image", "title": "", "caption": "", "description": "An image of the sun's surface, or photosphere, at 1:48 p.m. EDT on March 29, 2014, captured by the Helioseismic Magnetic Imager on NASA's Solar Dynamics Observatory.
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Credit: NASA/SDO/HMI\r", "items": [ { "id": 304772, "type": "media", "extra_data": null, "title": null, "caption": null, "instance": { "id": 455516, "url": "https://svs.gsfc.nasa.gov/vis/a010000/a011500/a011522/E_SDO_chromosphere_zoom.jpg", "filename": "E_SDO_chromosphere_zoom.jpg", "media_type": "Image", "alt_text": "A close-up of the sunspot at the root of the March 29, 2014, X-class flare. This image was taken using NASA's Solar Dynamics Observatory – which specializes in capturing images of the entire sun. Zooming in on a spot like this shows some detail but not at extremely high resolution.Credit: NASA/SDO/HMI\r", "width": 766, "height": 766, "pixels": 586756 } }, { "id": 304773, "type": "media", "extra_data": null, "title": null, "caption": null, "instance": { "id": 455515, "url": "https://svs.gsfc.nasa.gov/vis/a010000/a011500/a011522/E_SDO_chromosphere_zoom_web.jpg", "filename": "E_SDO_chromosphere_zoom_web.jpg", "media_type": "Image", "alt_text": "A close-up of the sunspot at the root of the March 29, 2014, X-class flare. This image was taken using NASA's Solar Dynamics Observatory – which specializes in capturing images of the entire sun. Zooming in on a spot like this shows some detail but not at extremely high resolution.Credit: NASA/SDO/HMI\r", "width": 320, "height": 320, "pixels": 102400 } }, { "id": 304774, "type": "media", "extra_data": null, "title": null, "caption": null, "instance": { "id": 455514, "url": "https://svs.gsfc.nasa.gov/vis/a010000/a011500/a011522/E_SDO_chromosphere_zoom_web.png", "filename": "E_SDO_chromosphere_zoom_web.png", "media_type": "Image", "alt_text": "A close-up of the sunspot at the root of the March 29, 2014, X-class flare. This image was taken using NASA's Solar Dynamics Observatory – which specializes in capturing images of the entire sun. Zooming in on a spot like this shows some detail but not at extremely high resolution.Credit: NASA/SDO/HMI\r", "width": 320, "height": 320, "pixels": 102400 } }, { "id": 304775, "type": "media", "extra_data": null, "title": null, "caption": null, "instance": { "id": 455513, "url": "https://svs.gsfc.nasa.gov/vis/a010000/a011500/a011522/E_SDO_chromosphere_zoom_thm.png", "filename": "E_SDO_chromosphere_zoom_thm.png", "media_type": "Image", "alt_text": "A close-up of the sunspot at the root of the March 29, 2014, X-class flare. This image was taken using NASA's Solar Dynamics Observatory – which specializes in capturing images of the entire sun. Zooming in on a spot like this shows some detail but not at extremely high resolution.Credit: NASA/SDO/HMI\r", "width": 80, "height": 40, "pixels": 3200 } } ], "extra_data": {} }, { "id": 344773, "url": "https://svs.gsfc.nasa.gov/11522/#media_group_344773", "widget": "Single image", "title": "", "caption": "", "description": "Like almost all solar observatories, NASA's IRIS can provide images of different layers of the sun's atmosphere, which together create a whole picture of what's happening. This image shows light at a wavelength of 1400 angstrom, which highlights material some 650 miles above the sun's surface. The vertical line in the middle shows the slit for IRIS's spectrograph, which can separate light into its many wavelengths to provide even more information about the temperature and velocity of material during a flare.
Credit: NASA/IRIS/Goddard Space Flight Center\r", "items": [ { "id": 304776, "type": "media", "extra_data": null, "title": null, "caption": null, "instance": { "id": 455520, "url": "https://svs.gsfc.nasa.gov/vis/a010000/a011500/a011522/L_IRIS.png", "filename": "L_IRIS.png", "media_type": "Image", "alt_text": "Like almost all solar observatories, NASA's IRIS can provide images of different layers of the sun's atmosphere, which together create a whole picture of what's happening. This image shows light at a wavelength of 1400 angstrom, which highlights material some 650 miles above the sun's surface. The vertical line in the middle shows the slit for IRIS's spectrograph, which can separate light into its many wavelengths to provide even more information about the temperature and velocity of material during a flare.Credit: NASA/IRIS/Goddard Space Flight Center\r", "width": 806, "height": 854, "pixels": 688324 } }, { "id": 304777, "type": "media", "extra_data": null, "title": null, "caption": null, "instance": { "id": 455519, "url": "https://svs.gsfc.nasa.gov/vis/a010000/a011500/a011522/L_IRIS_web.jpg", "filename": "L_IRIS_web.jpg", "media_type": "Image", "alt_text": "Like almost all solar observatories, NASA's IRIS can provide images of different layers of the sun's atmosphere, which together create a whole picture of what's happening. This image shows light at a wavelength of 1400 angstrom, which highlights material some 650 miles above the sun's surface. The vertical line in the middle shows the slit for IRIS's spectrograph, which can separate light into its many wavelengths to provide even more information about the temperature and velocity of material during a flare.Credit: NASA/IRIS/Goddard Space Flight Center\r", "width": 320, "height": 339, "pixels": 108480 } }, { "id": 304778, "type": "media", "extra_data": null, "title": null, "caption": null, "instance": { "id": 455518, "url": "https://svs.gsfc.nasa.gov/vis/a010000/a011500/a011522/L_IRIS_web.png", "filename": "L_IRIS_web.png", "media_type": "Image", "alt_text": "Like almost all solar observatories, NASA's IRIS can provide images of different layers of the sun's atmosphere, which together create a whole picture of what's happening. This image shows light at a wavelength of 1400 angstrom, which highlights material some 650 miles above the sun's surface. The vertical line in the middle shows the slit for IRIS's spectrograph, which can separate light into its many wavelengths to provide even more information about the temperature and velocity of material during a flare.Credit: NASA/IRIS/Goddard Space Flight Center\r", "width": 320, "height": 339, "pixels": 108480 } }, { "id": 304779, "type": "media", "extra_data": null, "title": null, "caption": null, "instance": { "id": 455517, "url": "https://svs.gsfc.nasa.gov/vis/a010000/a011500/a011522/L_IRIS_thm.png", "filename": "L_IRIS_thm.png", "media_type": "Image", "alt_text": "Like almost all solar observatories, NASA's IRIS can provide images of different layers of the sun's atmosphere, which together create a whole picture of what's happening. This image shows light at a wavelength of 1400 angstrom, which highlights material some 650 miles above the sun's surface. The vertical line in the middle shows the slit for IRIS's spectrograph, which can separate light into its many wavelengths to provide even more information about the temperature and velocity of material during a flare.Credit: NASA/IRIS/Goddard Space Flight Center\r", "width": 80, "height": 40, "pixels": 3200 } } ], "extra_data": {} }, { "id": 344774, "url": "https://svs.gsfc.nasa.gov/11522/#media_group_344774", "widget": "Single image", "title": "", "caption": "", "description": "NASA's Interface Region Imaging Spectrograph, or IRIS, captured this image of the X-class flare. This is the first X-class flare that IRIS has ever observed, as the telescope's pointing must be programmed in at least a day in advance – too far ahead to know exactly where or when a flare might occur. With these observations, IRIS provided the first comprehensive data set of how heat and energy move through the low layers of the sun's atmosphere during an X-class flare.
Credit: NASA/IRIS\r", "items": [ { "id": 304780, "type": "media", "extra_data": null, "title": null, "caption": null, "instance": { "id": 455524, "url": "https://svs.gsfc.nasa.gov/vis/a010000/a011500/a011522/K_IRIS_flare.png", "filename": "K_IRIS_flare.png", "media_type": "Image", "alt_text": "NASA's Interface Region Imaging Spectrograph, or IRIS, captured this image of the X-class flare. This is the first X-class flare that IRIS has ever observed, as the telescope's pointing must be programmed in at least a day in advance – too far ahead to know exactly where or when a flare might occur. With these observations, IRIS provided the first comprehensive data set of how heat and energy move through the low layers of the sun's atmosphere during an X-class flare. Credit: NASA/IRIS\r", "width": 733, "height": 758, "pixels": 555614 } }, { "id": 304781, "type": "media", "extra_data": null, "title": null, "caption": null, "instance": { "id": 455523, "url": "https://svs.gsfc.nasa.gov/vis/a010000/a011500/a011522/K_IRIS_flare_web.jpg", "filename": "K_IRIS_flare_web.jpg", "media_type": "Image", "alt_text": "NASA's Interface Region Imaging Spectrograph, or IRIS, captured this image of the X-class flare. This is the first X-class flare that IRIS has ever observed, as the telescope's pointing must be programmed in at least a day in advance – too far ahead to know exactly where or when a flare might occur. With these observations, IRIS provided the first comprehensive data set of how heat and energy move through the low layers of the sun's atmosphere during an X-class flare. Credit: NASA/IRIS\r", "width": 319, "height": 330, "pixels": 105270 } }, { "id": 304782, "type": "media", "extra_data": null, "title": null, "caption": null, "instance": { "id": 455522, "url": "https://svs.gsfc.nasa.gov/vis/a010000/a011500/a011522/K_IRIS_flare_web.png", "filename": "K_IRIS_flare_web.png", "media_type": "Image", "alt_text": "NASA's Interface Region Imaging Spectrograph, or IRIS, captured this image of the X-class flare. This is the first X-class flare that IRIS has ever observed, as the telescope's pointing must be programmed in at least a day in advance – too far ahead to know exactly where or when a flare might occur. With these observations, IRIS provided the first comprehensive data set of how heat and energy move through the low layers of the sun's atmosphere during an X-class flare. Credit: NASA/IRIS\r", "width": 320, "height": 330, "pixels": 105600 } }, { "id": 304783, "type": "media", "extra_data": null, "title": null, "caption": null, "instance": { "id": 455521, "url": "https://svs.gsfc.nasa.gov/vis/a010000/a011500/a011522/K_IRIS_flare_thm.png", "filename": "K_IRIS_flare_thm.png", "media_type": "Image", "alt_text": "NASA's Interface Region Imaging Spectrograph, or IRIS, captured this image of the X-class flare. This is the first X-class flare that IRIS has ever observed, as the telescope's pointing must be programmed in at least a day in advance – too far ahead to know exactly where or when a flare might occur. With these observations, IRIS provided the first comprehensive data set of how heat and energy move through the low layers of the sun's atmosphere during an X-class flare. Credit: NASA/IRIS\r", "width": 80, "height": 40, "pixels": 3200 } } ], "extra_data": {} }, { "id": 344775, "url": "https://svs.gsfc.nasa.gov/11522/#media_group_344775", "widget": "Single image", "title": "", "caption": "", "description": "This close-up of the sunspot underneath the March 29, 2014, flare shows incredible detail. The image was captured by the G-band camera at Sacramento Peak in New Mexico. This instrument can focus on only a small area at once, but provide very high resolution. Ground-based telescope data can be hindered by Earth's atmosphere, which blocks much of the sun's ultraviolet and X-ray light, and causes twinkling even in the light it does allow through. As it happens, the March 29 flare occurred at a time of day in New Mexico that often results in the best viewing times from the ground.
Credit: Kevin Reardon (National Solar Observatory), Lucia Kleint (BAER Institute)\r", "items": [ { "id": 304784, "type": "media", "extra_data": null, "title": null, "caption": null, "instance": { "id": 455528, "url": "https://svs.gsfc.nasa.gov/vis/a010000/a011500/a011522/F_Sac_Peak_Chromosphere.jpg", "filename": "F_Sac_Peak_Chromosphere.jpg", "media_type": "Image", "alt_text": "This close-up of the sunspot underneath the March 29, 2014, flare shows incredible detail. The image was captured by the G-band camera at Sacramento Peak in New Mexico. This instrument can focus on only a small area at once, but provide very high resolution. Ground-based telescope data can be hindered by Earth's atmosphere, which blocks much of the sun's ultraviolet and X-ray light, and causes twinkling even in the light it does allow through. As it happens, the March 29 flare occurred at a time of day in New Mexico that often results in the best viewing times from the ground.Credit: Kevin Reardon (National Solar Observatory), Lucia Kleint (BAER Institute)\r", "width": 766, "height": 766, "pixels": 586756 } }, { "id": 304785, "type": "media", "extra_data": null, "title": null, "caption": null, "instance": { "id": 455527, "url": "https://svs.gsfc.nasa.gov/vis/a010000/a011500/a011522/F_Sac_Peak_Chromosphere_web.jpg", "filename": "F_Sac_Peak_Chromosphere_web.jpg", "media_type": "Image", "alt_text": "This close-up of the sunspot underneath the March 29, 2014, flare shows incredible detail. The image was captured by the G-band camera at Sacramento Peak in New Mexico. This instrument can focus on only a small area at once, but provide very high resolution. Ground-based telescope data can be hindered by Earth's atmosphere, which blocks much of the sun's ultraviolet and X-ray light, and causes twinkling even in the light it does allow through. As it happens, the March 29 flare occurred at a time of day in New Mexico that often results in the best viewing times from the ground.Credit: Kevin Reardon (National Solar Observatory), Lucia Kleint (BAER Institute)\r", "width": 320, "height": 320, "pixels": 102400 } }, { "id": 304786, "type": "media", "extra_data": null, "title": null, "caption": null, "instance": { "id": 455526, "url": "https://svs.gsfc.nasa.gov/vis/a010000/a011500/a011522/F_Sac_Peak_Chromosphere_web.png", "filename": "F_Sac_Peak_Chromosphere_web.png", "media_type": "Image", "alt_text": "This close-up of the sunspot underneath the March 29, 2014, flare shows incredible detail. The image was captured by the G-band camera at Sacramento Peak in New Mexico. This instrument can focus on only a small area at once, but provide very high resolution. Ground-based telescope data can be hindered by Earth's atmosphere, which blocks much of the sun's ultraviolet and X-ray light, and causes twinkling even in the light it does allow through. As it happens, the March 29 flare occurred at a time of day in New Mexico that often results in the best viewing times from the ground.Credit: Kevin Reardon (National Solar Observatory), Lucia Kleint (BAER Institute)\r", "width": 320, "height": 320, "pixels": 102400 } }, { "id": 304787, "type": "media", "extra_data": null, "title": null, "caption": null, "instance": { "id": 455525, "url": "https://svs.gsfc.nasa.gov/vis/a010000/a011500/a011522/F_Sac_Peak_Chromosphere_thm.png", "filename": "F_Sac_Peak_Chromosphere_thm.png", "media_type": "Image", "alt_text": "This close-up of the sunspot underneath the March 29, 2014, flare shows incredible detail. The image was captured by the G-band camera at Sacramento Peak in New Mexico. This instrument can focus on only a small area at once, but provide very high resolution. Ground-based telescope data can be hindered by Earth's atmosphere, which blocks much of the sun's ultraviolet and X-ray light, and causes twinkling even in the light it does allow through. As it happens, the March 29 flare occurred at a time of day in New Mexico that often results in the best viewing times from the ground.Credit: Kevin Reardon (National Solar Observatory), Lucia Kleint (BAER Institute)\r", "width": 80, "height": 40, "pixels": 3200 } } ], "extra_data": {} }, { "id": 344776, "url": "https://svs.gsfc.nasa.gov/11522/#media_group_344776", "widget": "Single image", "title": "", "caption": "", "description": "An image from the ground-based Interferometric Bidimensional Spectrometer, or IBIS, at the National Solar Observatory's Sacramento Peak is overlaid on an image of the sun's surface. A thin bright line can be seen on the left, which is known as a flare ribbon. This flare ribbon lies right over one of the footpoints of the flare seen in other images, such as those from NASA's RHESSI. The other footpoint isn't visible in this image.
Credit: Alberto Sainz Dalda (Stanford University), Kevin Reardon (NSO)\r", "items": [ { "id": 304788, "type": "media", "extra_data": null, "title": null, "caption": null, "instance": { "id": 455532, "url": "https://svs.gsfc.nasa.gov/vis/a010000/a011500/a011522/H_IBIS_higher.jpg", "filename": "H_IBIS_higher.jpg", "media_type": "Image", "alt_text": "An image from the ground-based Interferometric Bidimensional Spectrometer, or IBIS, at the National Solar Observatory's Sacramento Peak is overlaid on an image of the sun's surface. A thin bright line can be seen on the left, which is known as a flare ribbon. This flare ribbon lies right over one of the footpoints of the flare seen in other images, such as those from NASA's RHESSI. The other footpoint isn't visible in this image.Credit: Alberto Sainz Dalda (Stanford University), Kevin Reardon (NSO)\r", "width": 766, "height": 766, "pixels": 586756 } }, { "id": 304789, "type": "media", "extra_data": null, "title": null, "caption": null, "instance": { "id": 455531, "url": "https://svs.gsfc.nasa.gov/vis/a010000/a011500/a011522/H_IBIS_higher_web.jpg", "filename": "H_IBIS_higher_web.jpg", "media_type": "Image", "alt_text": "An image from the ground-based Interferometric Bidimensional Spectrometer, or IBIS, at the National Solar Observatory's Sacramento Peak is overlaid on an image of the sun's surface. A thin bright line can be seen on the left, which is known as a flare ribbon. This flare ribbon lies right over one of the footpoints of the flare seen in other images, such as those from NASA's RHESSI. The other footpoint isn't visible in this image.Credit: Alberto Sainz Dalda (Stanford University), Kevin Reardon (NSO)\r", "width": 320, "height": 320, "pixels": 102400 } }, { "id": 304790, "type": "media", "extra_data": null, "title": null, "caption": null, "instance": { "id": 455530, "url": "https://svs.gsfc.nasa.gov/vis/a010000/a011500/a011522/H_IBIS_higher_web.png", "filename": "H_IBIS_higher_web.png", "media_type": "Image", "alt_text": "An image from the ground-based Interferometric Bidimensional Spectrometer, or IBIS, at the National Solar Observatory's Sacramento Peak is overlaid on an image of the sun's surface. A thin bright line can be seen on the left, which is known as a flare ribbon. This flare ribbon lies right over one of the footpoints of the flare seen in other images, such as those from NASA's RHESSI. The other footpoint isn't visible in this image.Credit: Alberto Sainz Dalda (Stanford University), Kevin Reardon (NSO)\r", "width": 320, "height": 320, "pixels": 102400 } }, { "id": 304791, "type": "media", "extra_data": null, "title": null, "caption": null, "instance": { "id": 455529, "url": "https://svs.gsfc.nasa.gov/vis/a010000/a011500/a011522/H_IBIS_higher_thm.png", "filename": "H_IBIS_higher_thm.png", "media_type": "Image", "alt_text": "An image from the ground-based Interferometric Bidimensional Spectrometer, or IBIS, at the National Solar Observatory's Sacramento Peak is overlaid on an image of the sun's surface. A thin bright line can be seen on the left, which is known as a flare ribbon. This flare ribbon lies right over one of the footpoints of the flare seen in other images, such as those from NASA's RHESSI. The other footpoint isn't visible in this image.Credit: Alberto Sainz Dalda (Stanford University), Kevin Reardon (NSO)\r", "width": 80, "height": 40, "pixels": 3200 } } ], "extra_data": {} }, { "id": 344777, "url": "https://svs.gsfc.nasa.gov/11522/#media_group_344777", "widget": "Single image", "title": "", "caption": "", "description": "IBIS can focus in on different wavelengths of light, and so reveal different layers at different heights in the sun's lower atmosphere, the chromosphere. This image shows a region slightly higher than the former one.
Credit: Lucia Kleint (BAER Institute), Paul Higgins (Trinity College Dublin, Ireland) \r", "items": [ { "id": 304792, "type": "media", "extra_data": null, "title": null, "caption": null, "instance": { "id": 455536, "url": "https://svs.gsfc.nasa.gov/vis/a010000/a011500/a011522/I_IBIS_highest.jpg", "filename": "I_IBIS_highest.jpg", "media_type": "Image", "alt_text": "IBIS can focus in on different wavelengths of light, and so reveal different layers at different heights in the sun's lower atmosphere, the chromosphere. This image shows a region slightly higher than the former one.Credit: Lucia Kleint (BAER Institute), Paul Higgins (Trinity College Dublin, Ireland) \r", "width": 766, "height": 766, "pixels": 586756 } }, { "id": 304793, "type": "media", "extra_data": null, "title": null, "caption": null, "instance": { "id": 455535, "url": "https://svs.gsfc.nasa.gov/vis/a010000/a011500/a011522/I_IBIS_highest_web.jpg", "filename": "I_IBIS_highest_web.jpg", "media_type": "Image", "alt_text": "IBIS can focus in on different wavelengths of light, and so reveal different layers at different heights in the sun's lower atmosphere, the chromosphere. This image shows a region slightly higher than the former one.Credit: Lucia Kleint (BAER Institute), Paul Higgins (Trinity College Dublin, Ireland) \r", "width": 320, "height": 320, "pixels": 102400 } }, { "id": 304794, "type": "media", "extra_data": null, "title": null, "caption": null, "instance": { "id": 455534, "url": "https://svs.gsfc.nasa.gov/vis/a010000/a011500/a011522/I_IBIS_highest_web.png", "filename": "I_IBIS_highest_web.png", "media_type": "Image", "alt_text": "IBIS can focus in on different wavelengths of light, and so reveal different layers at different heights in the sun's lower atmosphere, the chromosphere. This image shows a region slightly higher than the former one.Credit: Lucia Kleint (BAER Institute), Paul Higgins (Trinity College Dublin, Ireland) \r", "width": 320, "height": 320, "pixels": 102400 } }, { "id": 304795, "type": "media", "extra_data": null, "title": null, "caption": null, "instance": { "id": 455533, "url": "https://svs.gsfc.nasa.gov/vis/a010000/a011500/a011522/I_IBIS_highest_thm.png", "filename": "I_IBIS_highest_thm.png", "media_type": "Image", "alt_text": "IBIS can focus in on different wavelengths of light, and so reveal different layers at different heights in the sun's lower atmosphere, the chromosphere. This image shows a region slightly higher than the former one.Credit: Lucia Kleint (BAER Institute), Paul Higgins (Trinity College Dublin, Ireland) \r", "width": 80, "height": 40, "pixels": 3200 } } ], "extra_data": {} }, { "id": 344778, "url": "https://svs.gsfc.nasa.gov/11522/#media_group_344778", "widget": "Single image", "title": "", "caption": "", "description": "Each of these images from the Japan Aerospace Exploration Agency's and NASA's Hinode shows a progressively higher layer of the sun's atmosphere. The upper left corner shows material in a low part of the atmosphere, called the chromosphere – and the images progress ever upward through the heart of the flare up to over 3,000 miles above the surface in the image on the lower right. Each image shows a narrow swatch of the flare, which together can be combined to create a 3-dimensional picture. The images were captured by the EUV Imaging Spectrometer instrument on Hinode.
Credit: JAXA/NASA/Hinode/EIS\r", "items": [ { "id": 304796, "type": "media", "extra_data": null, "title": null, "caption": null, "instance": { "id": 455539, "url": "https://svs.gsfc.nasa.gov/vis/a010000/a011500/a011522/J_Hinode_EIS_series.jpeg", "filename": "J_Hinode_EIS_series.jpeg", "media_type": "Image", "alt_text": "Each of these images from the Japan Aerospace Exploration Agency's and NASA's Hinode shows a progressively higher layer of the sun's atmosphere. The upper left corner shows material in a low part of the atmosphere, called the chromosphere – and the images progress ever upward through the heart of the flare up to over 3,000 miles above the surface in the image on the lower right. Each image shows a narrow swatch of the flare, which together can be combined to create a 3-dimensional picture. The images were captured by the EUV Imaging Spectrometer instrument on Hinode.Credit: JAXA/NASA/Hinode/EIS\r", "width": 2000, "height": 811, "pixels": 1622000 } }, { "id": 304799, "type": "media", "extra_data": null, "title": null, "caption": null, "instance": { "id": 455540, "url": "https://svs.gsfc.nasa.gov/vis/a010000/a011500/a011522/J_Hinode_EIS_series_print.jpg", "filename": "J_Hinode_EIS_series_print.jpg", "media_type": "Image", "alt_text": "Each of these images from the Japan Aerospace Exploration Agency's and NASA's Hinode shows a progressively higher layer of the sun's atmosphere. The upper left corner shows material in a low part of the atmosphere, called the chromosphere – and the images progress ever upward through the heart of the flare up to over 3,000 miles above the surface in the image on the lower right. Each image shows a narrow swatch of the flare, which together can be combined to create a 3-dimensional picture. The images were captured by the EUV Imaging Spectrometer instrument on Hinode.Credit: JAXA/NASA/Hinode/EIS\r", "width": 1024, "height": 415, "pixels": 424960 } }, { "id": 304797, "type": "media", "extra_data": null, "title": null, "caption": null, "instance": { "id": 455538, "url": "https://svs.gsfc.nasa.gov/vis/a010000/a011500/a011522/J_Hinode_EIS_series_web.png", "filename": "J_Hinode_EIS_series_web.png", "media_type": "Image", "alt_text": "Each of these images from the Japan Aerospace Exploration Agency's and NASA's Hinode shows a progressively higher layer of the sun's atmosphere. The upper left corner shows material in a low part of the atmosphere, called the chromosphere – and the images progress ever upward through the heart of the flare up to over 3,000 miles above the surface in the image on the lower right. Each image shows a narrow swatch of the flare, which together can be combined to create a 3-dimensional picture. The images were captured by the EUV Imaging Spectrometer instrument on Hinode.Credit: JAXA/NASA/Hinode/EIS\r", "width": 320, "height": 129, "pixels": 41280 } }, { "id": 304798, "type": "media", "extra_data": null, "title": null, "caption": null, "instance": { "id": 455537, "url": "https://svs.gsfc.nasa.gov/vis/a010000/a011500/a011522/J_Hinode_EIS_series_thm.png", "filename": "J_Hinode_EIS_series_thm.png", "media_type": "Image", "alt_text": "Each of these images from the Japan Aerospace Exploration Agency's and NASA's Hinode shows a progressively higher layer of the sun's atmosphere. The upper left corner shows material in a low part of the atmosphere, called the chromosphere – and the images progress ever upward through the heart of the flare up to over 3,000 miles above the surface in the image on the lower right. Each image shows a narrow swatch of the flare, which together can be combined to create a 3-dimensional picture. The images were captured by the EUV Imaging Spectrometer instrument on Hinode.Credit: JAXA/NASA/Hinode/EIS\r", "width": 80, "height": 40, "pixels": 3200 } } ], "extra_data": {} }, { "id": 344779, "url": "https://svs.gsfc.nasa.gov/11522/#media_group_344779", "widget": "Single image", "title": "", "caption": "", "description": "This image of the solar surface — captured just as the flare peaked at 1:48 p.m. EDT, by the Solar Optical Telescope on the Japan Aerospace and Exploration Agency's and NASA's Hinode spacecraft – is what's called a magnetogram. The dark spots show where magnetic field lines travel in to the sun and the light regions show where they travel out. The intense white line on the left and the lower dark U-shape on the right, represent the footprints of the flare. Using these magnetograms, researchers were able to map the magnetic field's strength and direction change just before a flare in one of the highest resolution and best data sets ever gathered.
Credit: JAXA/NASA/Hinode\r\r", "items": [ { "id": 304800, "type": "media", "extra_data": null, "title": null, "caption": null, "instance": { "id": 455544, "url": "https://svs.gsfc.nasa.gov/vis/a010000/a011500/a011522/D_Hinode_SOT.jpg", "filename": "D_Hinode_SOT.jpg", "media_type": "Image", "alt_text": "This image of the solar surface — captured just as the flare peaked at 1:48 p.m. EDT, by the Solar Optical Telescope on the Japan Aerospace and Exploration Agency's and NASA's Hinode spacecraft – is what's called a magnetogram. The dark spots show where magnetic field lines travel in to the sun and the light regions show where they travel out. The intense white line on the left and the lower dark U-shape on the right, represent the footprints of the flare. Using these magnetograms, researchers were able to map the magnetic field's strength and direction change just before a flare in one of the highest resolution and best data sets ever gathered.Credit: JAXA/NASA/Hinode\r\r", "width": 1248, "height": 702, "pixels": 876096 } }, { "id": 304801, "type": "media", "extra_data": null, "title": null, "caption": null, "instance": { "id": 455543, "url": "https://svs.gsfc.nasa.gov/vis/a010000/a011500/a011522/D_Hinode_SOT_web.jpg", "filename": "D_Hinode_SOT_web.jpg", "media_type": "Image", "alt_text": "This image of the solar surface — captured just as the flare peaked at 1:48 p.m. EDT, by the Solar Optical Telescope on the Japan Aerospace and Exploration Agency's and NASA's Hinode spacecraft – is what's called a magnetogram. The dark spots show where magnetic field lines travel in to the sun and the light regions show where they travel out. The intense white line on the left and the lower dark U-shape on the right, represent the footprints of the flare. Using these magnetograms, researchers were able to map the magnetic field's strength and direction change just before a flare in one of the highest resolution and best data sets ever gathered.Credit: JAXA/NASA/Hinode\r\r", "width": 320, "height": 180, "pixels": 57600 } }, { "id": 304802, "type": "media", "extra_data": null, "title": null, "caption": null, "instance": { "id": 455542, "url": "https://svs.gsfc.nasa.gov/vis/a010000/a011500/a011522/D_Hinode_SOT_web.png", "filename": "D_Hinode_SOT_web.png", "media_type": "Image", "alt_text": "This image of the solar surface — captured just as the flare peaked at 1:48 p.m. EDT, by the Solar Optical Telescope on the Japan Aerospace and Exploration Agency's and NASA's Hinode spacecraft – is what's called a magnetogram. The dark spots show where magnetic field lines travel in to the sun and the light regions show where they travel out. The intense white line on the left and the lower dark U-shape on the right, represent the footprints of the flare. Using these magnetograms, researchers were able to map the magnetic field's strength and direction change just before a flare in one of the highest resolution and best data sets ever gathered.Credit: JAXA/NASA/Hinode\r\r", "width": 320, "height": 180, "pixels": 57600 } }, { "id": 304803, "type": "media", "extra_data": null, "title": null, "caption": null, "instance": { "id": 455541, "url": "https://svs.gsfc.nasa.gov/vis/a010000/a011500/a011522/D_Hinode_SOT_thm.png", "filename": "D_Hinode_SOT_thm.png", "media_type": "Image", "alt_text": "This image of the solar surface — captured just as the flare peaked at 1:48 p.m. EDT, by the Solar Optical Telescope on the Japan Aerospace and Exploration Agency's and NASA's Hinode spacecraft – is what's called a magnetogram. The dark spots show where magnetic field lines travel in to the sun and the light regions show where they travel out. The intense white line on the left and the lower dark U-shape on the right, represent the footprints of the flare. Using these magnetograms, researchers were able to map the magnetic field's strength and direction change just before a flare in one of the highest resolution and best data sets ever gathered.Credit: JAXA/NASA/Hinode\r\r", "width": 80, "height": 40, "pixels": 3200 } } ], "extra_data": {} }, { "id": 344780, "url": "https://svs.gsfc.nasa.gov/11522/#media_group_344780", "widget": "Single image", "title": "", "caption": "", "description": "NASA's Reuven Ramaty High Energy Solar Spectroscopic Imager, or RHESSI, observes both the intense particle acceleration caused by the flare and the hottest temperature material. The image on the left shows where flare-accelerated electrons interact with the chromosphere at the footpoints of the flare, which are situated above the sunspots seen on the surface of the sun in other images. The image on the right shows the 25 million Kelvin material higher in the flare loop in the corona.
Credit: NASA/RHESSI\r", "items": [ { "id": 304804, "type": "media", "extra_data": null, "title": null, "caption": null, "instance": { "id": 455547, "url": "https://svs.gsfc.nasa.gov/vis/a010000/a011500/a011522/M_RHESSI.jpg", "filename": "M_RHESSI.jpg", "media_type": "Image", "alt_text": "NASA's Reuven Ramaty High Energy Solar Spectroscopic Imager, or RHESSI, observes both the intense particle acceleration caused by the flare and the hottest temperature material. The image on the left shows where flare-accelerated electrons interact with the chromosphere at the footpoints of the flare, which are situated above the sunspots seen on the surface of the sun in other images. The image on the right shows the 25 million Kelvin material higher in the flare loop in the corona.Credit: NASA/RHESSI\r", "width": 1280, "height": 720, "pixels": 921600 } }, { "id": 304805, "type": "media", "extra_data": null, "title": null, "caption": null, "instance": { "id": 455548, "url": "https://svs.gsfc.nasa.gov/vis/a010000/a011500/a011522/M_RHESSI_web.jpg", "filename": "M_RHESSI_web.jpg", "media_type": "Image", "alt_text": "NASA's Reuven Ramaty High Energy Solar Spectroscopic Imager, or RHESSI, observes both the intense particle acceleration caused by the flare and the hottest temperature material. The image on the left shows where flare-accelerated electrons interact with the chromosphere at the footpoints of the flare, which are situated above the sunspots seen on the surface of the sun in other images. The image on the right shows the 25 million Kelvin material higher in the flare loop in the corona.Credit: NASA/RHESSI\r", "width": 320, "height": 180, "pixels": 57600 } }, { "id": 304806, "type": "media", "extra_data": null, "title": null, "caption": null, "instance": { "id": 455546, "url": "https://svs.gsfc.nasa.gov/vis/a010000/a011500/a011522/M_RHESSI_web.png", "filename": "M_RHESSI_web.png", "media_type": "Image", "alt_text": "NASA's Reuven Ramaty High Energy Solar Spectroscopic Imager, or RHESSI, observes both the intense particle acceleration caused by the flare and the hottest temperature material. The image on the left shows where flare-accelerated electrons interact with the chromosphere at the footpoints of the flare, which are situated above the sunspots seen on the surface of the sun in other images. The image on the right shows the 25 million Kelvin material higher in the flare loop in the corona.Credit: NASA/RHESSI\r", "width": 320, "height": 180, "pixels": 57600 } }, { "id": 304807, "type": "media", "extra_data": null, "title": null, "caption": null, "instance": { "id": 455545, "url": "https://svs.gsfc.nasa.gov/vis/a010000/a011500/a011522/M_RHESSI_thm.png", "filename": "M_RHESSI_thm.png", "media_type": "Image", "alt_text": "NASA's Reuven Ramaty High Energy Solar Spectroscopic Imager, or RHESSI, observes both the intense particle acceleration caused by the flare and the hottest temperature material. The image on the left shows where flare-accelerated electrons interact with the chromosphere at the footpoints of the flare, which are situated above the sunspots seen on the surface of the sun in other images. The image on the right shows the 25 million Kelvin material higher in the flare loop in the corona.Credit: NASA/RHESSI\r", "width": 80, "height": 40, "pixels": 3200 } } ], "extra_data": {} }, { "id": 344781, "url": "https://svs.gsfc.nasa.gov/11522/#media_group_344781", "widget": "Single image", "title": "", "caption": "", "description": "Not all solar observations come looking like pretty pictures. This data shoes how the National Oceanic and Atmospheric Administration's Geostationary Operational Environmental Satellite, or GOES, recorded the X-class flare. Note the high spike just before 18:00 – the Universal Time equivalent of 2:00 p.m. EDT — on March 29. That spike shows how GOES detected a surge in X-rays from the sun, the signature of a solar flare.", "items": [ { "id": 304808, "type": "media", "extra_data": null, "title": null, "caption": null, "instance": { "id": 455552, "url": "https://svs.gsfc.nasa.gov/vis/a010000/a011500/a011522/Q_GOES_primary_X-ray_flux.png", "filename": "Q_GOES_primary_X-ray_flux.png", "media_type": "Image", "alt_text": "Not all solar observations come looking like pretty pictures. This data shoes how the National Oceanic and Atmospheric Administration's Geostationary Operational Environmental Satellite, or GOES, recorded the X-class flare. Note the high spike just before 18:00 – the Universal Time equivalent of 2:00 p.m. EDT — on March 29. That spike shows how GOES detected a surge in X-rays from the sun, the signature of a solar flare.", "width": 787, "height": 330, "pixels": 259710 } }, { "id": 304809, "type": "media", "extra_data": null, "title": null, "caption": null, "instance": { "id": 455551, "url": "https://svs.gsfc.nasa.gov/vis/a010000/a011500/a011522/Q_GOES_primary_X-ray_flux_web.jpg", "filename": "Q_GOES_primary_X-ray_flux_web.jpg", "media_type": "Image", "alt_text": "Not all solar observations come looking like pretty pictures. This data shoes how the National Oceanic and Atmospheric Administration's Geostationary Operational Environmental Satellite, or GOES, recorded the X-class flare. Note the high spike just before 18:00 – the Universal Time equivalent of 2:00 p.m. EDT — on March 29. That spike shows how GOES detected a surge in X-rays from the sun, the signature of a solar flare.", "width": 320, "height": 134, "pixels": 42880 } }, { "id": 304810, "type": "media", "extra_data": null, "title": null, "caption": null, "instance": { "id": 455550, "url": "https://svs.gsfc.nasa.gov/vis/a010000/a011500/a011522/Q_GOES_primary_X-ray_flux_web.png", "filename": "Q_GOES_primary_X-ray_flux_web.png", "media_type": "Image", "alt_text": "Not all solar observations come looking like pretty pictures. This data shoes how the National Oceanic and Atmospheric Administration's Geostationary Operational Environmental Satellite, or GOES, recorded the X-class flare. Note the high spike just before 18:00 – the Universal Time equivalent of 2:00 p.m. EDT — on March 29. That spike shows how GOES detected a surge in X-rays from the sun, the signature of a solar flare.", "width": 320, "height": 134, "pixels": 42880 } }, { "id": 304811, "type": "media", "extra_data": null, "title": null, "caption": null, "instance": { "id": 455549, "url": "https://svs.gsfc.nasa.gov/vis/a010000/a011500/a011522/Q_GOES_primary_X-ray_flux_thm.png", "filename": "Q_GOES_primary_X-ray_flux_thm.png", "media_type": "Image", "alt_text": "Not all solar observations come looking like pretty pictures. This data shoes how the National Oceanic and Atmospheric Administration's Geostationary Operational Environmental Satellite, or GOES, recorded the X-class flare. Note the high spike just before 18:00 – the Universal Time equivalent of 2:00 p.m. EDT — on March 29. That spike shows how GOES detected a surge in X-rays from the sun, the signature of a solar flare.", "width": 80, "height": 40, "pixels": 3200 } } ], "extra_data": {} } ], "studio": "gms", "funding_sources": [ "PAO" ], "credits": [ { "role": "Animator", "people": [ { "name": "Tom Bridgman", "employer": "Global Science and Technology, Inc." }, { "name": "Walt Feimer", "employer": "HTSI" }, { "name": "Chris Meaney", "employer": "HTSI" } ] }, { "role": "Video editor", "people": [ { "name": "Genna Duberstein", "employer": "USRA" } ] }, { "role": "Narrator", "people": [ { "name": "Karen Fox", "employer": "ADNET Systems, Inc." } ] }, { "role": "Producer", "people": [ { "name": "Genna Duberstein", "employer": "USRA" } ] }, { "role": "Scientist", "people": [ { "name": "Adrian Daw", "employer": "NASA/GSFC" }, { "name": "William D. Pesnell", "employer": "NASA/GSFC" }, { "name": "Lucia Kleint", "employer": "BAER Institute" }, { "name": "Albert Shih", "employer": "NASA/GSFC" } ] }, { "role": "Project support", "people": [ { "name": "Aaron E. Lepsch", "employer": "ADNET Systems, Inc." } ] }, { "role": "Writer", "people": [ { "name": "Karen Fox", "employer": "ADNET Systems, Inc." } ] } ], "missions": [], "series": [ "Narrated Movies" ], "tapes": [ "One X-class Flare, Observed Four Ways (Produced by: Will Duquette)" ], "papers": [], "datasets": [], "nasa_science_categories": [ "Sun" ], "keywords": [ "HDTV", "Narrated" ], "recommended_pages": [], "related": [ { "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 } } ], "sources": [], "products": [], "newer_versions": [], "older_versions": [], "alternate_versions": [] }