{ "count": 49, "next": null, "previous": null, "results": [ { "id": 4892, "url": "https://svs.gsfc.nasa.gov/4892/", "result_type": "Visualization", "release_date": "2022-01-18T12:00:00-05:00", "title": "Faculae and Sunspots at Solar Maximum and Solar Minimum", "description": "Movie of SDO/AIA 1700 angstrom imagery, collected near solar maximum (April 2014). Note the small dark regions (sunspots) and the brighter speckled regions (faculae) around them. || SolarMax_AIA1700A_stand.HD1080i.00300_print.jpg (1024x576) [61.4 KB] || SolarMax_AIA1700A_stand.HD1080i.00300_searchweb.png (320x180) [35.9 KB] || SolarMax_AIA1700A_stand.HD1080i.00300_thm.png (80x40) [3.3 KB] || SolarMax_AIA1700A (1920x1080) [0 Item(s)] || SolarMax_AIA1700A_stand.HD1080i_p30.mp4 (1920x1080) [66.8 MB] || SolarMax_AIA1700A_stand.HD1080i_p30.webm (1920x1080) [3.0 MB] || SolarMax_AIA1700A (3840x2160) [0 Item(s)] || SolarMax_AIA1700A_stand.UHD2160_p30.mp4 (3840x2160) [270.8 MB] || SolarMax_AIA1700A_stand.HD1080i_p30.mp4.hwshow [201 bytes] || ", "hits": 112 }, { "id": 4907, "url": "https://svs.gsfc.nasa.gov/4907/", "result_type": "Visualization", "release_date": "2021-06-18T11:00:00-04:00", "title": "A Big Sunspot from Solar Cycle 24", "description": "A large sunspot rotates across the view in SDO/HMI || BigSunspot_HMIintensity_stand.HD1080i.00300_print.jpg (1024x576) [50.6 KB] || BigSunspot_HMIintensity_stand.HD1080i.00300_searchweb.png (320x180) [21.8 KB] || BigSunspot_HMIintensity_stand.HD1080i.00300_thm.png (80x40) [2.6 KB] || 1920x1080_16x9_30p (1920x1080) [0 Item(s)] || BigSunspot_HMIintensity.HD1080i_p30.mp4 (1920x1080) [29.1 MB] || BigSunspot_HMIintensity.HD1080i_p30.webm (1920x1080) [2.2 MB] || 3840x2160_16x9_30p (3840x2160) [0 Item(s)] || BigSunspot_HMIintensity.UHD2160_p30.mp4 (3840x2160) [171.4 MB] || BigSunspot_HMIintensity.HD1080i_p30.mp4.hwshow [201 bytes] || ", "hits": 60 }, { "id": 4715, "url": "https://svs.gsfc.nasa.gov/4715/", "result_type": "Visualization", "release_date": "2019-06-07T00:00:00-04:00", "title": "Swedish Solar Telescope: Solar Closeups", "description": "Close-up of Active Region 12593 through the 400 nm filter of the Swedish Solar Telescope. SDO/HMI provides the background image. || Sept2016_CHROMIS4000A_stand.HD1080i.00100_print.jpg (1024x576) [200.8 KB] || Sept2016_CHROMIS4000A_stand.HD1080i.00100_searchweb.png (180x320) [136.4 KB] || Sept2016_CHROMIS4000A_stand.HD1080i.00100_thm.png (80x40) [9.1 KB] || SwedishST (1920x1080) [0 Item(s)] || Sept2016_CHROMIS4000A.HD1080i_p30.mp4 (1920x1080) [19.4 MB] || Sept2016_CHROMIS4000A.HD1080i_p30.webm (1920x1080) [1.5 MB] || SwedishST (3840x2160) [0 Item(s)] || Sept2016_CHROMIS4000A.UHD3840_2160p30.mp4 (3840x2160) [50.6 MB] || Sept2016_CHROMIS4000A.HD1080i_p30.mp4.hwshow [199 bytes] || ", "hits": 133 }, { "id": 4623, "url": "https://svs.gsfc.nasa.gov/4623/", "result_type": "Visualization", "release_date": "2018-04-30T10:00:00-04:00", "title": "The Dynamic Solar Magnetic Field with Introduction", "description": "This narrated visualization transitions from a view of the Sun in visible light, to a view in ultraviolet light showing the plasma flowing along solar magnetic structures, to the underlying magnetic field of the solar photosphere, to a model construction of magnetic fieldlines above the photosphere.This video is also available on our YouTube channel. || SolarMagnetism_UHD3840.04000_print.jpg (1024x576) [198.9 KB] || SolarMagnetism_UHD3840.04000_thm.png (80x40) [6.0 KB] || SolarMagnetism_UHD3840.04000_web.png (320x180) [84.1 KB] || SolarMagnetism_ProRes3_HD1080_p30_Narrated.webm (1280x720) [33.9 MB] || SolarMagnetism_ProRes3_HD1080_p30_Narrated.mov (1280x720) [7.4 GB] || SolarMagnetism_ProRes3_UHD2160_p30_Narrated.mov (3840x2160) [12.8 GB] || ", "hits": 129 }, { "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": 83 }, { "id": 4002, "url": "https://svs.gsfc.nasa.gov/4002/", "result_type": "Visualization", "release_date": "2017-08-04T10:00:00-04:00", "title": "AR2665: The Lonely Sunspot of Solar Minimum", "description": "Full-disk view of sunspot group moving across the solar disk, AIA 171 ångstrom band. || July2017_AR2665_AIA171_stand.HD1080i.01000_print.jpg (1024x576) [53.8 KB] || AIA171 (1920x1080) [0 Item(s)] || July2017_AR2665_AIA171.HD1080i_p30.mp4 (1920x1080) [53.5 MB] || July2017_AR2665_AIA171.HD1080i_p30.webm (1920x1080) [8.5 MB] || July2017_AR2665_AIA171_2048p30.mp4 (2048x2048) [264.8 MB] || 171A-Frames (4096x4096) [0 Item(s)] || 171A-Time (4096x4096) [0 Item(s)] || July2017_AR2665_AIA171.HD1080i_p30.mp4.hwshow [200 bytes] || ", "hits": 50 }, { "id": 4551, "url": "https://svs.gsfc.nasa.gov/4551/", "result_type": "Visualization", "release_date": "2017-02-11T10:00:00-05:00", "title": "A Solar Cycle from Solar Dynamics Observatory", "description": "4K x 4K imagery from the SDO/HMI instrument. || SolarCycleHMI.02000_print.jpg (1024x1024) [154.4 KB] || SolarCycleHMI.02000_searchweb.png (320x180) [50.4 KB] || SolarCycleHMI.02000_thm.png (80x40) [3.7 KB] || SolarCycleHMI_1024p30.mp4 (1024x1024) [333.3 MB] || SolarCycleHMI_1024p30.webm (1024x1024) [19.2 MB] || Intensity-Frames (4096x4096) [512.0 KB] || Intensity-Time (4096x4096) [512.0 KB] || ", "hits": 49 }, { "id": 12500, "url": "https://svs.gsfc.nasa.gov/12500/", "result_type": "Produced Video", "release_date": "2017-02-11T10:00:00-05:00", "title": "SDO: Year 7", "description": "The Solar Dynamics Observatory, or SDO, has now captured nearly seven years worth of ultra-high resolution solar footage. This time lapse shows that full run from two of SDO's instruments. The large orange sun is visible light captured by the Helioseismic and Magnetic Imager, or HMI. The smaller golden sun is extreme ultraviolet light from the Atmospheric Imaging Assembly, or AIA, and reveals some of the sun's atmosphere, the corona. Both appear at one frame every 12 hours. SDO's nearly unbroken run is now long enough to watch the rise and fall of the current solar cycle. The graph of solar activity shows the sunspot number, a measurement based on the number of individual spots and the number of sunspot groups. In this case, the line represents a smoothed 26-day average to more clearly show the overall trend.Music: \"Web of Intrigue\" from Killer TracksWatch this video on the NASA Goddard YouTube channel.Complete transcript available. || SDO_Year7_Graph_Still.jpg (3840x2160) [1.2 MB] || 12500_SDO_Year_7_Good_H264_1080.m4v (1920x1080) [239.0 MB] || 12500_SDO_Year_7_1080.mov (1920x1080) [366.0 MB] || 12500_SDO_Year_7_FINAL_appletv.m4v (1280x720) [142.4 MB] || 12500_SDO_Year_7_Compatible.m4v (960x540) [98.1 MB] || 12500_SDO_Year_7_FINAL_appletv_subtitles.m4v (1280x720) [142.5 MB] || 12500_SDO_Year_7_Compatible.webm (960x540) [24.9 MB] || 12500_SDO_Year_7_ProRes_3840x2160_2997.mov (3840x2160) [12.1 GB] || 12500_SDO_Year_7_FINAL_youtube_hq.mov (3840x2160) [6.8 GB] || 12500_SDO_Year_7-Good_H264_4K.m4v (3840x2160) [1.1 GB] || 12500_SDO_Year_7_H264_4K.mov (3840x2160) [474.8 MB] || WMV_12500_SDO_Year_7_FINAL_HD.wmv (3840x2160) [2.2 GB] || 12500_SDO_Year_7_SRT_Captions.en_US.srt [1.4 KB] || 12500_SDO_Year_7_SRT_Captions.en_US.vtt [1.4 KB] || ", "hits": 116 }, { "id": 4269, "url": "https://svs.gsfc.nasa.gov/4269/", "result_type": "Visualization", "release_date": "2016-10-17T10:00:00-04:00", "title": "Various Sun Images for the Hyperwall", "description": "The Solar Dynamics Observatory (SDO) provides ultra high-definition imagery of the Sun in 13 different wavelengths, utilizing two imaging instruments, the Atmospheric Imaging Assembly (AIA) instrument and the Helioseismic and Magnetic Imager (HMI). These images were captured by SDO on December 6, 2010. || ", "hits": 133 }, { "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": 35 }, { "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": 53 }, { "id": 4177, "url": "https://svs.gsfc.nasa.gov/4177/", "result_type": "Visualization", "release_date": "2014-07-23T00:00:00-04:00", "title": "As Seen by STEREO-A: The Carrington-Class CME of 2012", "description": "STEREO-A, at a position along Earth's orbit where it has an unobstructed view of the far side of the Sun, could clearly observe possibly the most powerful coronal mass ejection (CME) of solar cyle 24 on July 23, 2012. The visualizations on this page cover the entire day.We see the flare erupt in the lower right quadrant of the solar disk from a large active region. The material is launched into space in a direction towards STEREO-A. This creates the ring-like 'halo' CME visible in the STEREO-A coronagraph, COR-2 (blue circular image).As the CME expands beyond the field of view of the COR-2 imager, the high energy particles reach STEREO-A, creating the snow-like noise in the image. The particles also strike the HI-2 imager (blue square) brightening the image.The HI-1 imager has had 'bloom removal' enabled and filled with contents of the immediately previous HI-1 image, which creates a linear artifact above and below bright stars and planets. || ", "hits": 261 }, { "id": 4178, "url": "https://svs.gsfc.nasa.gov/4178/", "result_type": "Visualization", "release_date": "2014-07-23T00:00:00-04:00", "title": "As Seen by STEREO-B: The Carrington-Class CME of 2012", "description": "Like SDO, STEREO-B did not have a direct view of the coronal mass ejection (CME) launched by the sun on July 23, 2012. However, the active region involved was very close to the limb of the sun (lower left quadrant) and STEREO-B provided an excellent view of plasma launched in both ultraviolet light and the white-light coronagraph. || ", "hits": 37 }, { "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": 45 }, { "id": 11460, "url": "https://svs.gsfc.nasa.gov/11460/", "result_type": "Produced Video", "release_date": "2014-02-11T12:00:00-05:00", "title": "SDO: Year 4", "description": "The sun is always changing and NASA's Solar Dynamics Observatory is always watching. Launched on Feb. 11, 2010, SDO keeps a 24-hour eye on the entire disk of the sun, with a prime view of the graceful dance of solar material coursing through the sun's atmosphere, the corona. SDO's fourth year in orbit was no exception: NASA is releasing a movie of some of SDO's best sightings of the year, including massive solar explosions and giant sunspot shows. SDO captures images of the sun in 10 different wavelengths, each of which helps highlight a different temperature of solar material. Different temperatures can, in turn, show specific structures on the sun such as solar flares, which are giant explosions of light and x-rays, or coronal loops, which are streams of solar material traveling up and down looping magnetic field lines. The movie shows examples of both, as well as what's called prominence eruptions, when masses of solar material leap off the sun. The movie also shows a sunspot group on the solar surface. This sunspot, a magnetically strong and complex region appearing in mid-January 2014, was one of the largest in nine years. Scientists study these images to better understand the complex electromagnetic system causing the constant movement on the sun, which can ultimately have an effect closer to Earth, too: Flares and another type of solar explosion called coronal mass ejections can sometimes disrupt technology in space. Moreover, studying our closest star is one way of learning about other stars in the galaxy. NASA's Goddard Space Flight Center in Greenbelt, Md. built, operates, and manages the SDO spacecraft for NASA's Science Mission Directorate in Washington, D.C.SDO: Year One here.SDO: Year 2 here.SDO: Year 3 here.Information about the individual clips used in this video is here. || ", "hits": 132 }, { "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": 43 }, { "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": 71 }, { "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": 79 }, { "id": 11211, "url": "https://svs.gsfc.nasa.gov/11211/", "result_type": "Produced Video", "release_date": "2013-02-22T10:00:00-05:00", "title": "SDO Observes Fast-Growing Sunspot", "description": "As magnetic fields on the sun rearrange and realign, dark spots known as sunspots can appear on its surface. Over the course of Feb. 19-20, 2013, scientists watched a giant sunspot form in under 48 hours. It has grown to over six Earth diameters across but its full extent is hard to judge since the spot lies on a sphere not a flat disk.The spot quickly evolved into what's called a delta region, in which the lighter areas around the sunspot, the penumbra, exhibit magnetic fields that point in the opposite direction of those fields in the center, dark area. This is a fairly unstable configuration that scientists know can lead to eruptions of radiation on the sun called solar flares. || ", "hits": 76 }, { "id": 4037, "url": "https://svs.gsfc.nasa.gov/4037/", "result_type": "Visualization", "release_date": "2013-02-11T10:00:00-05:00", "title": "Sunspot Growth in June 2012", "description": "Groups of sunspots grow and die over a matter of days. This is a movie built from images taken by the SDO/HMI instrument over the course of 13 days during the rise of solar cycle 24. || ", "hits": 34 }, { "id": 11203, "url": "https://svs.gsfc.nasa.gov/11203/", "result_type": "Produced Video", "release_date": "2013-02-11T10:00:00-05:00", "title": "SDO: Year 3", "description": "On Feb. 11, 2010, NASA launched an unprecedented solar observatory into space. The Solar Dynamics Observatory (SDO) flew up on an Atlas V rocket, carrying instruments that scientists hoped would revolutionize observations of the sun. If all went according to plan, SDO would provide incredibly high-resolution data of the entire solar disk almost as quickly as once a second. When the science team released its first images in April of 2010, SDO's data exceeded everyone's hopes and expectations, providing stunningly detailed views of the sun. In the three years since then, SDO's images have continued to show breathtaking pictures and movies of eruptive events on the sun. Such imagery is more than just pretty, they are the very data that scientists study. By highlighting different wavelengths of light, scientists can track how material on the sun moves. Such movement, in turn, holds clues as to what causes these giant explosions, which, when Earth-directed, can disrupt technology in space. SDO is the first mission in a NASA's Living With a Star program, the goal of which is to develop the scientific understanding necessary to address those aspects of the sun-Earth system that directly affect our lives and society. NASA's Goddard Space Flight Center in Greenbelt, Md. built, operates, and manages the SDO spacecraft for NASA's Science Mission Directorate in Washington, D.C.SDO: Year One here.SDO: Year 2 here.Information about the individual clips used in this video is here.Watch this video on YouTube. || ", "hits": 135 }, { "id": 3988, "url": "https://svs.gsfc.nasa.gov/3988/", "result_type": "Visualization", "release_date": "2012-11-20T09:00:00-05:00", "title": "The Active Sun from SDO: HMI Intensity", "description": "The Solar Dynamics Observatory (SDO) observes the Sun with many different instruments, in many different wavelengths of light. Many of these capabilities are not possible for ground-based observatories - hence the need for a space-based observing platform.The Helioseismic Magnetic Imager (HMI) aboard the Solar Dynamics Observatory takes a series of images every 45 seconds in a very narrow range of wavelengths in visible light of the solar photosphere. The wavelengths correspond to a region around the 6173 Ångstroms (617.3 nanometers) spectral line of neutral iron (Fe I). From this series of images, it constructs a set of images which extract other characteristics of the photosphere. For this dataset, it shows the solar photosphere in visible light.This visualization is one of a set of visualizations (others linked below) covering the same time span of 17 hours over the full wavelength range of the mission. They are setup to play synchronously on a Hyperwall, or can be run individually.The images are sampled every 36 seconds, 1/3 of the standard time-cadence for SDO. This visualization is useful for illustrating how different solar phenomena, such as sunspots and active regions, look very different in different wavelengths of light. These differences enable scientists to study them more completely, with an eventual goal of improving Space Weather forecasting. || ", "hits": 173 }, { "id": 4008, "url": "https://svs.gsfc.nasa.gov/4008/", "result_type": "Visualization", "release_date": "2012-11-20T09:00:00-05:00", "title": "SDO Jewelbox: The Many Eyes of SDO", "description": "5x3 Layout view. This version has the imagery organized in order of increasing wavelength, from upper left to lower right for AIA. The HMI products occupy the bottom row. || SDOJewelbox_5x3.0100.jpg (2400x810) [317.7 KB] || SDOJewelbox_5x3.0100_web.png (320x108) [28.9 KB] || SDOJewelbox_5x3.0100_thm.png (80x40) [3.7 KB] || SDOJewelbox_5x3.0100_searchweb.png (320x180) [29.2 KB] || SDOJewelbox_5x3.webmhd.webm (960x540) [3.3 MB] || SDOJewelbox_5x3.mov (2400x810) [91.5 MB] || SDOJewelbox_5x3.mp4 (2400x810) [91.5 MB] || 2400x810_80x27_30p (2400x810) [0 Item(s)] || ", "hits": 117 }, { "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": 34 }, { "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": 78 }, { "id": 3941, "url": "https://svs.gsfc.nasa.gov/3941/", "result_type": "Visualization", "release_date": "2012-06-11T14:00:00-04:00", "title": "Venus Transit 2012 Composited Visuals", "description": "These visualizations were generated by compositing the small field-of-view, high-cadence closeups of Venus with the full-disk, low-cadence imagery from Solar Dynamics Observatory (SDO). Two different instruments are used: the Helioseismic and Magnetic Imager (HMI) which sees light in the visible range, and the Atmospheric Imaging Assembly (AIA) which sees light in several wavelengths in the ultraviolet range. To find out more information about these instruments, check out The Atmospheric Imaging Assembly Tutorial.Some artifacts may be visible from the compositing, but you have to look pretty closely to see them.The color table threshold was raised for these images, reducing the amount of noise visible in the images. Note: There is an interesting artifact worthy of mention and clarification, and that is as Venus crosses the solar limb, the limb appears to be visible through the planet in some of the imagers (most notably the ultraviolet channels). Discussion with the scientists who built the imagers suggest this might be 'crosstalk' between the readouts of the four CCD panels that make up a complete image. It is an artifact of the imaging system. || ", "hits": 80 }, { "id": 10996, "url": "https://svs.gsfc.nasa.gov/10996/", "result_type": "Produced Video", "release_date": "2012-06-05T00:00:00-04:00", "title": "SDO's Ultra-high Definition View of 2012 Venus Transit", "description": "Launched on Feb. 11, 2010, the Solar Dynamics Observatory, or SDO, is the most advanced spacecraft ever designed to study the sun. During its five-year mission, it will examine the sun's atmosphere, magnetic field and also provide a better understanding of the role the sun plays in Earth's atmospheric chemistry and climate. SDO provides images with resolution 8 times better than high-definition television and returns more than a terabyte of data each day.On June 5 2012, SDO collected images of the rarest predictable solar event—the transit of Venus across the face of the sun. This event lasted approximately 6 hours and happens in pairs eight years apart, which are separated from each other by 105 or 121 years. The last transit was in 2004 and the next will not happen until 2117.The videos and images displayed here are constructed from several wavelengths of extreme ultraviolet light and a portion of the visible spectrum. The red colored sun is the 304 angstrom ultraviolet, the golden colored sun is 171 angstrom, the magenta sun is 1700 angstrom, and the orange sun is filtered visible light. 304 and 171 show the atmosphere of the sun, which does not appear in the visible part of the spectrum. || ", "hits": 369 }, { "id": 3933, "url": "https://svs.gsfc.nasa.gov/3933/", "result_type": "Visualization", "release_date": "2012-03-31T00:00:00-04:00", "title": "Sunspots on the Move: August 22, 2011", "description": "SDO/HMI movie of sunspots evolving across the solar disk. || HMI_IcChangingSpots.00300.jpg (4096x4096) [3.3 MB] || HMI_IcChangingSpots.00300_web.png (320x320) [89.7 KB] || HMI_IcChangingSpots.00300_thm.png (80x40) [3.8 KB] || HMI_IcChangingSpots.00300_searchweb.png (320x180) [57.8 KB] || HMI_Ic_ChangingSpots_1Kx1K.mov (1024x1024) [28.6 MB] || HMI_Ic_ChangingSpots_4Kx4K.webmhd.webm (960x540) [3.0 MB] || HMI_Ic_ChangingSpots_2Kx2K.mov (2048x2048) [168.7 MB] || 4096x4096_1x1_30p (4096x4096) [0 Item(s)] || HMI_Ic_ChangingSpots_4Kx4K.mov (4096x4096) [17.8 GB] || ", "hits": 38 }, { "id": 3897, "url": "https://svs.gsfc.nasa.gov/3897/", "result_type": "Visualization", "release_date": "2012-01-27T00:00:00-05:00", "title": "Growing Sunspots - A Full Disk View: February 2011", "description": "Here is a leisurely view of SDO/HMI data, sampled every hour, covering two weeks in the middle of February 2011. While the solar disk starts out featureless, eventually small groups of sunspots (the darker regions) emerge, grow, and then rotate out of view.For a closeup view of of one of these sunspot groups, see animation 3898, Growing Sunspots - Tracking Closeup: February 2011 || ", "hits": 68 }, { "id": 3898, "url": "https://svs.gsfc.nasa.gov/3898/", "result_type": "Visualization", "release_date": "2012-01-27T00:00:00-05:00", "title": "Growing Sunspots - Tracking Closeup: February 2011", "description": "This visualization tracks the emergence and evolution of a sunspot group as seen by SDO/HMI starting in early February 2011 and continuing for two weeks. Images are sampled one hour apart.In this version, the camera tracks the movement of the solar rotation.At this scale, a 'shimmer' of the solar surface is visible, created by the turnover of convection cells. A higher-resolution view of these convection cells can be seen in Hinode imagery (see entry #3412, Hinode's High-resolution view of solar granulation).For a full-disk view of the Sun, covering the same time frame, see entry #3897, Growing Sunspots - A Full Disk View: February 2011. || ", "hits": 39 }, { "id": 10748, "url": "https://svs.gsfc.nasa.gov/10748/", "result_type": "Produced Video", "release_date": "2011-04-21T09:00:00-04:00", "title": "SDO: Year One", "description": "April 21, 2011 marks the one-year anniversary of the Solar Dynamics Observatory (SDO) First Light press conference, where NASA revealed the first images taken by the spacecraft.In the last year, the sun has gone from its quietest period in years to the activity marking the beginning of solar cycle 24. SDO has captured every moment with a level of detail never-before possible. The mission has returned unprecedented images of solar flares, eruptions of prominences, and the early stages of coronal mass ejections (CMEs). In this video are some of the most beautiful, interesting, and mesmerizing events seen by SDO during its first year.In the order they appear in the video the events are:1. Prominence Eruption from AIA in 304 Ångstroms on March 30, 20102. Cusp Flow from AIA in 171 Ångstroms on February 14, 20113. Prominence Eruption from AIA in 304 Ångstroms on February 25, 20114. Cusp Flow from AIA in 304 Ångstroms on February 14, 20115. Merging Sunspots from HMI in Continuum on October 24-28, 20106. Prominence Eruption and active region from AIA in 304 Ångstroms on April 30, 20107. Solar activity and plasma loops from AIA in 171 Ångstroms on March 4-8, 20118. Flowing plasma from AIA in 304 Ångstroms on April 19, 20109. Active regions from HMI in Magnetogram on March 10, 201110. Filament eruption from AIA in 304 Ångstroms on December 6, 201011. CME start from AIA in 211 Ångstroms on March 8, 201112. X2 flare from AIA in 304 Ångstroms on February 15, 2011 || ", "hits": 59 }, { "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": 57 }, { "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": 28 }, { "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": 46 }, { "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": 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": 27 }, { "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": 26 }, { "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": 58 }, { "id": 3405, "url": "https://svs.gsfc.nasa.gov/3405/", "result_type": "Visualization", "release_date": "2007-03-01T00:00:00-05:00", "title": "STEREO Panoramic View", "description": "The STEREO mission presents a new view of the space between the Earth and the Sun.This view from the STEREO-A satellite, demonstrates the broad range of sky coverage by the five cameras of the SECCHI instrument. || ", "hits": 58 }, { "id": 3159, "url": "https://svs.gsfc.nasa.gov/3159/", "result_type": "Visualization", "release_date": "2005-05-24T12:00:00-04:00", "title": "SOHO/LASCO View of January 2005 Solar Events", "description": "The January 20 flare began just before 2 a.m. ET. A storm of energetic protons impacted Earth just 15 minutes later. These views of the flare are from the Solar and Heliospheric Observatory (SOHO). The proton storm near Earth causes `snow' in the images, obscuring the Sun as radiation swamps the cameras. The structure at the 1:30 position in the SOHO/LASCO/C3 data is the occulting disk pylon. || ", "hits": 40 }, { "id": 2961, "url": "https://svs.gsfc.nasa.gov/2961/", "result_type": "Visualization", "release_date": "2004-07-08T12:00:00-04:00", "title": "Halloween Solar Storms from SOHO/EIT and SOHO/LASCO", "description": "This movie is a combination of SOHO/EIT at 195 angstroms as well as the LASCO/C2 and C3 cameras. At this scale we can see the flashes from solar flares in SOHO/EIT (green) and the subsequent coronal mass ejections in SOHO/LASCO/C2 (red) and SOHO/LASCO/C3 (blue). This movie is synchronized to play with animation IDs 2960 and 2959. For more information on how X-ray solar flares are classified (B, C, M, X), visit SpaceWeather.com. || ", "hits": 37 }, { "id": 2964, "url": "https://svs.gsfc.nasa.gov/2964/", "result_type": "Visualization", "release_date": "2004-07-08T12:00:00-04:00", "title": "IMAGE Views of the Aurora from Space", "description": "The IMAGE spacecraft observed intense auroral displays in the Fall of 2003 as the material from the coronal mass ejection swept past the Earth. The pressure against the Earth's magnetosphere caused it to dump more electrons into the upper atmosphere, creating auroral displays, as we see here over the South Pole. This is a view of the IMAGE data reprojected onto a model of the Earth. || ", "hits": 37 }, { "id": 2936, "url": "https://svs.gsfc.nasa.gov/2936/", "result_type": "Visualization", "release_date": "2004-05-23T12:00:00-04:00", "title": "The fastest CME of Cycle 23 overtakes another fast CME", "description": "On November 4, 2003, the Sun produced its fastest coronal mass ejection (CME) for cycle 23 out of the active region 0486 located near the southwest limb of the Sun. The CME was expelled with a speed of approximately 2700 km/s. At the time of the launch of this CME, there was another ejection in progress from the same region. The previous ejection started about 7 hours earlier with a speed of about 1000 km/s. The fastest CME overtook the previous one within 2 hours and produced a spectacular radio radiation detected by the Wind, Ulysses and Cassini spacecraft. The movie shows the radio emission and the two interacting CMEs as observed by the SOHO spacecraft. || ", "hits": 52 }, { "id": 2764, "url": "https://svs.gsfc.nasa.gov/2764/", "result_type": "Visualization", "release_date": "2003-07-09T12:00:00-04:00", "title": "High Resolution Solar Views From VAULT", "description": "This movie illustrates the VAULT camera pointings in relation to the rest of the Sun and views from other instruments. || ", "hits": 26 }, { "id": 2765, "url": "https://svs.gsfc.nasa.gov/2765/", "result_type": "Visualization", "release_date": "2003-07-09T12:00:00-04:00", "title": "Hi-resolution Solar Views from VAULT: Active Region", "description": "This movie presents the VAULT imagery in the context of simultaneous multi-mission observations. We zoom-in to a subset of the image which focuses on an active solar region which shows plumes of hot gases rising above the solar surface. || ", "hits": 20 }, { "id": 2766, "url": "https://svs.gsfc.nasa.gov/2766/", "result_type": "Visualization", "release_date": "2003-07-09T12:00:00-04:00", "title": "Hi-resolution Solar Views from VAULT: Quiet Region", "description": "This movie presents the VAULT imagery in the context of simultaneous multi-mission observations. We zoom-in to a subset of the image which focuses on a relatively calm solar region which still reveals a great deal of activity. || ", "hits": 15 }, { "id": 2509, "url": "https://svs.gsfc.nasa.gov/2509/", "result_type": "Visualization", "release_date": "2003-01-31T12:00:00-05:00", "title": "A Multi-Mission View of the AR9906 Solar Flare with Instrument Labels", "description": "Here's a view of the Sun, from the point of view of a fleet of Sun-observing spacecraft - SOHO, TRACE, and RHESSI. The time scales of the data samples in this visualization range from six hours to as short as 12 seconds and the display rate varies throughout the movie. The region and event of interest is the solar flare over solar active region AR9906 on April 21, 2002. In this visualization, the instrument names appear in a color roughly matching the color used for the data, and black corresponds to no (current) instrument coverage. || ", "hits": 13 }, { "id": 2511, "url": "https://svs.gsfc.nasa.gov/2511/", "result_type": "Visualization", "release_date": "2003-01-31T12:00:00-05:00", "title": "A Multi-Mission View of the AR9906 Solar Flare without Instrument Labels", "description": "Here's a view of the Sun, from the point of view of a fleet of Sun-observing spacecraft - SOHO, TRACE, and RHESSI. The time scales of the data samples in this visualization range from 6 hours to as short as 12 seconds and the display rate varies throughout the movie. The region and event of interest is the solar flare over solar active region AR9906 on April 21, 2002. In this visualization, black corresponds to no (current) instrument coverage (there used to be a LASCO C1 camera inside the ring of LASCO C2, but that instrument didn't recover after SOHO was temporarily 'lost' in 1998). || ", "hits": 17 }, { "id": 2553, "url": "https://svs.gsfc.nasa.gov/2553/", "result_type": "Visualization", "release_date": "2003-01-31T12:00:00-05:00", "title": "A Multi-Mission View of the AR9906 Solar Flare with Alternate Instrument Labels", "description": "Here's a view of the Sun, from the point of view of a fleet of Sun-observing spacecraft - SOHO, TRACE, and RHESSI. The time scales of the data samples in this visualization range from 6 hours to as short as 12 seconds and the display rate varies throughout the movie. The region and event of interest is the solar flare over solar active region AR9906 on April 21, 2002. In this visualization, black corresponds to no (current) instrument coverage (there used to be a LASCO C1 camera inside the ring of LASCO C2, but that instrument didn't recover after SOHO was temporarily 'lost' in 1998). || ", "hits": 27 } ] }