{ "count": 114, "next": "https://svs.gsfc.nasa.gov/api/search/?keywords=SOHO&limit=100&offset=100", "previous": null, "results": [ { "id": 5443, "url": "https://svs.gsfc.nasa.gov/5443/", "result_type": "Visualization", "release_date": "2024-12-17T00:00:00-05:00", "title": "Heliophysics Sentinels 2024", "description": "There have been some changes since the 2022 Heliophysics Fleet. AIM and ICON have been decommissioned while two other instruments have been added. AWE is an instrument mounted on the ISS, and RAD is a particle detector on the Curiosity Mars rover. As of Winter 2024, here's a tour of the NASA Heliophysics fleet from the near-Earth satellites out to the Voyagers beyond the heliopause. || ", "hits": 54 }, { "id": 14552, "url": "https://svs.gsfc.nasa.gov/14552/", "result_type": "Produced Video", "release_date": "2024-03-27T10:00:00-04:00", "title": "Volunteers Help ESA & NASA Mission to Discover 5,000 Comets", "description": "The Solar and Heliospheric Observatory (SOHO), a joint mission of ESA (European Space Agency) and NASA, has discovered its 5,000th comet, thanks to the help of volunteer comet hunters participating in the NASA-funded Sungrazer Project.The sungrazing comet was spotted in SOHO images on March 25, 2024, by Hanjie Tan in the Czech Republic, who has participated in the Sungrazer Project since he was 13 years old. The comet is small and has a short orbital period around the Sun. It belongs to the “Marsden group” of comets, which are thought to be related to the larger comet 96P/Machholz. The group is named after the late scientist Brian Marsden, who first recognized the group using SOHO observations.To learn more about the discovery and SOHO, visit: https://science.nasa.gov/science-research/heliophysics/esa-nasa-solar-observatory-discovers-its-5000th-comet/Since the early 2000s, the Sungrazer Project has allowed anyone with a computer to search for comets in images taken by the SOHO spacecraft.To learn more about the Sungrazer Project, visit: https://science.nasa.gov/citizen-science/the-sungrazer-project/ || ", "hits": 60 }, { "id": 5136, "url": "https://svs.gsfc.nasa.gov/5136/", "result_type": "Visualization", "release_date": "2023-08-22T00:00:00-04:00", "title": "STEREO-A Returns by Earth", "description": "The Solar Terrestrial Relations Observatory (STEREO) mission was launched on October 25, 2006, with the purpose of tracing the flow of energy and matter from the Sun to Earth. The STEREO mission began with two spacecraft: STEREO-A and STEREO-B. Each was launched into Sun-orbiting trajectories - STEREO-A moving ahead of Earth, and STEREO-B moving behind Earth (STEREO's Routes to Solar Orbits). In mid-August 2023, the still-operational STEREO-A (STEREO-B went offline in October 2014) will pass Earth for the first time since its launch 17 years ago. Like race cars driving different speeds around a circular track, STEREO-A is traveling slightly faster than Earth around the Sun. After launch, STEREO-A pulled ahead of Earth and extended its lead a little bit more with each orbit. Now, STEREO-A’s lead is so great that it is catching up to Earth from behind and is about to “lap” Earth, having completed 18 circuits around the Sun while Earth completed just 17. || ", "hits": 148 }, { "id": 4898, "url": "https://svs.gsfc.nasa.gov/4898/", "result_type": "Visualization", "release_date": "2022-11-23T00:00:00-05:00", "title": "Heliophysics Sentinels 2022", "description": "There has been one significant change since the 2020 Heliophysics Fleet. SET has been decommissioned. As of Fall 2022, here's a tour of the NASA Heliophysics fleet from the near-Earth satellites out to the Voyagers beyond the heliopause.Excepting the Voyager missions, the satellite orbits are color coded for their observing program:Magenta: TIM (Thermosphere, Ionosphere, Mesosphere) observationsYellow: solar observations and imageryCyan: Geospace and magnetosphereViolet: Heliospheric observations || ", "hits": 41 }, { "id": 4970, "url": "https://svs.gsfc.nasa.gov/4970/", "result_type": "Visualization", "release_date": "2022-02-25T10:00:00-05:00", "title": "The Many Eyes on the Parker Solar Probe Perihelion (February 2022)", "description": "This visualization opens with a top-down view, then transtions to an oblique view of the inner solar system with the various solar-observing missions conducting coordinated observations of the plasma environment. This version displays the imaging instrument camera frustums and solar magnetic field alignments - the 'glyph' version. A version with just the orbits, no 'glyphs' is available in the [Download Options] menu. || SolarSynergiesPlus.Encounter2022FebTop2Side.HAE.AU.glyphs_CRTT.HD1080.01300_print.jpg (1024x576) [123.3 KB] || SolarSynergiesPlus.Encounter2022FebTop2Side.HAE.AU.glyphs_CRTT.HD1080.01300_searchweb.png (320x180) [78.9 KB] || SolarSynergiesPlus.Encounter2022FebTop2Side.HAE.AU.glyphs_CRTT.HD1080.01300_thm.png (80x40) [5.2 KB] || Encounter2022FebTop2Side (1920x1080) [0 Item(s)] || Encounter2022FebTop2Side.glyphs (1920x1080) [0 Item(s)] || SolarSynergiesPlus.Encounter2022FebTop2Side.HD1080_p30.mp4 (1920x1080) [47.0 MB] || SolarSynergiesPlus.Encounter2022FebTop2Side.glyphs.HD1080_p30.mp4 (1920x1080) [60.7 MB] || SolarSynergiesPlus.Encounter2022FebTop2Side.HD1080_p30.webm (1920x1080) [9.7 MB] || Encounter2022FebTop2Side (3840x2160) [0 Item(s)] || Encounter2022FebTop2Side.glyphs (3840x2160) [0 Item(s)] || SolarSynergiesPlus.Encounter2022FebTop2Side.UHD2160_p30.mp4 (3840x2160) [143.6 MB] || SolarSynergiesPlus.Encounter2022FebTop2Side.glyphs.UHD2160_p30.mp4 (3840x2160) [176.4 MB] || SolarSynergiesPlus.Encounter2022FebTop2Side.HD1080_p30.mp4.hwshow [220 bytes] || ", "hits": 94 }, { "id": 4887, "url": "https://svs.gsfc.nasa.gov/4887/", "result_type": "Visualization", "release_date": "2021-03-01T10:00:00-05:00", "title": "Heliophysics Sentinels 2020 (Forecast Version)", "description": "In addition to the NASA missions used in research for space weather (see 2020 Heliophysics Fleet) there are additional missions operated by NOAA used for space weather forecasting. As of spring 2020, here's a tour of the NASA and NOAA Heliophysics fleets from the near-Earth satellites out to the inner solar system.The satellite orbits are color coded for their observing program:Magenta: TIM (Thermosphere, Ionosphere, Mesosphere) observationsYellow: solar observations and imageryCyan: Geospace and magnetosphereViolet: Heliospheric observations || ", "hits": 30 }, { "id": 13775, "url": "https://svs.gsfc.nasa.gov/13775/", "result_type": "Produced Video", "release_date": "2020-12-02T11:00:00-05:00", "title": "25 Years of Sun from ESA/NASA's SOHO", "description": "December 2, 1995 marks the 25th anniversary of the Solar and Heliospheric Observatory, or SOHO — a joint mission of the European Space Agency and NASA. Since its launch on that date, the mission has kept watch on the Sun. || ", "hits": 87 }, { "id": 4822, "url": "https://svs.gsfc.nasa.gov/4822/", "result_type": "Visualization", "release_date": "2020-09-15T10:00:00-04:00", "title": "Heliophysics Sentinels 2020", "description": "There have been few changes since the 2018 Heliophysics Fleet. Van Allen Probes and SORCE have been decommissioned, while Solar Orbiter, ICON and SET have been added. As of spring 2020, here's a tour of the NASA Heliophysics fleet from the near-Earth satellites out to the Voyagers beyond the heliopause.Excepting the Voyager missions, the satellite orbits are color coded for their observing program:Magenta: TIM (Thermosphere, Ionosphere, Mesosphere) observationsYellow: solar observations and imageryCyan: Geospace and magnetosphereViolet: Heliospheric observations || ", "hits": 36 }, { "id": 13661, "url": "https://svs.gsfc.nasa.gov/13661/", "result_type": "Produced Video", "release_date": "2020-07-10T09:50:00-04:00", "title": "NASA Missions Spot Comet NEOWISE", "description": "These images from ESA and NASA’s Solar and Heliospheric Observatory show comet NEOWISE as it approached the Sun in late June 2020. The instrument that produced this data is a coronagraph, which uses a solid disk to block out the Sun’s bright face, revealing the comparatively outer atmosphere, the corona, along with objects like comet NEOWISE. Credit: ESA/NASA/SOHO || wide.00250_print.jpg (1024x576) [164.4 KB] || wide.mp4 (3840x2160) [72.2 MB] || wide.webm (3840x2160) [6.2 MB] || ", "hits": 93 }, { "id": 13623, "url": "https://svs.gsfc.nasa.gov/13623/", "result_type": "Produced Video", "release_date": "2020-06-17T10:00:00-04:00", "title": "Four of Our Favorite SOHO-discovered Comets", "description": "Karl Battams, manager of NASA's citizen science Sungrazer Project, talks about his four favorite comets that SOHO has observed.Music: \"Inducing Waves\" from Universal Production MusicWatch this video on the NASA Goddard YouTube channel.Complete transcript available. || 13623_SOHO4FavoriteComets_ProRes_1920x1080_2997.01026_print.jpg (1024x576) [155.4 KB] || 13623_SOHO4FavoriteComets_ProRes_1920x1080_2997.01026_searchweb.png (320x180) [72.1 KB] || 13623_SOHO4FavoriteComets_ProRes_1920x1080_2997.01026_thm.png (80x40) [5.3 KB] || 13623_SOHO4FavoriteComets_ProRes_1920x1080_2997.mov (1920x1080) [3.1 GB] || 13623_SOHO4FavoriteComets_1080.mp4 (1920x1080) [245.9 MB] || 13623_SOHO4FavoriteComets_Good_1080.mp4 (1920x1080) [128.8 MB] || 13623_SOHO4FavoriteComets_1080.webm (1920x1080) [27.2 MB] || SOHO_4000Comets_SRT_Captions.en_US.srt [4.8 KB] || SOHO_4000Comets_SRT_Captions.en_US.vtt [4.8 KB] || ", "hits": 35 }, { "id": 13622, "url": "https://svs.gsfc.nasa.gov/13622/", "result_type": "Produced Video", "release_date": "2020-05-19T10:00:00-04:00", "title": "Counting Comets", "description": "Music Credit: Birds in The Rain by Robert GuerrierComplete transcript available.Watch this video on the NASA Goddard YouTube channel. || cometthumb.jpg (1920x1080) [404.7 KB] || cometthumb_print.jpg (1024x576) [192.3 KB] || cometthumb_searchweb.png (320x180) [56.6 KB] || cometthumb_web.png (320x180) [56.6 KB] || cometthumb_thm.png (80x40) [5.1 KB] || 13622.Counting_Comets.Mobile720.mp4 (1280x720) [108.5 MB] || 13622.Counting_Comets.Twitter1080.mp4 (1920x1080) [40.1 MB] || 13622.Counting_CometsFB.mp4 (1920x1080) [215.9 MB] || 13622.Counting_Comets.YouTube1080.mp4 (1920x1080) [284.3 MB] || 13622.Counting_Comets.YouTube1080.webm (1920x1080) [20.2 MB] || Counting_CometsAPR.mov (1920x1080) [4.4 GB] || 13622Comets.en_US.srt [3.6 KB] || 13622Comets.en_US.vtt [3.7 KB] || ", "hits": 95 }, { "id": 13291, "url": "https://svs.gsfc.nasa.gov/13291/", "result_type": "Produced Video", "release_date": "2019-08-23T11:30:00-04:00", "title": "NASA’s New Solar Scope Is Ready For Balloon Flight", "description": "NASA and the Korea Astronomy and Space Science Institute, or KASI, are getting ready to test a new way to see the Sun, high over the New Mexico desert. A pearlescent balloon — large enough to hug a football field — is scheduled to take flight no earlier than Aug. 26, 2019, carrying beneath it a solar scope called BITSE. BITSE is a coronagraph, a kind of telescope that blocks the Sun’s bright face in order to reveal its dimmer atmosphere, called the corona. Short for Balloon-borne Investigation of Temperature and Speed of Electrons in the corona, BITSE seeks to explain how the Sun spits out the solar wind. || ", "hits": 57 }, { "id": 13275, "url": "https://svs.gsfc.nasa.gov/13275/", "result_type": "Produced Video", "release_date": "2019-08-07T11:30:00-04:00", "title": "How NASA Will Protect Astronauts From Space Radiation", "description": "Today, the Apollo-era flares serve as a reminder of the threat of radiation exposure for technology and astronauts in space. Understanding and predicting solar eruptions is crucial for safe space exploration. Almost 50 years since those 1972 storms, the data, technology and resources available to NASA have improved, enabling advancements towards space weather forecasts and astronaut protection — key to NASA’s Artemis program to return astronauts to the Moon.", "hits": 277 }, { "id": 4360, "url": "https://svs.gsfc.nasa.gov/4360/", "result_type": "Visualization", "release_date": "2018-12-10T11:00:00-05:00", "title": "Heliophysics Sentinels 2018", "description": "This movie presents the trajectories of the heliophysics fleet from close to Earth to out beyond the heliopause. || Sentinels2018.Sentinels2Voyager.GSE.AU.clockSlate_EarthTarget.UHD3840.00000_print.jpg (1024x576) [74.5 KB] || Sentinels2018.Sentinels2Voyager.GSE.AU.clockSlate_EarthTarget.UHD3840.00000_searchweb.png (180x320) [65.6 KB] || Sentinels2018.Sentinels2Voyager.GSE.AU.clockSlate_EarthTarget.UHD3840.00000_thm.png (80x40) [5.1 KB] || Sentinels2018.Sentinels2Voyager_1080p30.mp4 (1920x1080) [40.3 MB] || Sentinels2018.Sentinels2Voyager_1080p30.webm (1920x1080) [6.3 MB] || 1920x1080_16x9_30p (1920x1080) [0 Item(s)] || 3840x2160_16x9_30p (3840x2160) [0 Item(s)] || Sentinels2018.Sentinels2Voyager_2160p30.mp4 (3840x2160) [125.7 MB] || Sentinels2018.Sentinels2Voyager_1080p30.mp4.hwshow || ", "hits": 28 }, { "id": 12900, "url": "https://svs.gsfc.nasa.gov/12900/", "result_type": "Produced Video", "release_date": "2018-11-02T10:00:00-04:00", "title": "Insights on Comet Tails Are Blowing in the Solar Wind", "description": "Complete transcript available.Watch this video on the NASA Goddard YouTube channel.Music credit: Game Show Sphere 01 by Anselm Kreuzer || cometthumb.jpg (1920x1080) [773.3 KB] || cometthumb_searchweb.png (320x180) [67.8 KB] || cometthumb_thm.png (80x40) [4.6 KB] || 12900_comet_tailsV7.mov (1920x1080) [4.2 GB] || 12900_comet_tailsV7.mp4 (1920x1080) [158.1 MB] || 12900_comet_tailsV7_lowres.mp4 (1280x720) [41.0 MB] || YOUTUBE_1080_12900_comet_tailsV7_youtube_1080.mp4 (1920x1080) [282.0 MB] || 12900_comet_tailsV7_youtube_hq.mov (1920x1080) [794.5 MB] || 12900_comet_tailsV7_lowres.webm (1280x720) [18.0 MB] || 12900_comet_tailsV7.en_US.srt [2.7 KB] || 12900_comet_tailsV7.en_US.vtt [2.7 KB] || ", "hits": 235 }, { "id": 13011, "url": "https://svs.gsfc.nasa.gov/13011/", "result_type": "Produced Video", "release_date": "2018-07-25T00:00:00-04:00", "title": "Sounds of the Sun", "description": "An illustration of a sunspot inspired by imagery from NASA's Solar Dynamics Observatory (SDO). || sunspot.gif (1280x720) [1.5 MB] || sunspot_searchweb.png (320x180) [95.7 KB] || ", "hits": 202 }, { "id": 12890, "url": "https://svs.gsfc.nasa.gov/12890/", "result_type": "Produced Video", "release_date": "2018-03-09T10:00:00-05:00", "title": "Solar Highlights of 2018", "description": "3 NASA Satellite Recreate Solar Eruption in 3-DUsing data from three different satellites, scientists have developed new models that recreate, in 3-D, CMEs and shocks, separately. This movie illustrates the recreation of a CME and shock that erupted from the Sun on March 7, 2011. The pink lines show the CME structure and the yellow lines show the structure of the shock - a side effect of the CME that can spark space weather events around Earth.Scientists: Ryun Kwon (George Mason University), Angelos Vourlidas (The Johns Hopkins University Applied Physics Laboratory)Image credits: NASA’s Goddard Space Flight Center/GMU/APL/Joy NgWatch this video on the NASA.gov Video YouTube channel.Find this feature on NASA.gov. || 3DCME.00001_print.jpg (1024x576) [77.7 KB] || 3DCME.00001_searchweb.png (320x180) [52.1 KB] || 3DCME.00001_web.png (320x180) [52.1 KB] || 3DCME.00001_thm.png (80x40) [5.3 KB] || PRORES_B-ROLL_12890_3DCME_prores.mov (1280x720) [218.7 MB] || 3DCME_Prores.mov (1920x1080) [416.9 MB] || 3DCME.mp4 (1920x1080) [44.6 MB] || 12890_3DCME_appletv.m4v (1280x720) [24.5 MB] || NASA_TV_12890_3DCME.mpeg (1280x720) [102.5 MB] || LARGE_MP4_12890_3DCME_large.mp4 (1920x1080) [31.2 MB] || 3DCME.webm (1920x1080) [3.1 MB] || GSFC_20180309_CME_m12890_3DCME.en_US.vtt [64 bytes] || 12890_3DCME_ipod_sm.mp4 (320x240) [7.2 MB] || ", "hits": 42 }, { "id": 4589, "url": "https://svs.gsfc.nasa.gov/4589/", "result_type": "Visualization", "release_date": "2017-10-25T10:00:00-04:00", "title": "Heliophysics Sentinels 2017", "description": "This visualization starts from near Earth and the Earth orbiting satellite fleet out to the Moon, then past the Sun-Earth Lagrange point 1 to out beyond the heliopause. This is the long-play version. || Sentinels2017.Sentinels2Voyager.GSE.AU.clockSlate_EarthTarget.UHD3840.00000_print.jpg (1024x576) [136.1 KB] || Sentinels2017.Sentinels2Voyager.GSE.AU.clockSlate_EarthTarget.UHD3840.00000_searchweb.png (180x320) [84.6 KB] || Sentinels2017.Sentinels2Voyager.GSE.AU.clockSlate_EarthTarget.UHD3840.00000_thm.png (80x40) [6.0 KB] || Sentinels2017.Sentinels2Voyager.HD1080i_p30.webm (1920x1080) [12.4 MB] || SlowPlay (1920x1080) [0 Item(s)] || Sentinels2017.Sentinels2Voyager.HD1080i_p30.mp4 (1920x1080) [111.6 MB] || SlowPlay (3840x2160) [0 Item(s)] || Sentinels2017.Sentinels2Voyager_2160p30.mp4 (3840x2160) [336.2 MB] || Sentinels2017.Sentinels2Voyager.HD1080i_p30.mp4.hwshow [209 bytes] || ", "hits": 30 }, { "id": 30893, "url": "https://svs.gsfc.nasa.gov/30893/", "result_type": "Hyperwall Visual", "release_date": "2017-08-31T00:00:00-04:00", "title": "2017 Eclipse Image Collection", "description": "This image is a composite photograph that shows the progression of the total solar eclipse over Madras, Oregon.http://earthobservatory.nasa.gov/NaturalHazards/view.php?id=90796 || eclipsecomposite_pho_lrg.jpg (2231x1487) [541.4 KB] || eclipsecomposite_pho_lrg_searchweb.png (320x180) [47.2 KB] || eclipsecomposite_pho_lrg_thm.png (80x40) [3.3 KB] || 2017-eclipse-images-7.hwshow [293 bytes] || ", "hits": 148 }, { "id": 12698, "url": "https://svs.gsfc.nasa.gov/12698/", "result_type": "Produced Video", "release_date": "2017-08-30T10:00:00-04:00", "title": "What Spacecraft Saw During the 2017 Solar Eclipse", "description": "On Aug. 21, 2017, a solar eclipse passed over North America. People throughout the continent experienced a partial solar eclipse, and a total solar eclipse passed over a narrow swath of land stretching from Oregon to South Carolina, called the path of totality. NASA and its partner’s satellites had a unique vantage point to watch the eclipse. Several Sun-watching satellites were in a position to see the Moon cross in front of the Sun, while many Earth-observing satellites – and NASA’s Lunar Reconnaissance Orbiter, which typically images the Moon’s landscape – captured images of the Moon’s shadow on Earth’s surface. See more and download content at https://go.nasa.gov/2x7b8kf || ", "hits": 53 }, { "id": 12693, "url": "https://svs.gsfc.nasa.gov/12693/", "result_type": "Produced Video", "release_date": "2017-08-17T11:00:00-04:00", "title": "A Total Solar Eclipse Revealed Solar Storms 100 Years Before Satellites", "description": "Eclipses set the stage for historic science. NASA is taking advantage of the Aug. 21, 2017 eclipse by funding 11 ground-based scientific studies. As our scientists prepare their experiments for next week, we're looking back to an historic 1860 total solar eclipse, which many think gave humanity our first glimpse of solar storms — called coronal mass ejections — 100 years before scientists first understood what they were.Scientists observed these eruptions in the 1970s during the beginning of the modern satellite era, when satellites in space were able to capture thousands of images of solar activity that had never been seen before. But in hindsight, scientists realized their satellite images might not be the first record of these solar storms. Hand-drawn records of an 1860 total solar eclipse bore surprising resemblance to these groundbreaking satellite images.Eclipse archive imagery from: http://mlso.hao.ucar.edu/hao-eclipse-archive.php || ", "hits": 102 }, { "id": 30822, "url": "https://svs.gsfc.nasa.gov/30822/", "result_type": "Infographic", "release_date": "2016-12-06T00:00:00-05:00", "title": "NASA's Heliophysics Fleet", "description": "The current Heliophysics fleet || hpd-fleet-chart-jan-2024_print.jpg (1024x576) [180.0 KB] || hpd-fleet-chart-jan-2024.png (3840x2160) [7.3 MB] || hpd-fleet-chart-jan-2024_searchweb.png (320x180) [91.3 KB] || hpd-fleet-chart-jan-2024_thm.png (80x40) [7.2 KB] || nasas-fleets-by-division-helio-jewel.hwshow [228 bytes] ||", "hits": 53 }, { "id": 12052, "url": "https://svs.gsfc.nasa.gov/12052/", "result_type": "Produced Video", "release_date": "2015-12-01T10:00:00-05:00", "title": "SOHO Celebrates 20 Years of Space-based Science", "description": "Dr. Joe Gurman of NASA's Goddard Space Flight Center provides commentary on selected shots from SOHO's 20 years in space.Watch this video on YouTube || SOHO20thumb.jpg (1280x720) [108.1 KB] || SOHO20thumb_searchweb.png (320x180) [119.7 KB] || SOHO20thumb_thm.png (80x40) [19.1 KB] || APPLE_TV_12952_SOHO_20th_anniversary_ws_appletv.m4v (1280x720) [199.6 MB] || YOUTUBE_HQ_12952_SOHO_20th_anniversary_ws_youtube_hq.mov (1920x1080) [2.5 GB] || 12952_SOHO_20th_anniversary_ws-H264_Best_1920x1080_59.94.mov (1920x1080) [4.0 GB] || YOUTUBE_HQ_12952_SOHO_20th_anniversary_ws_youtube_hq.webm (1920x1080) [45.1 MB] || SOHO20.en_US.srt [7.6 KB] || 12952_SOHO_20th_anniversary_ws.key [200.0 MB] || 12952_SOHO_20th_anniversary_ws.pptx [199.8 MB] || 12952_SOHO_20th_anniversary_ws_lowres.mp4 (480x272) [52.9 MB] || NASA_PODCAST_12952_SOHO_20th_anniversary_ws_ipod_sm.mp4 (320x240) [67.5 MB] || ", "hits": 54 }, { "id": 12071, "url": "https://svs.gsfc.nasa.gov/12071/", "result_type": "Produced Video", "release_date": "2015-11-30T17:00:00-05:00", "title": "SOHO Anniversary Live Shot Page", "description": "B-roll for SOHO live shot || SOHO_Broadcast_broll_youtube_print.jpg (1024x576) [98.3 KB] || SOHO_Broadcast_broll_youtube_searchweb.png (320x180) [63.4 KB] || SOHO_Broadcast_broll_youtube_thm.png (80x40) [4.9 KB] || SOHO_Broadcast_broll_prores.mov (1280x720) [2.2 GB] || SOHO_Broadcast_broll_youtube.mp4 (1280x720) [250.3 MB] || SOHO_Broadcast_broll_youtube.webm (1280x720) [15.2 MB] || ", "hits": 35 }, { "id": 20230, "url": "https://svs.gsfc.nasa.gov/20230/", "result_type": "Animation", "release_date": "2015-11-30T00:00:00-05:00", "title": "Solar and Heliospheric Observatory (SOHO)", "description": "SOHO Beauty Pass || SOHO_00050_print.jpg (1024x576) [102.8 KB] || SOHO_00050_searchweb.png (320x180) [63.8 KB] || SOHO_00050_thm.png (80x40) [4.7 KB] || SOHO_prores.mov (1920x1080) [676.8 MB] || SOHO_h264.mov (1920x1080) [462.6 MB] || 1920x1080_16x9_60p (1920x1080) [64.0 KB] || SOHO_1080p60.mp4 (1920x1080) [15.9 MB] || SOHO_prores.webm (1920x1080) [2.2 MB] || ", "hits": 106 }, { "id": 11975, "url": "https://svs.gsfc.nasa.gov/11975/", "result_type": "Produced Video", "release_date": "2015-09-15T10:00:00-04:00", "title": "3,000 Comets for SOHO", "description": "Karl Battams of the Naval Research Lab talks us through a visualization of the comets that SOHO has witnessed.Watch this video on the NASAexplorer YouTube channel. || sohocometsthumb.jpg (1280x720) [150.9 KB] || sohocometsthumb_print.jpg (1024x576) [157.3 KB] || sohocometsthumb_searchweb.png (320x180) [82.6 KB] || sohocometsthumb_web.png (320x180) [82.6 KB] || sohocometsthumb_thm.png (80x40) [11.5 KB] || G2015-069_3000SOHOcometsV2-H264_Good_1080_29.97.mov (1920x1080) [565.6 MB] || G2015-069_3000SOHOcometsV2-H264_Best_1920x1080_59.94.mov (1920x1080) [3.3 GB] || VX-71391.m4v (1280x720) [134.5 MB] || VX-71391.mov (1920x1080) [2.1 GB] || VX-71391.webm (960x540) [108.0 MB] || 3000SOHOcometsV2.en_US.srt [4.5 KB] || 3000SOHOcometsV2.en_US.vtt [4.5 KB] || VX-71391.mp4 (480x272) [35.9 MB] || ", "hits": 28 }, { "id": 11905, "url": "https://svs.gsfc.nasa.gov/11905/", "result_type": "Produced Video", "release_date": "2015-06-23T12:00:00-04:00", "title": "Space Weather Imagery of June 22 - 23, 2015 Events", "description": "The sun emitted a CME and mid-level solar flare, peaking at 2:23 p.m. EDT, on June 22, 2015. Again on June 25, 2015, a mid-level solar flare peaked at 4:16 a.m. EDT.NASA’s Solar Dynamics Observatory, which watches the sun constantly, captured an image of the event. Solar flares are powerful bursts of radiation. Harmful radiation from a flare cannot pass through Earth's atmosphere to physically affect humans on the ground, however -- when intense enough -- they can disturb the atmosphere in the layer where GPS and communications signals travel. To see how this event may affect Earth, please visit NOAA's Space Weather Prediction Center at http://spaceweather.gov, the U.S. government's official source for space weather forecasts, alerts, watches and warnings. This first flare is classified as an M6.6 flare and the second was M7.9. M-class flares are a tenth the size of the most intense flares, the X-class flares. The number provides more information about its strength. An M2 is twice as intense as an M1, an M3 is three times as intense, etc. || ", "hits": 59 }, { "id": 11811, "url": "https://svs.gsfc.nasa.gov/11811/", "result_type": "Produced Video", "release_date": "2015-03-17T13:15:00-04:00", "title": "SOHO Observes March 14 Coronal Mass Ejection", "description": "The Joint ESA/NASA Solar and Heliospheric Observatory, or SOHO, captured this image series of a coronal mass ejection, or CME, on March 14, 2015. || JHV_movie_created_2015-03-17_19.37.12_print.jpg (1024x576) [73.7 KB] || JHV_movie_created_2015-03-17_19.37.12_searchweb.png (320x180) [48.6 KB] || JHV_movie_created_2015-03-17_19.37.12_web.png (320x180) [48.6 KB] || JHV_movie_created_2015-03-17_19.37.12.webm (1920x1080) [334.4 KB] || JHV_movie_created_2015-03-17_19.37.12.mp4 (1920x1080) [9.0 MB] || ", "hits": 49 }, { "id": 11558, "url": "https://svs.gsfc.nasa.gov/11558/", "result_type": "Produced Video", "release_date": "2014-09-24T10:00:00-04:00", "title": "NASA's Many Views of a Massive CME", "description": "On July 23, 2012, a massive cloud of solar material erupted off the sun's right side, zooming out into space. It soon passed one of NASA's Solar Terrestrial Relations Observatory, or STEREO, spacecraft, which clocked the CME as traveling between 1,800 and 2,200 miles per second as it left the sun. This was the fastest CME ever observed by STEREO. Two other observatories – NASA's Solar Dynamics Observatory and the joint European Space Agency/NASA Solar and Heliospheric Observatory — witnessed the eruption as well. The July 2012 CME didn't move toward Earth, but watching an unusually strong CME like this gives scientists an opportunity to observe how these events originate and travel through space. STEREO's unique viewpoint from the sides of the sun combined with the other two observatories watching from closer to Earth helped scientists create models of the entire July 2012 event. They learned that an earlier, smaller CME helped clear the path for the larger event, thus contributing to its unusual speed. Such data helps advance our understanding of what causes CMEs and improves modeling of similar CMEs that could be Earth-directed. || ", "hits": 149 }, { "id": 11493, "url": "https://svs.gsfc.nasa.gov/11493/", "result_type": "Produced Video", "release_date": "2014-02-25T00:00:00-05:00", "title": "NASA's SDO Provides Images of Significant Solar Flare", "description": "The sun emitted a significant solar flare, peaking at 7:49 p.m. EST on Feb. 24, 2014. NASA's Solar Dynamics Observatory, which keeps a constant watch on the sun, captured images of the event.This flare is classified as an X4.9-class flare. X-class denotes the most intense flares, while the number provides more information about its strength. An X2 is twice as intense as an X1, an X3 is three times as intense, etc. || ", "hits": 76 }, { "id": 30072, "url": "https://svs.gsfc.nasa.gov/30072/", "result_type": "Hyperwall Visual", "release_date": "2013-09-25T00:00:00-04:00", "title": "Heliophysics Fleet Captures Eruption and CME", "description": "On May 1, 2013, NASA's Solar Dynamics Observatory (SDO) watched as an active region (left) of the sun erupted with a huge cloud of solar material—a heated, charged gas called plasma. This eruption, called a coronal mass ejection, or CME, sent the plasma streaming out through the solar system. Viewing the sun in the extreme ultraviolet wavelength of 304 Ångström, SDO provided a beautiful view of the initial arc as it left the solar surface. In addition to the images captured by SDO the CME was also observed by the European Space Agency/NASA Solar and Heliospheric Observatory (SOHO). SOHO houses two overlapping Large Angle Spectrometric Coronagraph (LASCO) telescopes where the bright sun is blocked by a disk so it does not overpower the fainter solar atmosphere. Both LASCO telescopes, named C2 and C3, observed the CME. The LASCO C2 coronagraph shows the region out to about 2.5 million miles, while the LASCO C3 coronagraph expands even farther out to around 13.5 million miles. Both of these instruments show the CME as it expands and becomes fainter on its trip away from the sun. || ", "hits": 33 }, { "id": 11307, "url": "https://svs.gsfc.nasa.gov/11307/", "result_type": "Produced Video", "release_date": "2013-07-16T13:00:00-04:00", "title": "What is a Sungrazing Comet?", "description": "Sungrazing comets are a special class of comets that come very close to the sun at their nearest approach, a point called perihelion. To be considered a sungrazer, a comet needs to get within about 850,000 miles from the sun at perihelion. Many come even closer, even to within a few thousand miles. Being so close to the sun is very hard on comets for many reasons. They are subjected to a lot of solar radiation which boils off their water or other volatiles. The physical push of the radiation and the solar wind also helps form the tails. And as they get closer to the sun, the comets experience extremely strong tidal forces, or gravitational stress. In this hostile environment, many sungrazers do not survive their trip around the sun. Although they don't actually crash into the solar surface, the sun is able to destroy them anyway. Many sungrazing comets follow a similar orbit, called the Kreutz Path, and collectively belong to a population called the Kreutz Group. In fact, close to 85% of the sungrazers seen by the SOHO satellite are on this orbital highway. Scientists think one extremely large sungrazing comet broke up hundreds, or even thousands, of years ago, and the current comets on the Kreutz Path are the leftover fragments of it. As clumps of remnants make their way back around the sun, we experience a sharp increase in sungrazing comets, which appears to be going on now. Comet Lovejoy, which reached perihelion on December 15, 2011 is the best known recent Kreutz-group sungrazer. And so far, it is the only one that NASA's solar-observing fleet has seen survive its trip around the sun. Comet ISON, an upcoming sungrazer with a perihelion of 730,000 miles on November 28, 2013, is not on the Kreutz Path. In fact, ISON's orbit suggests that it may gain enough momentum to escape the solar system entirely, and never return. Before it does so, it will pass within about 40 million miles from Earth on December 26th. Assuming it survives its trip around the sun. || ", "hits": 164 }, { "id": 10785, "url": "https://svs.gsfc.nasa.gov/10785/", "result_type": "Produced Video", "release_date": "2013-05-07T11:00:00-04:00", "title": "NASA's Heliophysics Fleet Captures May 1, 2013 Prominence Eruption and CME", "description": "On May 1, 2013, NASA's Solar Dynamics Observatory (SDO) watched as an active region just around the East limb (left edge) of the sun erupted with a huge cloud of solar material—a heated, charged gas called plasma. This eruption, called a coronal mass ejection, or CME, sent the plasma streaming out through the solar system. Viewing the sun in the extreme ultraviolet wavelength of 304 angstroms, SDO provided a beautiful view of the initial arc as it left the solar surface. Such eruptions soon leave SDO's field of view, but other satellites in NASA's Heliophysics fleet can pick them up, tracking such space weather to determine if they are headed toward Earth or spacecraft near other planets. With advance warning, many space assets can be put into safe mode and protect themselves from the effects of such particle radiation.In addition to the images captured by SDO, the May 1, 2013 CME was also observed by the ESA/NASA Solar and Heliospheric Observatory (SOHO). SOHO houses two overlapping coronagraphs—telescopes where the bright sun is blocked by a disk so it doesn't overpower the fainter solar atmosphere—and they both saw the CME continue outward. The LASCO C2 coronagraph shows the region out to about 2.5 million miles. The LASCO C3 coronagraph expands even farther out to around 13.5 million miles. Both of these instruments show the CME as it expands and becomes fainter on its trip away from the sun.NASA's Solar Terrestrial Relations Observatory (STEREO) Ahead satellite saw the eruption from a very different angle. It, along with its twin STEREO Behind, is orbiting at a similar distance as Earth. STEREO-A orbits slightly faster than Earth and STEREO-B orbits slightly slower. Currently, STEREO-A is more than two-thirds of the way to being directly behind the sun, and has a view of the far side of the sun. From this perspective, the CME came off the right side of the sun. STEREO has an extreme ultraviolet camera similar to SDO's, but it also has coronagraphs like SOHO. As a result, using its two inner coronagraphs, it was able to track the CME from the solar surface out to 6.3 million miles.Working together, such missions provide excellent coverage of a wide variety of solar events, a wealth of scientific data—and lots of beautiful imagery.Watch this video on YouTube. || ", "hits": 102 }, { "id": 11246, "url": "https://svs.gsfc.nasa.gov/11246/", "result_type": "Produced Video", "release_date": "2013-04-11T12:00:00-04:00", "title": "The Sun Emits a Mid-level Flare and CME", "description": "The sun emitted a mid-level flare, peaking at 3:16 a.m. EDT on April 11, 2013.Solar flares are powerful bursts of radiation. Harmful radiation from a flare cannot pass through Earth's atmosphere to physically affect humans on the ground, however — when intense enough — they can disturb the atmosphere in the layer where GPS and communications signals travel. This disrupts the radio signals for as long as the flare is ongoing, anywhere from minutes to hours.This flare is classified as an M6.5 flare, some ten times less powerful than the strongest flares, which are labeled X-class flares. M-class flares are the weakest flares that can still cause some space weather effects near Earth. This flare produced a radio blackout that has since subsided. The blackout was categorized as an R2 on a scale between R1 and R5 on NOAA's space weather scales.This is the strongest flare seen so far in 2013. Increased numbers of flares are quite common at the moment, since the sun's normal 11-year activity cycle is ramping up toward solar maximum, which is expected in late 2013. Humans have tracked this solar cycle continuously since it was discovered, and it is normal for there to be many flares a day during the sun's peak activity. || ", "hits": 48 }, { "id": 11207, "url": "https://svs.gsfc.nasa.gov/11207/", "result_type": "Produced Video", "release_date": "2013-02-07T10:30:00-05:00", "title": "The Sun Produces Two CMEs", "description": "In the evening of Feb. 5, 2013, the sun erupted with two coronal mass ejections or CMEs that may glance near-Earth space. Experimental NASA research models, based on observations from the Solar Terrestrial Relations Observatory (STEREO) and ESA/NASA's Solar and Heliospheric Observatory, show that the first CME began at 7 p.m. EST and left the sun at speeds of around 750 miles per second. The second CME began at 10:36 p.m. EST and left the sun at speeds of around 350 miles per second. Historically, CMEs of this speed and direction have been benign.Not to be confused with a solar flare, a CME is a solar phenomenon that can send solar particles into space and reach Earth one to three days later.Earth-directed CMEs can cause a space weather phenomenon called a geomagnetic storm, which occurs when they connect with the outside of the Earth's magnetic envelope, the magnetosphere, for an extended period of time. In the past, CMEs at this strength have had little effect. They may cause auroras near the poles but are unlikely to disrupt electrical systems on Earth or interfere with GPS or satellite-based communications systems. || ", "hits": 53 }, { "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": 35 }, { "id": 3956, "url": "https://svs.gsfc.nasa.gov/3956/", "result_type": "Visualization", "release_date": "2012-09-20T00:00:00-04:00", "title": "Halloween Solar Storms - 2003", "description": "This is a 1024x1024 pixel version of solar storms providing a more complete view of the SOHO/LASCO/C3 field-of-view.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. || ", "hits": 140 }, { "id": 3995, "url": "https://svs.gsfc.nasa.gov/3995/", "result_type": "Visualization", "release_date": "2012-09-20T00:00:00-04:00", "title": "The Heliophysics Fleet at Lagrange Point 1", "description": "NASA and ESA operate a fleet of heliophysics satellites at the 'balance point' between the Earth and the Sun, known as Lagrange Point 1, or L1. SOHO, ACE, and Wind have been operating at this point for over 15 years (see SOHO @ 15, ACE @ 15). || ", "hits": 77 }, { "id": 10959, "url": "https://svs.gsfc.nasa.gov/10959/", "result_type": "Produced Video", "release_date": "2012-04-24T10:00:00-04:00", "title": "NASA Scientists Answer Top Space Weather Questions", "description": "NASA scientists answer some common questions about the sun, space weather, and how they affect the Earth. This is a two-part series.Part One addresses:1. What is space weather?2. What are coronal mass ejections?3. What are solar flares?4. What are solar energetic particles?5. What causes flares and CMEs?Part Two addresses:1. Do all flares and CMEs affect the Earth?2. What happens when a flare or CME hits the Earth?3. How quickly can we feel the effects of space weather?4. Why are there more flares and CMEs happening now?For more information about all these questions and more, visit NASA's Space Weather FAQ.For individual interview responses to frequently asked space weather questions, go here. || ", "hits": 69 }, { "id": 10109, "url": "https://svs.gsfc.nasa.gov/10109/", "result_type": "Produced Video", "release_date": "2011-08-09T10:00:00-04:00", "title": "X-Class: A Guide to Solar Flares", "description": "Flares happen when the powerful magnetic fields in and around the sun reconnect. They're usually associated with active regions, often seen as sun spots, where the magnetic fields are strongest. Flares are classified according to their strength. The smallest ones are B-class, followed by C, M and X, the largest. Similar to the Richter scale for earthquakes, each letter represents a ten-fold increase in energy output. So an X is 10 times an M and 100 times a C. Within each letter class, there is a finer scale from 1 to 9. C-class flares are too weak to noticeably affect Earth. M-class flares can cause brief radio blackouts at the poles and minor radiation storms that might endanger astronauts. Although X is the last letter, there are flares more than 10 times the power of an X1, so X-class flares can go higher than 9. The most powerful flare on record was in 2003, during the last solar maximum. It was so powerful that it overloaded the sensors measuring it. They cut-out at X17, and the flare was later estimated to be about X45. A powerful X-class flare like that can create long lasting radiation storms, which can harm satellites and even give airline passengers, flying near the poles, small radiation doses. X flares also have the potential to create global transmission problems and world-wide blackouts. || ", "hits": 2311 }, { "id": 10720, "url": "https://svs.gsfc.nasa.gov/10720/", "result_type": "Produced Video", "release_date": "2011-02-07T12:00:00-05:00", "title": "From Stonehenge to STEREO: A One Minute History of How We See the Sun", "description": "Humans have always wanted to learn about the Sun, but our understanding of our favorite star has changed through the centuries. In prepartion for Sun360, when the STEREO spacecrafts will provide the first uninterrupted view of the Sun, this video is a condensed history of how we have studied the Sun over time. || ", "hits": 36 }, { "id": 10718, "url": "https://svs.gsfc.nasa.gov/10718/", "result_type": "Produced Video", "release_date": "2011-02-06T10:00:00-05:00", "title": "STEREO Sun360", "description": "Launched in October 2006, STEREO traces the flow of energy and matter from the sun to Earth. It also provides unique and revolutionary views of the sun-Earth system. The mission observed the sun in 3-D for the first time in 2007. In 2009, the twin spacecraft revealed the 3-D structure of coronal mass ejections which are violent eruptions of matter from the sun that can disrupt communications, navigation, satellites and power grids on Earth.Seeing?the whole sun front and back simultaneously will enable significant advances in space weather forecasting for Earth and for planning for future robotic and manned spacecraft missions throughout the solar system.These views are the result of observations by NASA's two Solar TErrestrial Relations Observatory (STEREO) spacecraft. The duo are on diametrically opposite sides of the sun, 180 degrees apart. One is ahead of Earth in its orbit, the other trailing behind.For the STEREO Sun360 Teaser, go here.For the full visualization showing STEREO's path go here.For the visualization showing STEREO's increasing coverage of the sun (visual 3) go here.For animations from the STEREO Teaser and stages of coverage, go here.For animations showing STEREO's 3D coverage of a CME go here. || ", "hits": 217 }, { "id": 3755, "url": "https://svs.gsfc.nasa.gov/3755/", "result_type": "Visualization", "release_date": "2010-07-23T00:00:00-04:00", "title": "December 2006 Flare from SOHO/EIT and Hinode/XRT", "description": "This movie shows data of the December 13, 2006 flare event seen by SOHO/EIT (left) and Hinode XRT (right). The field-of-view of the Hinode images is marked with the yellow border on SOHO/EIT.This movie shows the same event as that in Hinode's High-Resolution View of the Sun. || ", "hits": 25 }, { "id": 3740, "url": "https://svs.gsfc.nasa.gov/3740/", "result_type": "Visualization", "release_date": "2010-07-08T00:00:00-04:00", "title": "Space Weather Event: The View from L1", "description": "We start from a position 'behind' the Earth, looking towards the Sun. From this position we see the orbit of the Moon as well as three of the heliospheric 'sentinels' (see \"Sentinels of the Heliosphere\"), ACE, SOHO, and Wind patrolling along 'halo orbits' (Wikipedia) around the Sun-Earth Lagrange Point, L1.The CME (orange isosurface) erupts, heading towards the Earth. The density enhancement of the CME is visible in slice of data in the Earth's orbit plane which provides a better sense of when the CME actually reaches the Earth.As the particle density enhancement from the CME strikes the Earth, we see the Earth's magnetosphere respond, with the outer, high density surface (red), 'blown away'. This surface location corresponds roughly to the location of the bow shock. The bow shock has not been eliminated, only some of its particles have been depleted, to be carried off in the CME and solar wind. As the densest material of the CME passes (orange surface), plasma from the CME continues to flow by the Earth, stretching the magnetosphere into a long, thin structure behind the Earth.The magnetosphere slowly recovers from the 'impact', and regions that can confine higher particle densities reform - the red surfaces return. But not for long as the rarefaction behind the CME reaches the Earth. This lower density region provides fewer particles to repopulate the magnetosphere and make it easier for particles confined in the magnetosphere to 'leak' out into the solar wind.For the BATS-R-US model, the isosurface colors are: red=20 AMUs per cubic centimeter, yellow=10.0 AMUs per cubic centimeter, light blue=1.0 AMUs per cubic centimeter, and blue=0.1 AMUs per cubic centimeter. An AMU corresponds to about the mass of a hydrogen atom, the dominant component of the solar wind.This visualization is part of a series of visualizations on space weather modeling. || ", "hits": 23 }, { "id": 10609, "url": "https://svs.gsfc.nasa.gov/10609/", "result_type": "Produced Video", "release_date": "2010-04-27T01:30:00-04:00", "title": "A Weather Satellite Watches The Sun", "description": "GOES is a series of weather satellites providing continuous delivery of real time data helping meteorologists predict weather on Earth with great accuracy. The GOES satellites also look at the Sun and send critical data to space weather forecasters. These space weather warnings are critical to power companies, airplanes, astronauts, and many more. || ", "hits": 247 }, { "id": 10583, "url": "https://svs.gsfc.nasa.gov/10583/", "result_type": "Produced Video", "release_date": "2010-03-16T00:00:00-04:00", "title": "Slices Through the Solar Interior", "description": "Scientists using SOHO/MDI data have looked just below the Sun's surface and clearly observed inward flowing material.The strong magnetic fields in the sunspots promote cooling. Cool material contracts and sinks at speeds of up to 3000 miles per hour. This drives an inward flow, like a planet-sized whirlpool, that holds the sunspot together as long as the field is strong enough. Scientists discovered this using a technique called acoustic tomography - a novel method similar to ultrasound diagnostics in medicine that uses sound waves to image structures inside the human body. Scientists also found that sunspots are surprisingly shallow. Conditions in sunspots change from cooler than the surrounding plasma to hotter than the surrounding plasma just 3000 miles below the surface. The cool part of a sunspot has the shape of a stack of two or three nickels. Sunspot magnetic fields block the flows that carry heat energy up from the hot solar interior. That results in higher temperatures below the blockage and cooler temperatures above. The downward flows mentioned above dissipate at the same depth. With these data one cannot get a sharp enough picture to really explain the details. Understanding sunspots is essential for understanding the 11-year solar cycle, solar flare explosions, and huge coronal mass ejections that affect life and society on Earth. || ", "hits": 56 }, { "id": 3505, "url": "https://svs.gsfc.nasa.gov/3505/", "result_type": "Visualization", "release_date": "2009-10-01T00:00:00-04:00", "title": "Solar Cycle 23: Minimum-Maximum-Minimum Synoptic Sequence", "description": "This is a sequence of solar synoptic maps covering Solar Cycle 23.The SOHO spacecraft began collecting this data in May of 1996, near the beginning (minimum) of the sunspot cycle. The sequence is projected in cylindrical-equidistant (CED) coordinates suitable for reprojection on spheres for animation or visualization purposes. These images are not suitable for scientific analysis.The original data were collected in FITS format from the SOHO/MDI archive, one image for each Carrington Rotation, which are 27.2753 days long.Solar minimum for Cycle 23 was in May 1996 (Carrington Rotation #1909), solar maximum around March 2000 (Carrington Rotation #1960), with a return to minimum about October 2008 (Carrington Rotation #2075). There are two gaps in the sequence, totalling four rotations, at Carrington rotations #1938, 1939, 1940, 1941, and 1998. These images are missing from the sequence due to SOHO being offline. Gaps in the data coverage for individual maps (occasional day outages or poor coverage near the poles of the Sun) were filled using data accumulated from previous maps.IMPORTANT NOTE: These images are for visualization purposes only. They are not suitable for scientific analysis. || ", "hits": 85 }, { "id": 3595, "url": "https://svs.gsfc.nasa.gov/3595/", "result_type": "Visualization", "release_date": "2009-07-27T00:00:00-04:00", "title": "Sentinels of the Heliosphere", "description": "Heliophysics is a term to describe the study of the Sun, its atmosphere or the heliosphere, and the planets within it as a system. As a result, it encompasses the study of planetary atmospheres and their magnetic environment, or magnetospheres. These environments are important in the study of space weather.As a society dependent on technology, both in everyday life, and as part of our economic growth, space weather becomes increasingly important. Changes in space weather, either by solar events or geomagnetic events, can disrupt and even damage power grids and satellite communications. Space weather events can also generate x-rays and gamma-rays, as well as particle radiations, that can jeopardize the lives of astronauts living and working in space.This visualization tours the regions of near-Earth orbit; the Earth's magnetosphere, sometimes called geospace; the region between the Earth and the Sun; and finally out beyond Pluto, where Voyager 1 and 2 are exploring the boundary between the Sun and the rest of our Milky Way galaxy. Along the way, we see these regions patrolled by a fleet of satellites that make up NASA's Heliophysics Observatory Telescopes. Many of these spacecraft do not take images in the conventional sense but record fields, particle energies and fluxes in situ. Many of these missions are operated in conjunction with international partners, such as the European Space Agency (ESA) and the Japanese Space Agency (JAXA).The Earth and distances are to scale. Larger objects are used to represent the satellites and other planets for clarity.Here are the spacecraft featured in this movie:Near-Earth Fleet:Hinode: Observes the Sun in multiple wavelengths up to x-rays. SVS pageRHESSI : Observes the Sun in x-rays and gamma-rays. SVS pageTRACE: Observes the Sun in visible and ultraviolet wavelengths. SVS pageTIMED: Studies the upper layers (40-110 miles up) of the Earth's atmosphere.FAST: Measures particles and fields in regions where aurora form.CINDI: Measures interactions of neutral and charged particles in the ionosphere. AIM: Images and measures noctilucent clouds. SVS pageGeospace Fleet:Geotail: Conducts measurements of electrons and ions in the Earth's magnetotail. Cluster: This is a group of four satellites which fly in formation to measure how particles and fields in the magnetosphere vary in space and time. SVS pageTHEMIS: This is a fleet of five satellites to study how magnetospheric instabilities produce substorms. SVS pageL1 Fleet: The L1 point is a Lagrange Point, a point between the Earth and the Sun where the gravitational pull is approximately equal. Spacecraft can orbit this location for continuous coverage of the Sun.SOHO: Studies the Sun with cameras and a multitude of other instruments. SVS pageACE: Measures the composition and characteristics of the solar wind. Wind: Measures particle flows and fields in the solar wind. Heliospheric FleetSTEREO-A and B: These two satellites observe the Sun, with imagers and particle detectors, off the Earth-Sun line, providing a 3-D view of solar activity. SVS pageHeliopause FleetVoyager 1 and 2: These spacecraft conducted the original 'Planetary Grand Tour' of the solar system in the 1970s and 1980s. They have now travelled further than any human-built spacecraft and are still returning measurements of the interplanetary medium. SVS pageThis enhanced, narrated visualization was shown at the SIGGRAPH 2009 Computer Animation Festival in New Orleans, LA in August 2009; an eariler version created for AGU was called NASA's Heliophysics Observatories Study the Sun and Geospace. || ", "hits": 99 }, { "id": 10421, "url": "https://svs.gsfc.nasa.gov/10421/", "result_type": "Produced Video", "release_date": "2009-04-07T00:00:00-04:00", "title": "SOHO/TRACE Intro", "description": "On April 3, 2009, countries from around the world participated in the '100 Hours of Astronomy' webcast to celebrate the International Year of Astronomy. This movie was used to introduce the SOHO/TRACE segment. Alex Young and Dawn Meyers, NASA scientists, describe how both SOHO and TRACE view the sun in their own unique way. || ", "hits": 54 }, { "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": 30 }, { "id": 3570, "url": "https://svs.gsfc.nasa.gov/3570/", "result_type": "Visualization", "release_date": "2008-12-15T00:00:00-05:00", "title": "NASA's Heliophysics Observatories Study the Sun and Geospace", "description": "Heliophysics is a term to describe the study of the Sun, its atmosphere or the heliosphere, and the planets within it as a system. As a result, it encompasses the study of planetary atmospheres and their magnetic environment, or magnetospheres. These environments are important in the study of space weather.As a society dependent on technology, both in everyday life, and as part of our economic growth, space weather becomes increasingly important. Changes in space weather, either by solar events or geomagnetic events, can disrupt and even damage power grids and satellite communications. Space weather events can also generate x-rays and gamma-rays, as well as particle radiations, that can jeopardize the lives of astronauts living and working in space.This visualization tours the regions of near-Earth orbit; the Earth's magnetosphere, sometimes called geospace; the region between the Earth and the Sun; and finally out beyond Pluto, where Voyager 1 and 2 are exploring the boundary between the Sun and the rest of our Milky Way galaxy. Along the way, we see these regions patrolled by a fleet of satellites that make up NASA's Heliophysics Observatory Telescopes. Many of these spacecraft do not take images in the conventional sense but record fields, particle energies and fluxes in situ. Many of these missions are operated in conjunction with international partners, such as the European Space Agency (ESA) and the Japanese Space Agency (JAXA).The Earth and distances are to scale. Larger objects are used to represent the satellites and other planets for clarity.Here are the spacecraft featured in this movie:Near-Earth Fleet:Hinode: Observes the Sun in multiple wavelengths up to x-rays. SVS pageRHESSI : Observes the Sun in x-rays and gamma-rays. SVS pageTRACE: Observes the Sun in visible and ultraviolet wavelengths. SVS pageTIMED: Studies the upper layers (40-110 miles up) of the Earth's atmosphere.FAST: Measures particles and fields in regions where aurora form.CINDI: Measures interactions of neutral and charged particles in the ionosphere. AIM: Images and measures noctilucent clouds. SVS pageGeospace Fleet:Geotail: Conducts measurements of electrons and ions in the Earth's magnetotail. Cluster: This is a group of four satellites which fly in formation to measure how particles and fields in the magnetosphere vary in space and time. SVS pageTHEMIS: This is a fleet of five satellites to study how magnetospheric instabilities produce substorms. SVS pageL1 Fleet: The L1 point is a Lagrange Point between the Sun and the Earth. Spacecraft can orbit this location for continuous coverage of the Sun.SOHO: Studies the Sun with cameras and a multitude of other instruments. SVS pageACE: Measures the composition and characteristics of the solar wind. Wind: Measures particle flows and fields in the solar wind. Heliospheric FleetSTEREO-A and B: These two satellites observe the Sun, with imagers and particle detectors, off the Earth-Sun line, providing a 3-D view of solar activity. SVS pageHeliopause FleetVoyager 1 and 2: These spacecraft conducted the original 'Planetary Grand Tour' of the solar system in the 1970s and 1980s. They have now travelled further than any human-built spacecraft and are still returning measurements of the interplanetary medium. SVS pageA refined and narrated version of this visualization, Sentinels of the Heliosphere, is now available. || ", "hits": 79 }, { "id": 3548, "url": "https://svs.gsfc.nasa.gov/3548/", "result_type": "Visualization", "release_date": "2008-09-10T00:00:00-04:00", "title": "Comparison: Solar Minimum from SOHO/EIT", "description": "This is a short movie of the Sun at the minimum of solar activity. This images are collected in ultraviolet light (a wavelength of 195 Å or 19.5 nanometers) which is only visible to space-based instruments. In visible light, few to now sunspots would be visible.At solar minimum, we see few bright active regions. The mottled look is from small 'hot spots' which last less than 48 hours. There are dark regions at the top and bottom of the Sun (corresponding to the north and south solar poles) created by solar magnetic field lines that connect to the interstellar magnetic field. A similar dark region, below the solar equator, is called a coronal hole, where open magnetic field lines enable particles to stream away at high speeds. || ", "hits": 44 }, { "id": 3549, "url": "https://svs.gsfc.nasa.gov/3549/", "result_type": "Visualization", "release_date": "2008-09-10T00:00:00-04:00", "title": "Comparison: Solar Maximum from SOHO/EIT", "description": "A short movie of the Sun at maximum solar activity as seen in ultraviolet light. These images are collected in ultraviolet light (a wavelength of 195Å or 19.5 nanometers) which is only visible to space-based instruments. In visible light, the bright white regions in these images would probably correspond to sunspots.At solar maximum, we see many bright active regions which tend to form in bands in the northern and southern hemispheres. Many of the active regions may eventually launch solar flares or coronal mass ejections (CME). || ", "hits": 35 }, { "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": 106 }, { "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": 220 }, { "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": 91 }, { "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": 24 }, { "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": 57 }, { "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": 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": 16 }, { "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": 24 }, { "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": 49 }, { "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": 75 }, { "id": 3431, "url": "https://svs.gsfc.nasa.gov/3431/", "result_type": "Visualization", "release_date": "2007-05-29T00:00:00-04:00", "title": "Coronal Mass Ejections (CME): Radio Quiet Variety", "description": "This is a simple comparison of SOHO/LASCO/C3 difference images (left side) combined with radio data from Wind/WAVES (right side).The LASCO difference images are produced from a time series of images by subtracting the previous image from the current image. Moving material therefore appears white on the leading edge and dark behind it. The WAVES spectrograph shows the variation of radio intensity (black is low, violet is high) in frequency (vertical axis) and time(horizontal axis). A vertical white bar marks the time of the LASCO image.This CME shows no radio-loud emission between 0.2-1.0 MHz. || ", "hits": 24 }, { "id": 3432, "url": "https://svs.gsfc.nasa.gov/3432/", "result_type": "Visualization", "release_date": "2007-05-29T00:00:00-04:00", "title": "Coronal Mass Ejections (CME): Radio Loud Variety", "description": "This is a simple comparison of SOHO/LASCO/C3 difference images (left side) combined with radio data from Wind/WAVES (right side).The LASCO difference images are produced from a time series of images by subtracting the previous image from the current image. Moving material therefore appears white on the leading edge and dark behind it. The WAVES spectrograph shows the variation of radio intensity (black is low, violet is high) in frequency (vertical axis) and time(horizontal axis). A vertical white bar marks the time of the LASCO image.The radio-loud emission of the CME is the yellow-orange band between 0.2-1.0 MHz. || ", "hits": 52 }, { "id": 3406, "url": "https://svs.gsfc.nasa.gov/3406/", "result_type": "Visualization", "release_date": "2007-03-01T00:00:00-05:00", "title": "STEREO Coronal Mass Ejection: From the EUVI to HI-2", "description": "This movie collects imagery from SOHO and STEREO-A of a coronal mass ejection (CME) during January of 2007. The instruments in this view, from left to right, are STEREO/HI-1, STEREO/HI-2, SOHO/LASCO/C3, SOHO/LASCO/C2, and STEREO/EUVI. The Heliospheric Imager, HI-2, shows some of the tail of comet McNaught. The dark trapezoidal shape on the left edge of the image in HI-2 is the Earth occulter which will block out the disk of the Earth when it moves into view (since the planet will appear so bright as to saturate the detectors). Due to ongoing work with the STEREO coronagraphs, COR1 and COR2, the SOHO/LASCO coronagraphs are used for this movie. The blue Sun in the center of the coronagraphs is STEREO/EUVI ultraviolet images.There is a 22 hour gap in the data coverage for HI-2 which creates the appearance of a jump in the playback.These are not standard images but are called 'running difference' images which highlight changes in the view. White pixels correspond to increases in brightness, while dark pixels reflect a decrease in brightness, with respect to the immediately previous image.'Running differencing' generates some unusual effects. For example, the mottled background is created by the motion of the stars through the field-of-view as the spacecraft pointing direction slowly changes (the Andromeda galaxy is the oblong 'smudge' near the upper left corner). The planets Venus (right edge of HI-2) and Mercury are visible (near center of HI-1), their column of pixels saturated due to their brightness.STEREO: Solar TErrestrial RElations ObservatorySOHO: SOlar Heliospheric ObservatoryLASCO: Large Angle and Spectrometric CoronagraphEUVI: Extreme UltraViolet Imager || ", "hits": 39 }, { "id": 3386, "url": "https://svs.gsfc.nasa.gov/3386/", "result_type": "Visualization", "release_date": "2006-11-08T00:00:00-05:00", "title": "Mercury Transit from SOHO/MDI", "description": "This is a view of the planet Mercury (the tiny moving black dot) as seen by the SOHO MDI.The narrow field-of-view for this camera mode necessitates the addition of black bars at the top and bottom of the frame to match HD720 resolution.This movie was generated from telemetry which has undergone a minimum of processing (to deliver quickly for the media) so data dropouts and other quick-processing artifacts may be visible. Special thanks to Steele Hill of the SOHO project for this effort. || ", "hits": 24 }, { "id": 3336, "url": "https://svs.gsfc.nasa.gov/3336/", "result_type": "Visualization", "release_date": "2006-04-01T00:00:00-05:00", "title": "The Visible Sun Revisited", "description": "Scientists working with the SOHO/MDI instrument have continued to improve on previous results. Since the first release (SOHO/MDI's 'Window' Through the Sun), improvements in helioseismology techniques have enabled them to extract more information from the same data. In this case, sonogram-type imaging of the solar far side (the side of the Sun NOT facing the Earth) has been improved to provide a more complete view of the farside. This is important in space weather forecasting as it enables us to see large sunspots and active regions before they are visible directly from the Earth. Active regions are a source of solar flares which can send high-energy protons towards the Earth. These protons can damage satellite electronics, endangering communications and weather forecasting, and are a health threat to astronauts. || ", "hits": 40 }, { "id": 3346, "url": "https://svs.gsfc.nasa.gov/3346/", "result_type": "Visualization", "release_date": "2006-03-30T00:00:00-05:00", "title": "Grand Tour of the Coronal Loops Model", "description": "This is a longer coronal loops tour combining components of the two previous versions (Animation IDs 3286 and 3287). The solar model is constructed from magnetogram data collected by SOHO/MDI. Because we do not see the full solar surface at any one time, the magnetograms collected over the course of a solar rotation are processed through a time-evolving solar surface model which provides a snapshot of the surface at a fixed time. The resulting magnetogram is then processed through the Potential Field Source Surface (PFSS) model which constructs the magnetic field above the solar surface. The magnetic field around the Sun is then analyzed for field lines, which creates the loop structures we see in the model. Hot plasma tends to flow along the magnetic field lines, creating the coronal loops. These loops are only visible at the higher temperatures corresponding to ultraviolet light, in this case, 195 angstroms, one of the filter wavelengths of SOHO/EIT. For this version, we color the coronal loops green for ready comparison to the EIT 195 angstrom imagery using the EIT standard color table. || ", "hits": 80 }, { "id": 3286, "url": "https://svs.gsfc.nasa.gov/3286/", "result_type": "Visualization", "release_date": "2005-10-27T00:00:00-04:00", "title": "Flight through the Coronal Loops", "description": "Here we illustrate the potential benefits of the 3-D views of the Sun which STEREO will provide. Starting with a simple 2-D EIT ultraviolet image from SOHO, we transition to a 3-D model and move through the coronal loops which are constructed along solar magnetic fields. The solar model is constructed from magnetogram data collected by SOHO/MDI. Because we do not see the full solar surface at any one time, the magnetograms collected over the course of a solar rotation are processed through a time-evolving solar surface model to provide a snapshot of the surface at a fixed time. The resulting magnetogram is then processed through the Potential Field Source Surface (PFSS) model. Coronal loops are visible at the higher temperatures of ultraviolet light, in this case, 195 angstroms, the filter wavelength of SOHO/EIT. For this version, we color the coronal loops green for ready comparison to the EIT 195 angstrom imagery using the EIT 'standard color table'. || ", "hits": 26 }, { "id": 3287, "url": "https://svs.gsfc.nasa.gov/3287/", "result_type": "Visualization", "release_date": "2005-10-27T00:00:00-04:00", "title": "Rotating Tour of Solar Coronal Loops", "description": "A slow rotating tour of a data-based coronal loop model. This version is designed for continuous loop play. The solar model is constructed from magnetogram data collected by SOHO/MDI. Because we do not see the full solar surface at any one time, the magnetograms collected over the course of a solar rotation are processed through a time-evolving solar surface model to provide a snapshot of the surface at a fixed time. The resulting magnetogram is then processed through the Potential Field Source Surface (PFSS) model. Coronal loops are visible at the higher temperatures of ultraviolet light, in this case, 195 angstroms, the filter wavelength of SOHO/EIT. || ", "hits": 49 }, { "id": 3211, "url": "https://svs.gsfc.nasa.gov/3211/", "result_type": "Visualization", "release_date": "2005-08-16T12:00:00-04:00", "title": "Space Weather Forecasting: Quiet Times Ahead", "description": "SOHO/MDI magnetograms combined with the Potential-Field Source-Surface (PFSS) model can be used to generate a model of magnetic field lines in the lower part of the solar corona. When these models are compared to the loops visible in TRACE imagery, a good match (as in this case) indicates that the region will not generate flare events over the next few days. || ", "hits": 10 }, { "id": 3212, "url": "https://svs.gsfc.nasa.gov/3212/", "result_type": "Visualization", "release_date": "2005-08-16T12:00:00-04:00", "title": "Space Weather Forecasting: Active Times Ahead", "description": "SOHO/MDI magnetograms combined with the Potential-Field Source-Surface (PFSS) model can be used to generate a model of magnetic field lines in the lower part of the solar corona. When these models are compared to the loops visible in TRACE imagery, a bad match (as in this case) indicates that the region will generate flare events over the next few days. || ", "hits": 11 }, { "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": 32 }, { "id": 3160, "url": "https://svs.gsfc.nasa.gov/3160/", "result_type": "Visualization", "release_date": "2005-05-24T12:00:00-04:00", "title": "January 2005 Solar Flares from SOHO/EIT", "description": "SOHO/EIT's view of the Sun in late January 2005. || fast_eit.0000.jpg (720x480) [44.6 KB] || fast_eit_320x240_pre.jpg (320x240) [8.1 KB] || fast_eit_NTSC.webmhd.webm (960x540) [4.1 MB] || fast_eit_640x480.mpg (640x480) [15.0 MB] || fast_eit_NTSC.m2v (720x480) [24.0 MB] || 720x480_4x3_30 (720x480) [32.0 KB] || a003160_fast_eit_NTSC.mp4 (640x480) [4.8 MB] || fast_eit_320x240.mpg (320x240) [3.9 MB] || ", "hits": 35 }, { "id": 2922, "url": "https://svs.gsfc.nasa.gov/2922/", "result_type": "Visualization", "release_date": "2005-03-08T12:00:00-05:00", "title": "Solar Tsunamis - View with a Spin", "description": "Push-in to a region of the Sun to witness a 'solar tsunami' after a flare event. The tsunami moves hot gas (bright) out of the region, revealing cooler regions (darker) below. This view rotates on the push-in to keep the region of the flare event visible (to the left in the final frame). || ", "hits": 10 }, { "id": 2959, "url": "https://svs.gsfc.nasa.gov/2959/", "result_type": "Visualization", "release_date": "2004-07-08T12:00:00-04:00", "title": "Halloween Solar Storms from SOHO/EIT, 195 Angstroms", "description": "This view from SOHO/EIT in the 195 angstrom band, shows the multitude of solar flares released in the Fall of 2003 as a group of active regions rotated back into view. This movie is synchronized to play with animation IDs 2960 and 2961. For more information on how X-ray solar flares are classified (B, C, M, X), visit SpaceWeather.com. || ", "hits": 23 }, { "id": 2960, "url": "https://svs.gsfc.nasa.gov/2960/", "result_type": "Visualization", "release_date": "2004-07-08T12:00:00-04:00", "title": "Halloween Solar Storms from SOHO/EIT, 304 Angstroms", "description": "This view from SOHO/EIT in the 304 angstrom band, shows a group of active regions rotating back into view. This movie is synchronized to play with animation IDs 2959 and 2961. One obvious difference is that solar flares are not as visible at this wavelength than at the 195 angstrom band. The 304 angstrom filter was not used as frequently as the 195 angstrom filter, so this movie has more jumps in its time coverage. For more information on how X-ray solar flares are classified (B, C, M, X), visit SpaceWeather.com. || ", "hits": 15 }, { "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": 39 }, { "id": 2950, "url": "https://svs.gsfc.nasa.gov/2950/", "result_type": "Visualization", "release_date": "2004-07-01T12:00:00-04:00", "title": "Building a 3-D Coronal Mass Ejection from 2-D Data", "description": "Using differences in polarization of light directly from the Sun vs. scattered from the CME electrons, it is possible to derive a distance of matter along the line-of-sight. This version is an early release of animation #2958. || ", "hits": 17 }, { "id": 2958, "url": "https://svs.gsfc.nasa.gov/2958/", "result_type": "Visualization", "release_date": "2004-07-01T12:00:00-04:00", "title": "Building a 3-D Coronal Mass Ejection from 2-D Data", "description": "Using differences in polarization of light directly from the Sun vs. scattered from the CME electrons, it is possible to derive a distance of matter along the line-of-sight. This version is an enhanced version of animation ID 2950 with a color table enhanced to show fainter regions of the CME. || ", "hits": 26 }, { "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": 54 }, { "id": 2923, "url": "https://svs.gsfc.nasa.gov/2923/", "result_type": "Visualization", "release_date": "2004-03-08T12:00:00-05:00", "title": "SOHO/MDI's 'Window' Through the Sun", "description": "Using the mathematical techniques, the SOHO/MDI view of the front side of the Sun can be processed to reveal features on the far side of the Sun. || ", "hits": 35 }, { "id": 2917, "url": "https://svs.gsfc.nasa.gov/2917/", "result_type": "Visualization", "release_date": "2004-02-20T12:00:00-05:00", "title": "SORCE Monitors Solar Variability during Record Solar Flares", "description": "The SORCE mission monitors solar variability to determine its impact on the Earth's climate. The X-ray photometer aboard SORCE observes the record-breaking solar flares in the Fall of 2003. The line graph shows the photometer's measured solar radiation flux in the 1-7 nanometer wavelength band (x-ray) measured in milliwatts per square meter. The ultraviolet (195 angstrom) imagery from SOHO/EIT (green) illustrates where the flares (the bright white spots) are located on the solar disk. || ", "hits": 30 }, { "id": 2918, "url": "https://svs.gsfc.nasa.gov/2918/", "result_type": "Visualization", "release_date": "2004-02-20T12:00:00-05:00", "title": "SORCE Monitors Solar Variability during Record Solar Flares - Video version", "description": "The SORCE mission monitors solar variability to determine its impact on the Earth's climate. The X-ray photometer aboard SORCE observes the record-breaking solar flares in the Fall of 2003. The line graph shows the photometer's measured solar radiation flux in the 1-7 nanometer wavelength band (x-ray) measured in milliwatts per square meter. The ultraviolet (195 angstrom) imagery from SOHO/EIT (green) illustrates where the flares (the bright white spots) are located on the solar disk. This version has the contents slightly smaller for use in video. || ", "hits": 64 }, { "id": 2750, "url": "https://svs.gsfc.nasa.gov/2750/", "result_type": "Visualization", "release_date": "2003-09-02T12:00:00-04:00", "title": "RHESSI Observes 2.2 MeV Line Emission from a Solar Flare", "description": "The solar flare at Active Region 10039 on July 23, 2002 exhibits many exceptional high-energy phenomena including the 2.223 MeV neutron capture line and the 511 keV electron-positron (antimatter) annihilation line. In the animation, the RHESSI low-energy channels (12-25 keV) are represented in red and appears predominantly in coronal loops. The high-energy flux appears as blue at the footpoints of the coronal loops. Violet is used to indicate the location and relative intensity of the 2.2MeV emission. || ", "hits": 41 }, { "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": 13 }, { "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": 11 }, { "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": 16 }, { "id": 2735, "url": "https://svs.gsfc.nasa.gov/2735/", "result_type": "Visualization", "release_date": "2003-05-07T12:00:00-04:00", "title": "Mercury Transit of the Sun", "description": "The planet Mercury is visible passing between the Sun and the TRACE spacecraft. Data collected on May 7, 2003, from 04:32:04 to 08:08:57. || a002735.00005_print.png (720x480) [358.5 KB] || a002735.00240_print.png (720x480) [528.2 KB] || MercuryTransit_640x480_pre.jpg (320x240) [5.5 KB] || MercuryTransit_320x240_pre.jpg (320x240) [5.3 KB] || a002735.webmhd.webm (960x540) [4.3 MB] || MercuryTransit_640x480.mpg (640x480) [7.7 MB] || a002735.m2v (720x480) [10.4 MB] || 720x480_4x3_30p (720x486) [16.0 KB] || a002735.dv (720x480) [54.9 MB] || a002735.mp4 (640x480) [2.5 MB] || MercuryTransit_320x240.mpg (320x240) [2.0 MB] || ", "hits": 37 }, { "id": 20075, "url": "https://svs.gsfc.nasa.gov/20075/", "result_type": "Animation", "release_date": "2003-03-26T12:00:00-05:00", "title": "Wave", "description": "Like fans doing the wave at a stadium, large cell-like features called supergranules are moving in a vertical motion, giving the illusion of the solar surface rotating faster than the Sun. || ", "hits": 14 }, { "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": 12 }, { "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": 9 }, { "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": 37 }, { "id": 2655, "url": "https://svs.gsfc.nasa.gov/2655/", "result_type": "Visualization", "release_date": "2002-12-06T12:00:00-05:00", "title": "Solar Eclipse: December 4, 2002", "description": "A composite of red continuum with SOHO/EIT near totality. The red image was taken in Ceduna, South Australia. The images are co-registered so one can install smooth dissolves between them. || Solar eclipse in red continuum || eclipse0002.jpg (1280x960) [46.6 KB] || eclipse0002_web.jpg (320x240) [3.9 KB] || eclipse0002.tif (1280x960) [208.4 KB] || ", "hits": 21 }, { "id": 2495, "url": "https://svs.gsfc.nasa.gov/2495/", "result_type": "Visualization", "release_date": "2002-07-25T12:00:00-04:00", "title": "SOHO/EIT views solar 'Grand Slam'", "description": "A full view of the sun at 195 angstroms from SOHO/EIT. The time covers July 15-23, 2002. Four X-class flares erupted: an X3.0 on July 15, an X1.8 on July 18, a X3.3 on July 20 and an X4.0 on July 23. || ", "hits": 8 }, { "id": 2496, "url": "https://svs.gsfc.nasa.gov/2496/", "result_type": "Visualization", "release_date": "2002-07-25T12:00:00-04:00", "title": "SOHO/EIT Views Solar 'Grand Slam' with Zoom", "description": "A view of the sun at 195 angstroms from SOHO/EIT. The time covers July 15-23, 2002. Four X-class flares erupted: an X3.0 on July 15, an X1.8 on July 18, a X3.3 on July 20 and an X4.0 on July 23. The version zooms in slightly to the flare region. || ", "hits": 15 }, { "id": 2460, "url": "https://svs.gsfc.nasa.gov/2460/", "result_type": "Visualization", "release_date": "2002-06-05T12:00:00-04:00", "title": "RHESSI Observes the Flare over AR9906 - zoom with times", "description": "Zoom in to solar active region AR9906 on April 21, 2002 with SOHO/EIT, TRACE and RHESSI data. RHESSI observes x-rays from this flare. The red contours represent the 12-25 keV photon energy range and the blue contours represent 50-100 keV. || Movie of RHESSI and TRACE data. || a002460.00100_print.png (720x480) [447.6 KB] || ar9906-zoom-dates_pre.jpg (320x240) [6.9 KB] || a002460.webmhd.webm (960x540) [6.9 MB] || ar9906-zoom-dates.mpg (640x480) [15.0 MB] || a002460.dv (720x480) [118.8 MB] || ", "hits": 15 }, { "id": 2461, "url": "https://svs.gsfc.nasa.gov/2461/", "result_type": "Visualization", "release_date": "2002-06-05T12:00:00-04:00", "title": "RHESSI Observes the Flare over AR9906 - zoom without times", "description": "Zoom in to solar active region AR9906 on April 21, 2002 with SOHO/EIT, TRACE and RHESSI data. RHESSI observes x-rays from this flare. The red contours represent the 12-25 keV photon energy range and the blue contours represent 50-100 keV. || ", "hits": 15 }, { "id": 2462, "url": "https://svs.gsfc.nasa.gov/2462/", "result_type": "Visualization", "release_date": "2002-06-05T12:00:00-04:00", "title": "RHESSI Observes the Flare over AR9906 - rotate view with times", "description": "Zoom in (with rotation) to solar active region AR9906 on April 21, 2002 with SOHO/EIT,TRACE and RHESSI data. RHESSI observes x-rays from this flare. The red contours represent the 12-25 keV photon energy range and the blue contours represent 50-100 keV. || ", "hits": 12 } ] }