{ "count": 90, "next": null, "previous": null, "results": [ { "id": 4911, "url": "https://svs.gsfc.nasa.gov/4911/", "result_type": "Visualization", "release_date": "2021-07-23T10:00:00-04:00", "title": "Aging (Instruments) in Space", "description": "The space environment is harsh not only on humans and other living organisms, but instruments also.Damage from solar energetic particles and cosmic rays can slowly degrade performance of an instrument. Fortunately there are ways to characterize and correct for this degradation. The graphics on this page are based on the tutorial AIApy: Modeling Channel Degradation over Time. || ", "hits": 26 }, { "id": 13859, "url": "https://svs.gsfc.nasa.gov/13859/", "result_type": "Produced Video", "release_date": "2021-06-18T12:00:00-04:00", "title": "Why Does NASA Observe The Sun in Different Colors?", "description": "The Solar Dynamics Observatory, or SDO, was launched on Feb. 11, 2010, and began collecting science data a few months later. With two imaging instruments – the Atmospheric Imaging Assembly and the Helioseismic and Magnetic Imager, which were designed in concert to provide complementary views of the Sun – SDO sees the Sun in more than 10 distinct wavelengths of light, showing solar material at different temperatures. SDO also measures the Sun’s magnetic field and the motion of solar material at its surface, and, using a technique called helioseismology, allows scientists to probe deep into the Sun's interior, where the Sun’s complex magnetic fields sprout from. And with more than a decade of observation under its belt, SDO has provided scientists with hundreds of millions of images of our star. || ", "hits": 202 }, { "id": 13776, "url": "https://svs.gsfc.nasa.gov/13776/", "result_type": "Produced Video", "release_date": "2020-12-15T21:00:00-05:00", "title": "2020 AGU Roundtable: What will we learn from Solar Cycle 25?", "description": "Solar Cycle 25 is here, ushering in the next season of space weather from the Sun. As our star’s activity ramps up—a natural part of its roughly 11-year cycle—scientists are eager to test their predictions. In this AGU 2020 media roundtable, scientists will discuss outstanding questions in solar cycle science, what opportunities this new cycle provides researchers, and how we track progress in predictions. || ", "hits": 258 }, { "id": 4776, "url": "https://svs.gsfc.nasa.gov/4776/", "result_type": "Visualization", "release_date": "2020-06-24T10:00:00-04:00", "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] || ", "hits": 67 }, { "id": 4788, "url": "https://svs.gsfc.nasa.gov/4788/", "result_type": "Visualization", "release_date": "2020-02-04T12:00:00-05:00", "title": "The Solar Polar Magnetic Field", "description": "From our single vantage point of Earth, our view of the Sun is never complete. While the far-side of the Sun eventually rotates into view, coverage of the Sun's polar regions is never satisfactory as perspective effects either completely block our view or create a distorted view. We must often resort to computer modeling of these solar polar regions.This visualization presents the Potential Field Source Surface (PFSS) magnetic field model based on solar observations covering the years 2017-2019. One version also presents the 'hole' in our measurements of the solar polar region. The region oscillates in size over the course of the year due to the changing perspective created by the tilt of Earth's orbital plane with the solar equator. In this region, researchers must resort to approximations to build a more complete view of the solar magnetic field.Why is the solar magnetic field in this region important? Because the combined with the outgoing flow of the solar wind, the magnetic field lines from the polar regions curve up, and then back down to near the Sun's equatorial plane, which is still fairly close to the orbital plane of Earth and other planets in our solar system. This gives the Sun's polar magnetic field a significant influence on the space weather impacting Earth and crewed and uncrewed assets around the solar system. || ", "hits": 73 }, { "id": 4763, "url": "https://svs.gsfc.nasa.gov/4763/", "result_type": "Visualization", "release_date": "2019-11-11T16:30:00-05:00", "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] || ", "hits": 58 }, { "id": 4352, "url": "https://svs.gsfc.nasa.gov/4352/", "result_type": "Visualization", "release_date": "2017-08-20T10:00:00-04:00", "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] || ", "hits": 67 }, { "id": 4461, "url": "https://svs.gsfc.nasa.gov/4461/", "result_type": "Visualization", "release_date": "2016-06-01T10:00:00-04:00", "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)] || ", "hits": 28 }, { "id": 4462, "url": "https://svs.gsfc.nasa.gov/4462/", "result_type": "Visualization", "release_date": "2016-06-01T10:00:00-04:00", "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)] || ", "hits": 37 }, { "id": 4463, "url": "https://svs.gsfc.nasa.gov/4463/", "result_type": "Visualization", "release_date": "2016-06-01T10:00:00-04:00", "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)] || ", "hits": 36 }, { "id": 4319, "url": "https://svs.gsfc.nasa.gov/4319/", "result_type": "Visualization", "release_date": "2016-02-11T00:00:00-05:00", "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] || ", "hits": 50 }, { "id": 4380, "url": "https://svs.gsfc.nasa.gov/4380/", "result_type": "Visualization", "release_date": "2015-10-14T00:00:00-04:00", "title": "The Sun from SDO: The See-Saw Filament", "description": "1080HD movie of the Sun in AIA 304 angstrom filter. || May2015SeeSawFilament_304A_stand.HD1080i.00300_print.jpg (1024x576) [65.5 KB] || May2015SeeSawFilament_304A_stand.HD1080i.00300_searchweb.png (320x180) [37.8 KB] || May2015SeeSawFilament_304A_stand.HD1080i.00300_thm.png (80x40) [3.1 KB] || 1920x1080_16x9_30p (1920x1080) [0 Item(s)] || May2015SeeSawFilament_304A_stand_1080p.webm (1920x1080) [3.0 MB] || May2015SeeSawFilament_304A_stand_1080p.mp4 (1920x1080) [28.7 MB] || May2015SeeSawFilament_304A_stand_1080p.mp4.hwshow [204 bytes] || ", "hits": 28 }, { "id": 11993, "url": "https://svs.gsfc.nasa.gov/11993/", "result_type": "Produced Video", "release_date": "2015-09-14T00:00:00-04:00", "title": "SDO Transit - September 2015", "description": "The Earth and moon photobomb SDO.Watch this video on the NASAexplorer YouTube channel. || sdophotobombthumb.jpg (1280x720) [78.0 KB] || G2015-072_SDOtransit9.13.15.mov (1920x1080) [1.3 GB] || G2015-072_SDOtransit9.13.15.webm (1920x1080) [5.7 MB] || G2015-072_SDOtransit9.13.15-H264_Best_1920x1080_59.94.mov (1920x1080) [253.2 MB] || G2015-072_SDOtransit9.13.15-H264_Good_1080_29.97.mov (1920x1080) [48.7 MB] || G2015-072_SDOtransit9.13.15_youtube_hq.mov (1920x1080) [131.1 MB] || G2015-072_SDOtransit9.13.15_appletv.m4v (1280x720) [30.9 MB] || G2015-072_SDOtransit9.13.15_appletv_subtitles.m4v (1280x720) [30.9 MB] || G2015-072_SDOtransit9.en_US.srt [514 bytes] || G2015-072_SDOtransit9.en_US.vtt [527 bytes] || G2015-072_SDOtransit9.13.15_ipod_sm.mp4 (320x240) [12.1 MB] || ", "hits": 19 }, { "id": 11840, "url": "https://svs.gsfc.nasa.gov/11840/", "result_type": "Produced Video", "release_date": "2015-05-05T11:00:00-04:00", "title": "Solar Vibrations", "description": "Images from space reveal the chaotic motions on the surface of the sun. || c-1280.jpg (1280x720) [204.6 KB] || c-1024.jpg (1024x576) [136.5 KB] || c-1024_print.jpg (1024x576) [123.1 KB] || c-1024_searchweb.png (320x180) [50.0 KB] || ", "hits": 88 }, { "id": 11755, "url": "https://svs.gsfc.nasa.gov/11755/", "result_type": "Produced Video", "release_date": "2015-03-10T11:00:00-04:00", "title": "Solar Exposures", "description": "See a five-year time-lapse of the sun. || c_1024.jpg (1024x576) [180.4 KB] || c_1280.jpg (1280x720) [254.4 KB] || c_1920.jpg (1920x1080) [1.3 MB] || c_1024_print.jpg (1024x576) [181.8 KB] || c_1024_searchweb.png (320x180) [70.7 KB] || c_1024_print_thm.png (80x40) [14.9 KB] || ", "hits": 59 }, { "id": 4277, "url": "https://svs.gsfc.nasa.gov/4277/", "result_type": "Visualization", "release_date": "2015-03-03T00:00:00-05:00", "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] || ", "hits": 29 }, { "id": 4125, "url": "https://svs.gsfc.nasa.gov/4125/", "result_type": "Visualization", "release_date": "2015-02-11T00:00:00-05:00", "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. || ", "hits": 20 }, { "id": 4166, "url": "https://svs.gsfc.nasa.gov/4166/", "result_type": "Visualization", "release_date": "2015-02-11T00:00:00-05:00", "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. || ", "hits": 40 }, { "id": 4182, "url": "https://svs.gsfc.nasa.gov/4182/", "result_type": "Visualization", "release_date": "2015-02-11T00:00:00-05:00", "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. || ", "hits": 28 }, { "id": 4202, "url": "https://svs.gsfc.nasa.gov/4202/", "result_type": "Visualization", "release_date": "2015-02-11T00:00:00-05:00", "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. || ", "hits": 20 }, { "id": 4216, "url": "https://svs.gsfc.nasa.gov/4216/", "result_type": "Visualization", "release_date": "2015-02-11T00:00:00-05:00", "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. || ", "hits": 31 }, { "id": 4225, "url": "https://svs.gsfc.nasa.gov/4225/", "result_type": "Visualization", "release_date": "2015-02-11T00:00:00-05:00", "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] || ", "hits": 19 }, { "id": 4232, "url": "https://svs.gsfc.nasa.gov/4232/", "result_type": "Visualization", "release_date": "2015-02-11T00:00:00-05:00", "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] || ", "hits": 33 }, { "id": 4235, "url": "https://svs.gsfc.nasa.gov/4235/", "result_type": "Visualization", "release_date": "2015-02-11T00:00:00-05:00", "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] || ", "hits": 24 }, { "id": 4244, "url": "https://svs.gsfc.nasa.gov/4244/", "result_type": "Visualization", "release_date": "2015-02-11T00:00:00-05:00", "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] || ", "hits": 38 }, { "id": 4246, "url": "https://svs.gsfc.nasa.gov/4246/", "result_type": "Visualization", "release_date": "2015-02-11T00:00:00-05:00", "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] || ", "hits": 58 }, { "id": 4250, "url": "https://svs.gsfc.nasa.gov/4250/", "result_type": "Visualization", "release_date": "2015-02-11T00:00:00-05:00", "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] || ", "hits": 61 }, { "id": 4259, "url": "https://svs.gsfc.nasa.gov/4259/", "result_type": "Visualization", "release_date": "2015-02-11T00:00:00-05:00", "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] || ", "hits": 28 }, { "id": 4267, "url": "https://svs.gsfc.nasa.gov/4267/", "result_type": "Visualization", "release_date": "2015-02-11T00:00:00-05:00", "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] || ", "hits": 32 }, { "id": 4151, "url": "https://svs.gsfc.nasa.gov/4151/", "result_type": "Visualization", "release_date": "2014-05-16T00:00:00-04:00", "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 || ", "hits": 59 }, { "id": 11522, "url": "https://svs.gsfc.nasa.gov/11522/", "result_type": "Produced Video", "release_date": "2014-05-07T12:00:00-04:00", "title": "The Best Observed X-class Flare", "description": "On March 29, 2014 the sun released an X-class flare. It was observed by NASA's Interface Region Imaging Spectrograph, or IRIS; NASA's Solar Dynamics Observatory, or SDO; NASA's Reuven Ramaty High Energy Solar Spectroscopic Imager, or RHESSI; the Japanese Aerospace Exploration Agency's Hinode; and the National Solar Observatory's Dunn Solar Telescope located at Sacramento Peak in New Mexico. 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. || ", "hits": 82 }, { "id": 4164, "url": "https://svs.gsfc.nasa.gov/4164/", "result_type": "Visualization", "release_date": "2014-05-07T10:00:00-04:00", "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. || ", "hits": 55 }, { "id": 4150, "url": "https://svs.gsfc.nasa.gov/4150/", "result_type": "Visualization", "release_date": "2014-03-14T00:00:00-04:00", "title": "January 2012 - Arcade of Coronal Loops from SDO", "description": "An arcade of coronal loops forms and erupts - upper right quadrant of disk. || ", "hits": 13 }, { "id": 4132, "url": "https://svs.gsfc.nasa.gov/4132/", "result_type": "Visualization", "release_date": "2014-02-11T10:00:00-05:00", "title": "May 2013: 'Light bulb'-shaped prominence", "description": "The active region on the solar limb (left side) generates a large bulb-shaped prominence before demonstrating more energetic activity. See SDO View of a May 2013 Solar Flare. || ", "hits": 23 }, { "id": 4133, "url": "https://svs.gsfc.nasa.gov/4133/", "result_type": "Visualization", "release_date": "2014-02-11T10:00:00-05:00", "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. || ", "hits": 54 }, { "id": 4136, "url": "https://svs.gsfc.nasa.gov/4136/", "result_type": "Visualization", "release_date": "2014-02-11T10:00:00-05:00", "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. || ", "hits": 42 }, { "id": 11418, "url": "https://svs.gsfc.nasa.gov/11418/", "result_type": "Produced Video", "release_date": "2014-01-02T00:00:00-05:00", "title": "Solar Continuum", "description": "Many of the sun's features are invisible to the naked eye. To paint a full picture of our constantly changing star, scientists use telescopes launched into space. Each telescope is outfitted with special filters that can see the sun in different wavelengths of light. To track how material and heat of different temperature moves through the sun's atmosphere, scientists only need to select the specific wavelength with which a feature can best be seen. Watch the video for a tour of the wide range of wavelengths that NASA's Solar Dynamics Observatory spacecraft uses to observe the sun. || ", "hits": 93 }, { "id": 4128, "url": "https://svs.gsfc.nasa.gov/4128/", "result_type": "Visualization", "release_date": "2013-12-24T00:00:00-05:00", "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. || ", "hits": 70 }, { "id": 4117, "url": "https://svs.gsfc.nasa.gov/4117/", "result_type": "Visualization", "release_date": "2013-12-17T10:00:00-05:00", "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. || ", "hits": 78 }, { "id": 11385, "url": "https://svs.gsfc.nasa.gov/11385/", "result_type": "Produced Video", "release_date": "2013-12-17T10:00:00-05:00", "title": "Jewel Box Sun", "description": "Telescopes help distant objects appear bigger, but this is only one of their advantages. Telescopes can also collect light in ranges that our eyes alone cannot see, providing scientists ways of observing a whole host of material and processes that would otherwise be inaccessible. A new NASA movie of the sun based on data from NASA's Solar Dynamics Observatory, or SDO, shows the wide range of wavelengths – invisible to the naked eye – that the telescope can view. SDO converts the wavelengths into an image humans can see, and the light is colorized into a rainbow of colors. As the colors sweep around the sun in the movie, viewers should note how different the same area of the sun appears. This happens because each wavelength of light represents solar material at specific temperatures. Different wavelengths convey information about different components of the sun's surface and atmosphere, so scientists use them to paint a full picture of our constantly changing and varying star.Yellow light of 5800 angstroms, for example, generally emanates from material of about 10,000 degrees F (5700 degrees C), which represents the surface of the sun. Extreme ultraviolet light of 94 angstroms, which is typically colorized in green in SDO images, comes from atoms that are about 11 million degrees F (6,300,000 degrees C) and is a good wavelength for looking at solar flares, which can reach such high temperatures. By examining pictures of the sun in a variety of wavelengths – as is done not only by SDO, but also by NASA's Interface Region Imaging Spectrograph, NASA's Solar Terrestrial Relations Observatory and the European Space Agency/NASA Solar and Heliospheric Observatory — scientists can track how particles and heat move through the sun's atmosphere. || ", "hits": 51 }, { "id": 4017, "url": "https://svs.gsfc.nasa.gov/4017/", "result_type": "Visualization", "release_date": "2013-03-29T11:00:00-04:00", "title": "Comet ISON Approaches Perihelion", "description": "Currently located beyond the orbit of Jupiter, Comet ISON is heading for a very close encounter with the sun next year. In November 2013, it will pass less than 0.012 Astronomical Units (Wikipedia) (1.8 million kilometers) from the center of the Sun, 1.2 million kilometers from the solar surface. The fierce heating it experiences in that approach could turn the comet into a bright naked-eye object.NOTE: This visualization was revised in March 2013 to fix an ephemeris error. Other enhancements were included in the revision. Also fixed an error where perihelion distance was mistakenly labeled as distance from solar surface. || ", "hits": 177 }, { "id": 11145, "url": "https://svs.gsfc.nasa.gov/11145/", "result_type": "Produced Video", "release_date": "2013-02-06T10:00:00-05:00", "title": "Counting Comets", "description": "As comets orbit the sun, many come too close and evaporate completely. Others survive the journey, but their orbits gradually move closer to the sun. Ultimately, the heat of the solar atmosphere melts the ice that binds a comet together and breaks it apart into smaller bodies that follow similar orbits. These are the sungrazers, and scientists and amateur astronomers are seeing more of them than ever. As of 1979, we only knew of a dozen. Nearing the end of 2012, thanks to better observation tools, we have now seen 3,000. The bulk of the sungrazers are known as Kreutz comets, and are likely derived from a single original comet observed as early as 371 AD. Watch the videos to learn more about and see NASA satellite footage of sungrazing comets. || ", "hits": 31 }, { "id": 11156, "url": "https://svs.gsfc.nasa.gov/11156/", "result_type": "Produced Video", "release_date": "2013-02-06T10:00:00-05:00", "title": "Sungrazers Galore", "description": "Before 1979, there were less than a dozen known sungrazing comets. As of December 2012, we know of 2,500. Why did this number increase? With solar observatories like SOHO, STEREO, and SDO, we have not only better means of viewing the sun, but also the comets that approach it. SOHO allows us to see smaller, fainter comets closer to the sun than we have ever been able to see before. Even though many of these comets do not survive their journey past the sun, they survive long enough to be observed, and be added to our record of sungrazing comets. || ", "hits": 26 }, { "id": 4018, "url": "https://svs.gsfc.nasa.gov/4018/", "result_type": "Visualization", "release_date": "2012-12-10T00:00:00-05:00", "title": "Kreutz Comet Orbits", "description": "HD movie of representative orbit of a sungrazing comet. || Kreutz.noslate_HEEmove.HD1080i.0350.jpg (1920x1080) [582.0 KB] || Kreutz.noslate_HEEmove.HD1080i.0350_web.png (320x180) [92.0 KB] || Kreutz.noslate_HEEmove.HD1080i.0350_thm.png (80x40) [4.5 KB] || Kreutz-Lovejoy_HD1080.mov (1920x1080) [13.2 MB] || Kreutz-Lovejoy_HD1080.mp4 (1920x1080) [13.2 MB] || 1920x1080_16x9_30p (1920x1080) [64.0 KB] || Kreutz-Lovejoy_HD1080.webmhd.webm (960x540) [2.9 MB] || Kreutz-Lovejoy_iPod.m4v (640x360) [3.0 MB] || ", "hits": 25 }, { "id": 11158, "url": "https://svs.gsfc.nasa.gov/11158/", "result_type": "Produced Video", "release_date": "2012-12-04T15:00:00-05:00", "title": "Sun Grazing Comets as Solar Probes", "description": "To observe how winds move high in Earth's atmosphere, scientists sometimes release clouds of barium as tracers to track how the material corkscrews and sweeps around — but scientists have no similar technique to study the turbulent atmosphere of the sun. So researchers were excited in December 2011, when Comet Lovejoy swept right through the sun's corona with its long tail streaming behind it. NASA's Solar Dynamics Observatory (SDO) captured images of the comet, showing how its long tail was buffeted by systems around the sun, offering scientists a unique way of observing movement as if they'd orchestrated the experiment themselves. Since comet tails have ionized gases, they are also affected by the sun's magnetic field, and can act as tracers of the complex magnetic system higher up in the atmosphere. Comets can also aid in the study of coronal mass ejections and the solar wind.Watch this video on YouTube. || ", "hits": 41 }, { "id": 11124, "url": "https://svs.gsfc.nasa.gov/11124/", "result_type": "Produced Video", "release_date": "2012-11-08T00:00:00-05:00", "title": "Out Of Focus", "description": "Twice a year, for three weeks near the vernal and autumnal equinox, NASA's Solar Dynamics Observatory (SDO) spacecraft moves into its eclipse season—a brief spell when Earth blocks its view of the sun for a period of time each day. Any spacecraft observing the sun from an orbit around Earth has to contend with such eclipses. But SDO's orbit is designed to minimize their occurrence as they also cause a temporary blurring of images in one of its instruments. The most recent eclipse season took place September 6-29, 2012. As Earth entered and exited SDO's field of vision, its advanced imaging instruments captured partial views of the sun at multiple wavelengths. Solar scientists do not get much use from these images, though atmospheric researchers may be able to gain some insights by observing the sun's light as it moves through Earth's atmosphere. Watch the video to see images of Earth passing between the sun and SDO. || ", "hits": 33 }, { "id": 11111, "url": "https://svs.gsfc.nasa.gov/11111/", "result_type": "Produced Video", "release_date": "2012-10-05T10:00:00-04:00", "title": "Getting NASA's SDO into Focus", "description": "From Sep. 6 to Sep. 29, 2012, NASA's Solar Dynamic Observatory (SDO) moved into its semi-annual eclipse season, a time when Earth blocks the telescope's view of the sun for a period of time each day. Scientists choose orbits for solar telescopes to minimize eclipses as much as possible, but they are a fact of life — one that comes with a period of fuzzy imagery directly after the eclipse. The Helioseismic and Magnetic Imager (HMI) on SDO observes the sun through a glass window. The window can change shape in response to temperature changes, and does so dramatically and quickly when it doesn't directly feel the sun's heat. \"You've got a piece of glass looking at the sun, and then suddenly it isn't,\" says Dean Pesnell, the project scientist for SDO at NASA's Goddard Space Flight Center in Greenbelt, Md. \"The glass gets colder and flexes. It becomes like a lens. It's as if we put a set of eye glasses in front of the instrument, causing the observations to blur.\" To counteract this effect, HMI was built with heaters to warm the window during an eclipse. By adjusting the timing and temperature of the heater, the HMI team has learned the best procedures for improving resolution quickly. Without adjusting the HMI front window heaters, it takes about two hours to return to optimal observing. Over the two years since SDO launched in 2010, the team has brought the time it takes to get a clear image down from 60 minutes to around 45 to 50 minutes after an eclipse. \"We allocated an hour for these more blurry images,\" says Pesnell. \"And we've learned to do a lot better than that. With 45 eclipses a year, the team gets a lot of practice.\" SDO will enter its next eclipse season on March 3, 2013. || ", "hits": 48 }, { "id": 3940, "url": "https://svs.gsfc.nasa.gov/3940/", "result_type": "Visualization", "release_date": "2012-06-12T00:00:00-04:00", "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. || ", "hits": 32 }, { "id": 3828, "url": "https://svs.gsfc.nasa.gov/3828/", "result_type": "Visualization", "release_date": "2011-12-07T00:00:00-05:00", "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. || ", "hits": 139 }, { "id": 10784, "url": "https://svs.gsfc.nasa.gov/10784/", "result_type": "Produced Video", "release_date": "2011-07-27T08:00:00-04:00", "title": "Revealing the Old Man in the Sun", "description": "When one moves through 11 SDO images taken at the same time, and shown in order from the lowest temperature material being imaged to the highest, a funny thing thing happens: the features of a face in the sun begin to appear. The movie underscores the fact that images taken at different wavelengths do reveal different features. The images also start at the sun's surface and gradually move out to the sun's upper corona. Enjoy the show! || ", "hits": 107 }, { "id": 3838, "url": "https://svs.gsfc.nasa.gov/3838/", "result_type": "Visualization", "release_date": "2011-07-01T10:00:00-04:00", "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). || ", "hits": 54 }, { "id": 10733, "url": "https://svs.gsfc.nasa.gov/10733/", "result_type": "Produced Video", "release_date": "2011-03-03T16:00:00-05:00", "title": "SDO First Light Media", "description": "A compilation of some of the videos and stills used during the SDO First Light press conference.There are more video and stills available. || ", "hits": 61 }, { "id": 10551, "url": "https://svs.gsfc.nasa.gov/10551/", "result_type": "Produced Video", "release_date": "2010-06-10T00:00:00-04:00", "title": "SDO First Light Press Conference", "description": "A unique NASA spacecraft launched February 11, 2010, called the Solar Dynamics Observatory, or SDO, has started delivering images of the sun that have astonished scientists. SDO is the most advanced spacecraft ever designed to study the sun and its dynamic behavior. The spacecraft can produce images with clarity ten times better than high definition television and provide more comprehensive science data faster than any solar observing spacecraft in history. The goal of the mission is to help scientists study solar activity to improve forecasts of how the sun affects Earth.On April 21, 2010, NASA held a live press conference at the Newseum in Washington D.C. to unveil the first images and videos from SDO—SDO's First Light.A version of the press conference with captioning is available. || ", "hits": 28 }, { "id": 10535, "url": "https://svs.gsfc.nasa.gov/10535/", "result_type": "Produced Video", "release_date": "2010-05-18T09:00:00-04:00", "title": "SDO: Commissioning and Handover", "description": "In order to provide the clearest scientific data for its entire 5 year mission, SDO had to undergo a rigorous, 2 month testing phase. After giving it an all-clear, the team of people who designed, built and tested the satellite now have to say goodbye as they hand it over to the scientists who will begin collecting data. || ", "hits": 12 }, { "id": 10610, "url": "https://svs.gsfc.nasa.gov/10610/", "result_type": "Produced Video", "release_date": "2010-04-28T11:00:00-04:00", "title": "SDO First Light High Resolution Stills", "description": "Stills from the AIA instrument on SDO. They show the March 30, 2010 \"First Light\" prominence eruption captured just after the AIA sensors were activated. All images are from the ultraviolet part of the spectrum, specifically the wavelengths of 304, 211, 193, and 171 Ångstroms. The stills are in multiple resolutions and are available as tiff and jpeg files. || ", "hits": 89 }, { "id": 3692, "url": "https://svs.gsfc.nasa.gov/3692/", "result_type": "Visualization", "release_date": "2010-04-21T14:15:00-04:00", "title": "SDO/AIA CME Event of April 8, 2010 (Multiband)", "description": "This is a close-up view of the April 8 CME in ultraviolet light which reveals a wave (darker regions) expanding outward from the flare event. This movie creates a color image by combining filters for 211 Ångstroms (red), 193 Ångstroms (green) and 171 Ångstroms (blue). || ", "hits": 19 }, { "id": 3693, "url": "https://svs.gsfc.nasa.gov/3693/", "result_type": "Visualization", "release_date": "2010-04-21T14:15:00-04:00", "title": "SDO/AIA Zoom-In on Launching Filament (Bands 304, 171, 211)", "description": "As the AIA camera was activated, one of its first views was this fliament launching from the Sun. || ", "hits": 14 }, { "id": 3695, "url": "https://svs.gsfc.nasa.gov/3695/", "result_type": "Visualization", "release_date": "2010-04-21T14:15:00-04:00", "title": "SDO/AIA CME Event of April 8, 2010 Full Disk (Multiband)", "description": "This visualization is a full-disk view of the CME launched from the Sun on April 8, 2010. This is a 3-color image produced by combining three different filters from the AIA instrument: 211 (red), 193 (green), and 171 (blue). || ", "hits": 27 }, { "id": 3696, "url": "https://svs.gsfc.nasa.gov/3696/", "result_type": "Visualization", "release_date": "2010-04-21T14:15:00-04:00", "title": "SDO/HMI Continuum Full Disk View - March 29, 2010", "description": "This early sequence of HMI images from SDO focuses on a large sunspot group of Solar Cycle 24. || ", "hits": 33 }, { "id": 3697, "url": "https://svs.gsfc.nasa.gov/3697/", "result_type": "Visualization", "release_date": "2010-04-21T14:15:00-04:00", "title": "SDO/HMI Magnetogram Full Disk View - March 29, 2010", "description": "This early sequence of images from the HMI imager is processed to reveal the magnetic field structure (magnetogram). White locations represent a positive magnetic field value (north polarity) while black represents a negative magnetic field value (south polarity). Grey is zero magnetic field.The black and white region slightly above the center corresponds to a visible sunspot. Weaker magnetic regions are visible around the disk. || ", "hits": 29 }, { "id": 3703, "url": "https://svs.gsfc.nasa.gov/3703/", "result_type": "Visualization", "release_date": "2010-04-21T14:15:00-04:00", "title": "SDO/HMI Continuum Sunspot Closeup - March 29, 2010", "description": "This is a close-up view of a large sunspot group visible as the HMI instrument turned on their imagers. || ", "hits": 26 }, { "id": 3704, "url": "https://svs.gsfc.nasa.gov/3704/", "result_type": "Visualization", "release_date": "2010-04-21T14:15:00-04:00", "title": "SDO/HMI Continuum Sunspot Zoom-in - March 29, 2010", "description": "This is a zoom-in view of a large sunspot group visible as the HMI instrument turned on their imagers. || ", "hits": 36 }, { "id": 3705, "url": "https://svs.gsfc.nasa.gov/3705/", "result_type": "Visualization", "release_date": "2010-04-21T14:15:00-04:00", "title": "SDO/HMI Magnetogram Sunspot Close-Up - March 29, 2010", "description": "This early sequence of images from the HMI imager is processed to reveal the magnetic field structure (magnetogram). White locations represent a positive magnetic field value (north polarity) while black represents a negative magnetic field value (south polarity). Grey is zero magnetic field.This version is a close-up view of a large sunspot group. || ", "hits": 72 }, { "id": 3706, "url": "https://svs.gsfc.nasa.gov/3706/", "result_type": "Visualization", "release_date": "2010-04-21T14:15:00-04:00", "title": "SDO/HMI Magnetogram Sunspot Zoom-In - March 29, 2010", "description": "This early sequence of images from the HMI imager is processed to reveal the magnetic field structure (magnetogram). White locations represent a positive magnetic field value (north polarity) while black represents a negative magnetic field value (south polarity). Grey is zero magnetic field.This movie zooms-in on a large sunspot group. || ", "hits": 22 }, { "id": 3712, "url": "https://svs.gsfc.nasa.gov/3712/", "result_type": "Visualization", "release_date": "2010-04-21T14:15:00-04:00", "title": "SDO/HMI Continuum Full Disk View - April 7, 2010", "description": "This early sequence of HMI images from SDO focuses on a large sunspot group of Solar Cycle 24. || ", "hits": 82 }, { "id": 3713, "url": "https://svs.gsfc.nasa.gov/3713/", "result_type": "Visualization", "release_date": "2010-04-21T14:15:00-04:00", "title": "SDO/HMI Magnetogram Full Disk View - April 7, 2010", "description": "This early sequence of images from the HMI imager is processed to reveal the magnetic field structure (magnetogram). White locations represent a positive magnetic field value (north polarity) while black represents a negative magnetic field value (south polarity). Gray is zero magnetic field.Notice that the surface magnetic fields reveal much more structure than the white-light images in SDO/HMI Continuum Full Disk View - April 7, 2010. || ", "hits": 21 }, { "id": 3714, "url": "https://svs.gsfc.nasa.gov/3714/", "result_type": "Visualization", "release_date": "2010-04-21T14:15:00-04:00", "title": "SDO/HMI Dopplergram Sunspot Close-Up - March 29, 2010", "description": "The dopplergram from SDO/HMI data shows the velocity of solar material on the line-of-sight. White pixels are moving away from the camera and black pixels are moving towards the camera. || ", "hits": 19 }, { "id": 3715, "url": "https://svs.gsfc.nasa.gov/3715/", "result_type": "Visualization", "release_date": "2010-04-21T14:15:00-04:00", "title": "SDO/AIA Close-up on Launching Filament (band 304)", "description": "A close-up view of the filament launch in the 304 band, which corresponds to a wavelength of about 304 Ångstroms. || ", "hits": 18 }, { "id": 3716, "url": "https://svs.gsfc.nasa.gov/3716/", "result_type": "Visualization", "release_date": "2010-04-21T14:15:00-04:00", "title": "SDO/AIA Full-Disk View of Launching Filament (Band 304)", "description": "Full disk view of a filament launch in the SDO AIA 304 band. || ", "hits": 24 }, { "id": 3717, "url": "https://svs.gsfc.nasa.gov/3717/", "result_type": "Visualization", "release_date": "2010-04-21T14:15:00-04:00", "title": "SDO/AIA Zoom-out of Launching Filament (Band 304)", "description": "This view of the filament launch loops several times before pulling out to show the full solar disk. || ", "hits": 13 }, { "id": 3683, "url": "https://svs.gsfc.nasa.gov/3683/", "result_type": "Visualization", "release_date": "2010-04-02T00:00:00-04:00", "title": "Halloween 2003 Solar Storms: GOES/SXI X-ray view", "description": "Here is a view of the full solar disk during a two-week period in October and November of 2003 which exhibited some of the largest solar activity events since the advent of space-based solar observing. The GOES-12/Solar X-Ray Imager was experiencing significant problems during this time period and was offline during part of the opening and closing portions of this movie, which is why there is a significant number of black frames. Actual data collection began on October 28, 2003 and terminated on November 5, 2003.This movie is part of a series of movies with matching cadence designed to play synchronously with each other. The other movies in this series are Halloween 2003 Solar Storms: SOHO/EIT Ultraviolet, 195 angstromsHalloween 2003 Solar Storms: SOHO/EIT Ultraviolet, 304 angstromsHalloween 2003 Solar Storms: SOHO/MDI ContinuumHalloween 2003 Solar Storms: SOHO/MDI MagnetogramsHalloween 2003 Solar Storms: SOHO/EIT and SOHO/LASCO || ", "hits": 22 }, { "id": 3691, "url": "https://svs.gsfc.nasa.gov/3691/", "result_type": "Visualization", "release_date": "2010-03-31T00:00:00-04:00", "title": "A Comparative View of the Sun: SDO/AIA 193 and SOHO/EIT 195", "description": "This movie compares the spatial and temporal resolutions of the SDO/AIA (Atmospheric Imaging Assembly) imager to the SOHO/EIT (Extreme ultraviolet Imaging Telescope) imager. SOHO/EIT's highest resolution is 1024x1024 pixels with images taken about every 12 minutes for the 195 Ångstrom band. The SDO/AIA 193 band takes images at 4096x4096 pixels every twelve seconds!In this movie we can see the difference this makes for a closeup view of Active Region 1087. EIT reveals changes in the active region, which AIA reveals many details.This visualization is a companion piece to A Comparative View of the Sun: SDO/AIA 193 and STEREO-B/EUVI 195. || ", "hits": 31 }, { "id": 3694, "url": "https://svs.gsfc.nasa.gov/3694/", "result_type": "Visualization", "release_date": "2010-03-24T00:00:00-04:00", "title": "A Comparative View of the Sun: SDO/AIA 193 and STEREO-B/EUVI 195", "description": "This movie compares the spatial and temporal resolutions of the SDO/AIA (Atmospheric Imaging Assembly) imager to the STEREO/EUVI (Extreme UltraViolet Imager) imager. STEREO-B/EUVI's highest resolution is 2048x2048 pixels with images taken about every 5 minutes for the 195 Ångstrom band. The SDO/AIA 193 band takes images at 4096x4096 pixels every twelve seconds!While STEREO's vantage point at this time is very different from SDO, we can still identify some features of the Active Region 1087 in these two views. EUVI shows the launch of the filament, while AIA reveals many finer details.This visualization is a companion piece to A Comparative View of the Sun: SDO/AIA 193 and SOHO/EIT 195. || ", "hits": 16 }, { "id": 20180, "url": "https://svs.gsfc.nasa.gov/20180/", "result_type": "Animation", "release_date": "2010-01-21T00:00:00-05:00", "title": "SDO's Geosynchronus Orbit", "description": "This animation shows the SDO satellite in its inclined geosynchronous orbit. SDO's geosynchronous orbit will keep the observatory in constant view of the dedicated relay station's two 18-meter dishes around the clock for the duration of the observatory's five-year mission. || ", "hits": 28 }, { "id": 20181, "url": "https://svs.gsfc.nasa.gov/20181/", "result_type": "Animation", "release_date": "2010-01-21T00:00:00-05:00", "title": "SDO Figure 8", "description": "This video shows the dedicated ground station in White Sands, New Mexico and the path of the Solar Dynamics Observatory satellite. SDO is in an inclined geosynchronous orbit and traces a figure-8 every 24 hours. This allows the satellite to keep a continuous, high-data-rate link with the ground. || ", "hits": 32 }, { "id": 20182, "url": "https://svs.gsfc.nasa.gov/20182/", "result_type": "Animation", "release_date": "2010-01-21T00:00:00-05:00", "title": "SDO Launch and Deployment", "description": "This animation follows the Solar Dynamics Observatory from its launch at pad 41A from Kennedy Space Center through deployment. || ", "hits": 21 }, { "id": 10441, "url": "https://svs.gsfc.nasa.gov/10441/", "result_type": "Produced Video", "release_date": "2009-07-02T15:00:00-04:00", "title": "SDO's Science", "description": "These animations and web shorts explain how SDO's instruments will look at the sun and allow us to better predict how the sun will affect us in the future. || ", "hits": 45 }, { "id": 3566, "url": "https://svs.gsfc.nasa.gov/3566/", "result_type": "Visualization", "release_date": "2008-12-18T00:00:00-05:00", "title": "Multi-Sun Composition", "description": "This movie is a composition of multiple solar datasets synchronized in time. The time frame is late October and early November of 2003, the time of some record-breaking solar activity.The background of the movie shows the view of the wide-angle coronagraphs (blue/white), or LASCO instruments, aboard SOHO. They show streams of electrons outbound from the Sun, part of the solar atmosphere. The central green image is the Sun in ultraviolet light from the EIT instrument. Note that flashes of solar flares in the ultraviolet quickly propagate out from the Sun and are visible in LASCO. These events are coronal mass ejections, or CMEs.Overlaid on the upper left is a better view of the EIT ultraviolet image at a wavelength of 195 angstroms (19.5 nanometers).On the lower left, the orange movie is the EIT ultraviolet movie at 304 angstroms (30.4 nanometers).On the upper right is a solar magnetogram, taken by the MDI instrument. The white regions correspond to positive (north) magnetic flux and the dark regions to negative (south) magnetic flux.The colors for the sequences above are not real. They are chosen by convention since the properties recorded by the cameras are not visible to the human eye.The final image on the lower right is also from MDI. It is a combination of several optical wavelengths and is the best representation from SOHO of the Sun in visible light, as we would see it through ground-based telescopes.The movies that are part of this composition are also available individually on the SVS site: Halloween Solar Storms 2003: SOHO/EIT and SOHO/LASCOHalloween Solar Storms 2003: SOHO/EIT Ultraviolet, 195 angstromsHalloween Solar Storms 2003: SOHO/EIT Ultraviolet, 304 angstromsHalloween Solar Storms 2003: SOHO/MDI ContinuumHalloween Solar Storms 2003: SOHO/MDI Magnetograms || ", "hits": 32 }, { "id": 3496, "url": "https://svs.gsfc.nasa.gov/3496/", "result_type": "Visualization", "release_date": "2008-08-19T00:00:00-04:00", "title": "The Solar Dynamo: Plasma Flows", "description": "In this visualization, we illustrate the fluid flows in the Sun which drive the solar magnetic dynamo. The flows can be considered as a combination of two components, a toroidal component and a meridional component. The toroidal flow corresponds to the rotational motion of the Sun. In the cut-away view, this motion is represented by the streaking flow vectors. The color code of the cross-section on the right-hand side illustrates the rotational period of this flow. Here we see that flow near the equator (in violet) takes about 24.5 days to make it all the way around the Sun. As we move to higher latitudes, we see that the flow gets steadily slower, increasing the time it takes to go around the Sun to as much as 34 days (in red) near the poles. A non-uniform fluid flow such as this is known as differential rotation. This motion in the interior can be measured at the solar surface through techniques of helioseismology.Deeper into the Sun, we see the different colors of the outer layers transition to a solid color (olive green). This transition point is called the tachocline. It is the boundary between the outer zone of the Sun where thermal energy is transferred by convection (the convective zone), and the inner region of the Sun where thermal energy is transferred by radiation (the radiative zone). The radiative zone is believed to rotate as a solid body with a period of about 28 days in this model.The yellow and white center in this model represents the solar radiative zone.In the cross-section on the left-side, we represent the other component of the flow, called the meridional flow, which moves plasma between the equator and the polar regions.These flows of solar plasma are used as input data for dynamo modeling (see The Solar Dynamo: Toroidal and Poloidal Fields and The Solar Dynamo: Toroidal and Radial Fields.) || ", "hits": 143 }, { "id": 3521, "url": "https://svs.gsfc.nasa.gov/3521/", "result_type": "Visualization", "release_date": "2008-08-19T00:00:00-04:00", "title": "The Solar Dynamo: Toroidal and Poloidal Magnetic Fields", "description": "Using the solar plasma flows as input (see The Solar Dynamo: Plasma Flows), the equations of magnetohydrodynamics, and 'seeding' the calculations with an initial small magnetic field, one can compute how a magnetic field can grow and be maintained. This is the dynamo process, the net result being that part of the Sun's outflowing thermal convective energy from nuclear processes is used to create the magnetic field.In this view of the solar dynamo mechanism, we examine the evolution of the toroidal magnetic field, the field intensity represented by colors on the right-hand cross-section, and the poloidal magnetic potential field, represented by colors on the left-hand cross-section. The poloidal magnetic potential is a scalar quantity that contains information about the radial and latitudinal magnetic field vectors. To see the radial magnetic field, see The Solar Dynamo: Toroidal and Radial Magnetic Fields.In this visualization, the magnetic field lines (represented by the 'copper wire' structures) are 'snapshots' of the field structure constructed at each time step of the model. These field lines should not be considered as 'moving' or 'stretching' as the model evolves in time. Even this simplified model reproduces a number of characteristics observed in the actual solar magnetic field. Cyclic behavior with oscillations in the magnetic field amplitude.Magnetic regions at the surface migrate from high latitudes towards the equator as the solar cycle progresses. This reproduces the \"Butterfly Diagram\" pattern.Surface magnetic polarities reverse with each cycleBecause this model is axisymmetric, it cannot simulate non-axisymmetric features such as active longitudes. || ", "hits": 228 }, { "id": 3583, "url": "https://svs.gsfc.nasa.gov/3583/", "result_type": "Visualization", "release_date": "2008-08-19T00:00:00-04:00", "title": "The Solar Dynamo: Toroidal and Radial Magnetic Fields", "description": "Using the solar plasma flows as input (see The Solar Dynamo: Plasma Flows), the equations of magnetohydrodynamics, and 'seeding' the calculations with an initial small magnetic field, one can compute how a magnetic field can grow and be maintained. This is the dynamo process, the net result being that part of the Sun's outflowing thermal convective energy from nuclear processes is used to create the magnetic field.In this view of the solar dynamo mechanism, we examine the evolution of the toroidal magnetic field, intensities represented by color on the right-hand cross-section, and the radial magnetic field, represented on the left-hand cross-section. To see the poloidal magnetic vector potential, see The Solar Dynamo: Toroidal and Poloidal Magnetic Fields.In this visualization, the magnetic field lines (represented by the 'copper wire' structures) are 'snapshots' of the field structure constructed at each time step of the model. These field lines should not be considered as 'moving' or 'stretching' as the model evolves in time.Even this simplified model reproduces a number of characteristics observed in the actual solar magnetic field.Cyclic behavior with oscillations in the magnetic field amplitude.Magnetic regions at the surface migrate from high latitudes towards the equator. This reproduces the \"Butterfly Diagram\" pattern.Surface magnetic polarities reverse with each cycleBecause this model is axisymmetric, it cannot simulate non-axisymmetric features such as active longitudes. || ", "hits": 106 }, { "id": 3535, "url": "https://svs.gsfc.nasa.gov/3535/", "result_type": "Visualization", "release_date": "2008-08-15T00:00:00-04:00", "title": "Halloween Storms 2003: SOHO/EIT and TRACE at 195 Angstroms", "description": "This visualization compares the full-disk solar view of SOHO/EIT (green, on the left) with the small field of view of the TRACE ultraviolet telescope (gold, on the right). The yellow border of the TRACE imagery is projected on the appropriate location on the green EIT imagery. Notice that TRACE can track features as they move across the solar disk. The instrument pointing is adjusted on a regular basis, which can produce a considerable amount of jittering in the image. This is a variation on the treatment of the same data as Solar Dynamics Observatory (SDO): Data Collection Comparison.Note that this movie does not play synchronous with the other animations that are part of the SDO Prelaunch package. || ", "hits": 34 }, { "id": 3500, "url": "https://svs.gsfc.nasa.gov/3500/", "result_type": "Visualization", "release_date": "2008-04-02T00:00:00-04:00", "title": "Halloween 2003 Solar Storms: SOHO/EIT Ultraviolet, 195 Angstroms", "description": "Here is a view of the full solar disk during a two-week period in October and November of 2003 which exhibited some of the largest solar activity events since the advent of space-based solar observing. The Extreme ultraviolet Imaging Telescope (EIT) collects solar images in an extremely short wavelength of ultraviolet light, not visible from the surface of the Earth. The narrow wavelength band at 195 angstroms corresponds (19.5 nanometers) corresponds to a spectral line of multiply-ionized iron atoms. This movie is part of a series of movies with matching cadence designed to play synchronously with each other. The other movies in this series are Halloween 2003 Solar Storms: SOHO/EIT Ultraviolet, 304 A Halloween 2003 Solar Storms: SOHO/MDI Continuum Halloween 2003 Solar Storms: SOHO/MDI Magnetograms Halloween 2003 Solar Storms: SOHO/EIT and SOHO/LASCO For more information, visit the SOHO project page. || ", "hits": 41 }, { "id": 3501, "url": "https://svs.gsfc.nasa.gov/3501/", "result_type": "Visualization", "release_date": "2008-04-02T00:00:00-04:00", "title": "Halloween 2003 Solar Storms: SOHO/EIT Ultraviolet, 304 Angstroms", "description": "Here is a view of the full solar disk during a two-week period in October and November of 2003 which exhibited some of the largest solar activity events since the advent of space-based solar observing. The Extreme ultraviolet Imaging Telescope (EIT) collects solar images in an extremely short wavelength of ultraviolet light, not visible from the surface of the Earth. The narrow wavelength band at 304 Ångstroms corresponds (30.4 nanometers) corresponds to a spectral line of multiply-ionized iron atoms. This movie is part of a series of movies with matching cadence designed to play synchronously with each other. The other movies in this series are Halloween 2003 Solar Storms: SOHO/EIT Ultraviolet, 195 ÅHalloween 2003 Solar Storms: SOHO/MDI Continuum Halloween 2003 Solar Storms: SOHO/MDI Magnetograms Halloween 2003 Solar Storms: SOHO/EIT and SOHO/LASCO For more information, visit the SOHO project page. || ", "hits": 34 }, { "id": 3502, "url": "https://svs.gsfc.nasa.gov/3502/", "result_type": "Visualization", "release_date": "2008-04-02T00:00:00-04:00", "title": "Halloween 2003 Solar Storms: SOHO/MDI Continuum", "description": "Here is a view of the full solar disk during a two-week period in October and November of 2003 which exhibited some of the largest solar activity events since the advent of space-based solar observing. The Michelson Doppler Interferometer (MDI) records images at several very narrow wavelength bands in the visible light. These images are often used as proxies for white-light solar images. This movie is part of a series of movies with matching cadence designed to play synchronously with each other. The other movies in this series are Halloween 2003 Solar Storms: SOHO/EIT Ultraviolet, 195 angstroms Halloween 2003 Solar Storms: SOHO/EIT Ultraviolet, 304 angstroms Halloween 2003 Solar Storms: SOHO/MDI Magnetograms Halloween 2003 Solar Storms: SOHO/EIT and SOHO/LASCO For more information, visit the SOHO project page. || ", "hits": 27 }, { "id": 3503, "url": "https://svs.gsfc.nasa.gov/3503/", "result_type": "Visualization", "release_date": "2008-04-02T00:00:00-04:00", "title": "Halloween 2003 Solar Storms: SOHO/MDI Magnetograms", "description": "Here is a view of the full solar disk during a two-week period in October and November of 2003 which exhibited some of the largest solar activity events since the advent of space-based solar observing.The Michelson Doppler Interferometer (MDI) takes images of the Sun at five very narrow wavelength bands and four different polarizations in visible light. For this sequence, the images are processed in a form that reveals the magnetic field strength on the solar photosphere. Other combinations of the images act as white-light images and dopplergrams (which measure the velocity of the solar 'surface').This movie is part of a series of movies with matching cadence designed to play synchronously with each other. The other movies in this series are Halloween 2003 Solar Storms: SOHO/EIT Ultraviolet, 195 angstroms Halloween 2003 Solar Storms: SOHO/EIT Ultraviolet, 304 angstroms Halloween 2003 Solar Storms: SOHO/MDI Continuum Halloween 2003 Solar Storms: SOHO/EIT and SOHO/LASCO For more information, visit the SOHO project page.. || ", "hits": 49 }, { "id": 3504, "url": "https://svs.gsfc.nasa.gov/3504/", "result_type": "Visualization", "release_date": "2008-04-02T00:00:00-04:00", "title": "Halloween 2003 Solar Storms: SOHO/EIT and SOHO/LASCO", "description": "Here is a view of the solar disk in 195 Å ultraviolet light (colored green in this movie) and the Sun's extended atmosphere, or corona, (blue and white in this movie). The corona is visible to the SOHO/LASCO coronagraph instruments, which block the bright disk of the Sun so the significantly fainter corona can be seen. In this movie, the inner coronagraph (designated C2) is combined with the outer coronagraph (C3). This movie covers a two week period in October and November 2003 which exhibited some of the largest solar activity events since the advent of space-based solar observing.As the movie plays, we can observe a number of features of the active Sun. Long streamers radiate outward from the Sun and wave gently due to their interaction with the solar wind. The bright white regions are visible due to their high density of free electrons which scatter the light from the photosphere towards the observer. Protons and other ionized atoms are there as well, but are not as visible since they do not interact with photons as strongly as electrons. Coronal Mass Ejections (CMEs) are occasionally observed launching from the Sun. Some of these launch particle events which can saturate the cameras with snow-like artifacts.Also visible in the coronagraphs are stars and planets. Stars are seen to drift slowly to the right, carried by the relative motion of the Sun and the Earth. The planet Mercury is visible as the bright point moving left of the Sun. The horizontal 'extension' in the image is called 'blooming' and is due to a charge leakage along the readout wires in the CCD imager in the camera.This movie is part of a series of movies with matching cadence designed to play synchronously with each other. The other movies in this series are Halloween 2003 Solar Storms: SOHO/EIT Ultraviolet, 195 angstromHalloween 2003 Solar Storms: SOHO/EIT Ultraviolet, 304 angstromHalloween 2003 Solar Storms: SOHO/MDI Continuum Halloween 2003 Solar Storms: SOHO/MDI Magnetograms For more information, visit the SOHO project page.. || ", "hits": 66 }, { "id": 10188, "url": "https://svs.gsfc.nasa.gov/10188/", "result_type": "Produced Video", "release_date": "2008-03-02T00:00:00-05:00", "title": "NASA's SDO Mission", "description": "A new NASA spacecraft called the Solar Dynamics Observatory (SDO) will deliver startling images of the sun with ten times more detail than HDTV. The goal of the mission is to help scientists zoom in on solar activity such as sunspots, solar flares and coronal mass ejections, thus improving forcasts of solar storms. The complete script is available. For more information on the Solar Dynamics Observatory, check out their web site at http://sdo.gsfc.nasa.gov. || ", "hits": 40 }, { "id": 20118, "url": "https://svs.gsfc.nasa.gov/20118/", "result_type": "Animation", "release_date": "2007-09-10T00:00:00-04:00", "title": "The Solar Dynamics Observatory (SDO)", "description": "SDO is designed to help us understand the Sun's influence on Earth and Near-Earth space by studying the solar atmosphere on small scales of space and time and in many wavelengths simultaneously. || ", "hits": 62 }, { "id": 3435, "url": "https://svs.gsfc.nasa.gov/3435/", "result_type": "Visualization", "release_date": "2007-08-14T00:00:00-04:00", "title": "Solar Dynamics Observatory (SDO): Data Collection Comparison", "description": "Solar Dynamics Observatory (SDO) will dramatically increase our ability to collect data about the Sun. This visualization compares the temporal and spatial resolution of SOHO/EIT with TRACE. SDO will enable TRACE-like image and temporal resolution over the entire solar disk. This movie opens with a full-disk view of the Sun in ultraviolet light (195 angstroms) from SOHO/EIT using the traditional TRACE 'gold' color table. We zoom in on the active region on the western limb where the TRACE instrument is pointing and fade-in an inset of the higher-resolution TRACE data. To emphasize the comparison, the TRACE inset is moved aside (with a solid white border) revealing the matching EIT data view (enclosed in the faint white border). At this point, we step through the time series of data frames. In this movie, much of the TRACE imagery is collected at time intervals between 3 and 40 seconds. On the other hand, a new SOHO/EIT image is taken about every 12 minutes (720 seconds). The SDO Atmospheric Imaging Assembly (AIA) will take full-disk solar images at four times the SOHO/EIT spatial resolution, a whopping 4096x4096, and at least 70 times the temporal resolution, 10 seconds or better per image. This creates a data rate over 1000x higher than SOHO/EIT. It is roughly equivalent to TRACE spatial and temporal resolution, but over the entire solar disk. || ", "hits": 42 } ] }