{ "count": 100, "next": null, "previous": null, "results": [ { "id": 40548, "url": "https://svs.gsfc.nasa.gov/gallery/solarand-heliospheric-observatory-soho/", "result_type": "Gallery", "release_date": "2026-03-03T00:00:00-05:00", "title": "SOHO – Solar and Heliospheric Observatory", "description": "Launched in December 1995, the Solar and Heliospheric Observatory (SOHO) is a joint mission between NASA and ESA (European Space Agency) designed to study the Sun inside out. Though its mission was originally scheduled to last until 1998, SOHO continues to collect observations about the Sun’s interior, the solar atmosphere, and the constant stream of solar particles known as the solar wind, adding to scientists' understanding of our closest star and making many new discoveries, including finding more than 5,000 comets.\n\nLearn more: https://science.nasa.gov/mission/soho/", "hits": 468 }, { "id": 5609, "url": "https://svs.gsfc.nasa.gov/5609/", "result_type": "Visualization", "release_date": "2026-01-26T05:00:00-05:00", "title": "Heliophysics Satellite Fleet - 2026", "description": "A tour of the NASA Heliophysics fleet from near-Earth satellites out to the Voyagers beyond the heliopause.", "hits": 861 }, { "id": 14802, "url": "https://svs.gsfc.nasa.gov/14802/", "result_type": "Produced Video", "release_date": "2025-03-28T14:31:59-04:00", "title": "Earth to Space: A National Symphony Orchestra Concert", "description": "Explore the vastness of space with music inspired by the planets, stars, and beyond! In anticipation of the upcoming voyage of Artemis II, the National Symphony Orchestra celebrates the discoveries and beauty of space through music and images produced by NASA. Explore this page to learn more about the visuals used in the Kennedy Center's 2025 Earth to Space Festival NSO Family Concert.", "hits": 140 }, { "id": 14779, "url": "https://svs.gsfc.nasa.gov/14779/", "result_type": "Produced Video", "release_date": "2025-02-11T09:00:00-05:00", "title": "NASA's Illuminate Series (2025)", "description": "NASA's Illuminate is a video series about out-of-this-world images that shine light on our Sun and solar system. || ", "hits": 226 }, { "id": 14741, "url": "https://svs.gsfc.nasa.gov/14741/", "result_type": "Produced Video", "release_date": "2024-12-27T13:00:00-05:00", "title": "Parker Solar Probe: Humanity’s Closest Encounter with the Sun", "description": "Controllers have confirmed NASA’s mission to “touch” the Sun survived its record-breaking closest approach to the solar surface on Dec. 24, 2024.Breaking its previous record by flying just 3.8 million miles above the surface of the Sun, NASA’s Parker Solar Probe hurtled through the solar atmosphere at a blazing 430,000 miles per hour — faster than any human-made object has ever moved. A beacon tone received in the late evening hours of Dec. 26 confirmed the spacecraft had made it through the encounter safely and is operating normally.This pass, the first of more to come at this distance, allows the spacecraft to conduct unrivaled scientific measurements with the potential to change our understanding of the Sun. || ", "hits": 522 }, { "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": 83 }, { "id": 20388, "url": "https://svs.gsfc.nasa.gov/20388/", "result_type": "Animation", "release_date": "2023-12-05T14:00:00-05:00", "title": "PUNCH Spacecraft Beauty Passes", "description": "NASA’s Polarimeter to Unify the Corona and Heliosphere (PUNCH) mission is a constellation of four small satellites in Sun-synchronous, low Earth orbit that will make global, 3D observations of the young solar wind, from the outermost solar atmosphere to the inner heliopshere. Images of unprecedented quality will help to close a 60-year gap in measurements of understanding of what occurs in this region of space. PUNCH will share a ride to space with NASA’s Jet Propulsion Laboratory’s Spectro-Photometer for the History of the Universe, Epoch of Re-ionization, and Ices Explorer (SPHEREx) mission. The missions launched on March 11, 2025, on a SpaceX Falcon 9 rocket from Space Launch Complex 4 East at Vandenberg Space Force Base in California.Get the latest updates on NASA's PUNCH blog. || ", "hits": 76 }, { "id": 14374, "url": "https://svs.gsfc.nasa.gov/14374/", "result_type": "Infographic", "release_date": "2023-08-03T11:00:00-04:00", "title": "A Guide to Cosmic Temperatures", "description": "Explore the temperatures of the cosmos, from absolute zero to the hottest temperatures yet achieved, with this infographic. Targets for the XRISM mission include supernova remnants, binary systems with stellar-mass black holes, galaxies powered by supermassive black holes, and vast clusters of galaxies.Credit: NASA's Goddard Space Flight Center/Scott WiessingerMachine-readable PDF copy || Cosmic_Temperatures_Infographic_Final_small.jpg (1383x2048) [1.3 MB] || Cosmic_Temperatures_Infographic_Final_Full.png (5530x8192) [60.5 MB] || Cosmic_Temperatures_Infographic_Final_Full.jpg (5530x8192) [10.3 MB] || Cosmic_Temperatures_Infographic_Final_8bit.png (5530x8192) [24.5 MB] || Cosmic_Temperatures_Infographic_Final_Half.png (2765x4096) [7.0 MB] || Cosmic_Temperatures_Infographic_Final_Half.jpg (2765x4096) [4.7 MB] || ", "hits": 1095 }, { "id": 14276, "url": "https://svs.gsfc.nasa.gov/14276/", "result_type": "Produced Video", "release_date": "2023-01-12T08:00:00-05:00", "title": "Strong Solar Flare Erupts from Sun on January 10, 2023", "description": "An X1.0 class solar flare flashes on the left edge of the Sun on January 10, 2023. This image was captured by NASA's Solar Dynamics Observatory and shows a blend of light from the 304 and 131 angstrom wavelengths.Credit: NASA/GSFC/SDO || 1-10-23_2251UT_131_304_X1.jpg (4096x4096) [2.0 MB] || JHV_2023-01-10_18.38.48-0001.png (4096x4096) [19.1 MB] || 1-10-23_2251UT_131_304_X1_searchweb.png (320x180) [104.2 KB] || 1-10-23_2251UT_131_304_X1_thm.png (80x40) [6.9 KB] || ", "hits": 62 }, { "id": 14279, "url": "https://svs.gsfc.nasa.gov/14279/", "result_type": "Produced Video", "release_date": "2022-12-14T00:00:00-05:00", "title": "Mid-level Solar Flare Erupts from Sun on December 14, 2022", "description": "An M6.2 class solar flare flashes on the right side of the Sun on December 14, 2022. This imagery was captured by NASA's Solar Dynamics Observatory and shows light in the 131 angstrom wavelengths.Credit: NASA/SDO || M6pt3Flare12142022_131.gif (500x500) [4.5 MB] || ", "hits": 47 }, { "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": 45 }, { "id": 14275, "url": "https://svs.gsfc.nasa.gov/14275/", "result_type": "Produced Video", "release_date": "2022-10-02T07:00:00-04:00", "title": "Sun Releases X1.0 Flare on October 2, 2022", "description": "An X1.0 class solar flare flashes on the right edge of the Sun on October 2, 2022. This image was captured by NASA's Solar Dynamics Observatory and shows a blend of light from the 171 and 304 angstrom wavelengths.Credit: NASA/GSFC/SDO || Oct_2_2022_X1_flare_131-171.jpg (4096x4096) [3.8 MB] || Oct_2_2022_X1_flare_131-171_searchweb.png (320x180) [98.8 KB] || Oct_2_2022_X1_flare_131-171_thm.png (80x40) [7.7 KB] || ", "hits": 47 }, { "id": 14160, "url": "https://svs.gsfc.nasa.gov/14160/", "result_type": "Produced Video", "release_date": "2022-05-21T13:00:00-04:00", "title": "Sun Emits X1.5 Flare on May 10, 2022", "description": "Short video of the X1.5 flare emitted by the Sun on May 10, 2022 and captured by the Solar Dynamics Observatory in three wavelengths of extreme ultraviolet light that highlight different temperatures and features of the Sun's atmosphere, the corona.Credit: NASA/GSFC/SDOMusic: \"Examples\" from Universal Production MusicComplete transcript available. || May102022_X1pt5Flare_171-131-304.jpg (1920x1080) [979.2 KB] || May102022_X1pt5Flare_171-131-304_searchweb.png (320x180) [55.6 KB] || May102022_X1pt5Flare_171-131-304_thm.png (80x40) [4.4 KB] || 14160_May102022_X1pt5_Flare_ProRes_1920x1080_2997.mov (1920x1080) [829.3 MB] || 14160_May102022_X1pt5_Flare_Best_1080.mp4 (1920x1080) [138.6 MB] || 14160_May102022_X1pt5_Flare_1080.mp4 (1920x1080) [57.0 MB] || 14160_May102022_X1pt5_Flare_ProRes_1920x1080_2997.webm (1920x1080) [5.6 MB] || 14160_May102022_X1pt5_Flare_SRT_Captions.en_US.srt [547 bytes] || 14160_May102022_X1pt5_Flare_SRT_Captions.en_US.vtt [560 bytes] || ", "hits": 64 }, { "id": 14159, "url": "https://svs.gsfc.nasa.gov/14159/", "result_type": "Produced Video", "release_date": "2022-05-06T12:00:00-04:00", "title": "Active Sun in Early May, 2022", "description": "NASA’s Solar Dynamics Observatory captured this image of an X1.1 solar flare – as seen in the bright flash in the upper right portion of the image – on May 3, 2022 at 13:25 UTC. The image is a wavelength of extreme ultraviolet light – 131 angstrom – that highlights the extremely hot material in flares and which is colorized teal.Credit: NASA/SDO || 20220503_FlareX11_131A.00146_print.jpg (1024x1024) [302.4 KB] || 20220503_FlareX11_131A.00146_searchweb.png (320x180) [60.4 KB] || 20220503_FlareX11_131A.00146_thm.png (80x40) [5.1 KB] || 20220503_FlareX11_131A.00146.tiff (4096x4096) [64.0 MB] || ", "hits": 35 }, { "id": 14152, "url": "https://svs.gsfc.nasa.gov/14152/", "result_type": "Produced Video", "release_date": "2022-05-02T11:00:00-04:00", "title": "Strong Solar Flare Erupts from Sun on April 30, 2022", "description": "NASA’s Solar Dynamics Observatory captured this image sequence of an X1.1 solar flare – as seen in the bright flash in the upper right portion of the image – on April 30, 2022. The image is a blend of three wavelengths of extreme ultraviolet light that highlights the extremely hot material in flares and which is colorized in red. The three wavelengths are 131 angstrom, 171 angstrom and 304 angstrom. The sequence has a cadence of one image every 15 minutes and covers 8pm EDT April 29th to 8pm EDT April 30th.Credit: NASA/SDO || April_30_X1_flare_131-171-304.gif (500x500) [6.1 MB] || April_30_X1_flare_4k.mov (4096x4096) [654.3 MB] || April_30_X1_flare_4k.mp4 (4096x4096) [27.5 MB] || April_30_X1_flare_4k.webm (4096x4096) [4.9 MB] || ", "hits": 69 }, { "id": 14129, "url": "https://svs.gsfc.nasa.gov/14129/", "result_type": "Produced Video", "release_date": "2022-04-01T07:00:00-04:00", "title": "Mid-level Solar Flare Erupts from Sun on March 31, 2022", "description": "This is a close-up image captured by NASA’s Solar Dynamics Observatory of today’s solar flare. The image shows a a blend of 131 and 171 angstrom extreme ultraviolet light that highlights the extremely hot material in flares.Credit: NASA/GSFC/SDO || March_31_M9pt7_flare_131-171_1080.jpg (1920x1080) [381.4 KB] || March_31_M9pt7_flare_131-171_1080_searchweb.png (320x180) [87.3 KB] || March_31_M9pt7_flare_131-171_1080_thm.png (80x40) [6.9 KB] || ", "hits": 41 }, { "id": 14128, "url": "https://svs.gsfc.nasa.gov/14128/", "result_type": "Produced Video", "release_date": "2022-03-30T16:00:00-04:00", "title": "Significant Solar Flare Erupts From Sun on March 30, 2022", "description": "An X1.3 class solar flare flashes in center of the Sun on Mar. 30, 2022. This image was captured by NASA's Solar Dynamics Observatory and shows a blend of light from the 171 and 131 angstrom wavelengths.Credit: NASA/GSFC/SDO || Mar302022FlareX1pt3_171-131Blend_2k.jpg (2048x2048) [617.2 KB] || Mar302022FlareX1pt3_171-131Blend_2k_print.jpg (1024x1024) [196.3 KB] || Mar302022FlareX1pt3_171-131Blend_2k_searchweb.png (320x180) [105.8 KB] || Mar302022FlareX1pt3_171-131Blend_2k_thm.png (80x40) [8.3 KB] || ", "hits": 70 }, { "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": 109 }, { "id": 14078, "url": "https://svs.gsfc.nasa.gov/14078/", "result_type": "Produced Video", "release_date": "2022-01-21T22:00:00-05:00", "title": "Mid-Level Flare Erupts From Sun", "description": "The Sun emitted a mid-level solar flare on Jan. 20, 2022, peaking at 1:01 a.m. EST. NASA’s Solar Dynamics Observatory, which watches the Sun constantly, captured an image of the event.Solar flares are powerful bursts of energy. Flares and solar eruptions can impact radio communications, electric power grids, navigation signals, and pose risks to spacecraft and astronauts.This flare is classified as a M5.5 class flare. More info on how flares are classified here.To see how such space weather may affect Earth, please visit NOAA’s Space Weather Prediction Center https://spaceweather.gov/, the U.S. government’s official source for space weather forecasts, watches, warnings, and alerts. NASA works as a research arm of the nation’s space weather effort. NASA observes the Sun and our space environment constantly with a fleet of spacecraft that study everything from the Sun’s activity to the solar atmosphere, and to the particles and magnetic fields in the space surrounding Earth. || ", "hits": 94 }, { "id": 14055, "url": "https://svs.gsfc.nasa.gov/14055/", "result_type": "Produced Video", "release_date": "2021-12-20T22:00:00-05:00", "title": "Parker Solar Probe's WISPR Images Inside The Sun's Atmosphere", "description": "For the first time in history, a spacecraft has touched the Sun. NASA’s Parker Solar Probe has now flown through the Sun’s upper atmosphere – the corona – and sampled particles and magnetic fields there. As Parker Solar Probe flew through the corona, its WISPR instrument captured images.The Wide-Field Imager for Parker Solar Probe (WISPR) is the only imaging instrument aboard the spacecraft. WISPR looks at the large-scale structure of the corona and solar wind before the spacecraft flies through it. About the size of a shoebox, WISPR takes images from afar of structures like coronal mass ejections, or CMEs, jets and other ejecta from the Sun. These structures travel out from the Sun and eventually overtake the spacecraft, where the spacecraft’s other instruments take in-situ measurements. WISPR helps link what’s happening in the large-scale coronal structure to the detailed physical measurements being captured directly in the near-Sun environment.To image the solar atmosphere, WISPR uses the heat shield to block most of the Sun’s light, which would otherwise obscure the much fainter corona. Specially designed baffles and occulters reflect and absorb the residual stray light that has been reflected or diffracted off the edge of the heat shield or other parts of the spacecraft.WISPR uses two cameras with radiation-hardened Active Pixel Sensor CMOS detectors. These detectors are used in place of traditional CCDs because they are lighter and use less power. They are also less susceptible to effects of radiation damage from cosmic rays and other high-energy particles, which are a big concern close to the Sun. The camera’s lenses are made of a radiation hard BK7, a common type of glass used for space telescopes, which is also sufficiently hardened against the impacts of dust.WISPR was designed and developed by the Solar and Heliophysics Physics Branch at the Naval Research Laboratory in Washington, D.C. (principal investigator Russell Howard), which will also develop the observing program. || ", "hits": 438 }, { "id": 14046, "url": "https://svs.gsfc.nasa.gov/14046/", "result_type": "Produced Video", "release_date": "2021-12-17T19:00:00-05:00", "title": "NASA's Solar Tour", "description": "Starting Dec. 3, we took a journey from Earth to the Sun. We made pit stops along the way to learn how the Sun influences everything in the solar system.In 2018, NASA launched Parker Solar Probe to study the Sun up close. But the mission has also taught us much more about our solar system.On the final day of the #SolarTour, we had big news to share: Parker Solar Probe officially “touched” the Sun, becoming the first spacecraft in history to fly through the solar atmosphere.Below are postcards we released at each pit stop of the Solar Tour campaign. || ", "hits": 42 }, { "id": 14035, "url": "https://svs.gsfc.nasa.gov/14035/", "result_type": "Produced Video", "release_date": "2021-12-14T12:00:00-05:00", "title": "AGU 2021 - Major discoveries as NASA’s Parker Solar Probe closes in on the Sun", "description": "NASA’s Parker Solar Probe has now done what no spacecraft has done before—it has officially touched the Sun. Launched in 2018 to study the Sun’s biggest mysteries, the spacecraft has now grazed the edge of the solar atmosphere and gathered new close-up observations of our star. This is allowing us to see the Sun as never before—including the findings in two new papers, which were presented at AGU, that are helping scientists answer fundamental questions about the Sun.PANELISTSDr. Nicola Fox• Heliophysics Division Director of the Science Mission Directorate at NASA HeadquartersDr. Nour Raouafi• Project Scientist for NASA’s Parker Solar Probe• The Johns Hopkins Applied Physics Laboratory Dr. Justin Kasper• Principal Investigator for Solar Wind Electrons Alphas and Protons (SWEAP) Investigation on Parker Solar Probe • BWX Technologies, Inc., University of MichiganProf. Stuart D. Bale• Principal Investigator for Fields Experiment (FIELDS) on Parker Solar Probe • University of California, Berkeley Dr. Kelly Korreck• Program Scientist at NASA Headquarters• Smithsonian Astrophysical Observatory || ", "hits": 130 }, { "id": 14036, "url": "https://svs.gsfc.nasa.gov/14036/", "result_type": "Produced Video", "release_date": "2021-12-14T12:00:00-05:00", "title": "Animation: NASA's Parker Solar Probe Enters Solar Atmosphere", "description": "For the first time in history, a spacecraft has touched the Sun. NASA’s Parker Solar Probe has now flown through the Sun’s upper atmosphere – the corona – and sampled particles and magnetic fields there. The new milestone marks one major step for Parker Solar Probe and one giant leap for solar science. Just as landing on the Moon allowed scientists to understand how it was formed, touching the very stuff the Sun is made of will help scientists uncover critical information about our closest star and its influence on the solar system. On April 28, 2021, during its eighth flyby of the Sun, Parker Solar Probe encountered the specific magnetic and particle conditions at 18.8 solar radii (8.127 million miles) above the solar surface that told scientists it had crossed the Alfvén critical surface for the first time and finally entered the solar atmosphere.More information here. || ", "hits": 201 }, { "id": 14045, "url": "https://svs.gsfc.nasa.gov/14045/", "result_type": "Produced Video", "release_date": "2021-12-14T12:00:00-05:00", "title": "NASA's Parker Solar Probe Touches The Sun For The First Time", "description": "For the first time in history, a spacecraft has touched the Sun. NASA’s Parker Solar Probe has now flown through the Sun’s upper atmosphere – the corona – and sampled particles and magnetic fields there. The new milestone marks one major step for Parker Solar Probe and one giant leap for solar science. Just as landing on the Moon allowed scientists to understand how it was formed, touching the very stuff the Sun is made of will help scientists uncover critical information about our closest star and its influence on the solar system. More information here. || ", "hits": 234 }, { "id": 20354, "url": "https://svs.gsfc.nasa.gov/20354/", "result_type": "Animation", "release_date": "2021-12-14T12:00:00-05:00", "title": "Animation: Origins of Switchbacks", "description": "On recent solar encounters, Parker Solar Probe collected data pinpointing the origin of zig-zag-shaped structures in the solar wind, called switchbacks. The data showed one spot switchbacks originate is at the visible surface of the Sun – the photosphere. By the time it reaches Earth, 93 million miles away, the solar wind is an unrelenting headwind of particles and magnetic fields. But as it escapes the Sun, the solar wind is structured and patchy. In the mid-1990s, the NASA-European Space Agency mission Ulysses flew over the Sun’s poles and discovered a handful of bizarre S-shaped kinks in the solar wind’s magnetic field lines, which detoured charged particles on a zig-zag path as they escaped the Sun. For decades, scientists thought these occasional switchbacks were oddities confined to the Sun’s polar regions. In 2019, at 34 solar radii from the Sun, Parker Solar Probe discovered that switchbacks were not rare, but common in the solar wind. This renewed interest in the features raised new questions: Where are they coming from and how do they form and evolve? Were they forged at the surface of the Sun, or shaped by some process kinking magnetic fields in the solar atmosphere? The new findings, in press at the Astrophysical Journal, finally confirm one origin point near the solar surface. More information here. || ", "hits": 81 }, { "id": 13982, "url": "https://svs.gsfc.nasa.gov/13982/", "result_type": "Produced Video", "release_date": "2021-10-28T14:00:00-04:00", "title": "Active October Sun Emits X-class Flare", "description": "Brighter than a shimmering ghost, faster than the flick of a black cat’s tail, the Sun cast a spell in our direction, just in time for Halloween. This imagery captured by NASA’s Solar Dynamics Observatory covers a busy few days of activity between Oct. 25-28 that ended with a significant solar flare. From late afternoon Oct. 25 through mid-morning Oct. 26, an active region on the left limb of the Sun flickered with a series of small flares and petal-like eruptions of solar material. Meanwhile, the Sun was sporting more active regions at its lower center, directly facing Earth. On Oct. 28, the biggest of these released a significant flare, which peaked at 11:35 a.m. EDT. Credit: NASA/GSFC/SDOMusic: \"Immersion\" from Above and Below. Written and produced by Lars LeonhardWatch this video on the NASA Goddard YouTube channel.Complete transcript available. || ActiveOctober_Still.jpg (1920x1080) [956.2 KB] || 13982_ActiveOctober_ProRes_1920x1080_2997.mov (1920x1080) [2.4 GB] || 13982_ActiveOctober_1080_Best.mp4 (1920x1080) [436.2 MB] || 13982_ActiveOctober_1080.mp4 (1920x1080) [188.1 MB] || 13982_ActiveOctober_1080_Best.webm (1920x1080) [19.7 MB] || 13982_ActiveOctober_SRT_Captions.en_US.srt [574 bytes] || 13982_ActiveOctober_SRT_Captions.en_US.vtt [587 bytes] || ", "hits": 100 }, { "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": 48 }, { "id": 4805, "url": "https://svs.gsfc.nasa.gov/4805/", "result_type": "Visualization", "release_date": "2020-12-07T10:00:00-05:00", "title": "Coordinated Heliosphere - How Solar Missions Work Together", "description": "Using Solar Orbiter, Parker Solar Probe, and other sun-observing missions, in coordinated observations, we can learn far more about the solar atmosphere which surrounds and impacts Earth and other missions in space, crewed and uncrewed. || ", "hits": 48 }, { "id": 13691, "url": "https://svs.gsfc.nasa.gov/13691/", "result_type": "Produced Video", "release_date": "2020-09-21T11:00:00-04:00", "title": "NASA’s IRIS spots Nanojets: Shining light on heating the solar corona", "description": "In pursuit of understanding why the Sun's atmosphere is so much hotter than the surface, and to help differentiate between a host of theories about what causes this heating, researchers turn to NASA's Interface Region Imaging Spectrograph (IRIS) mission. IRIS was finely tuned with a high-resolution imager to zoom in on specific hard-to-see events on the Sun.A paper published in Nature on Sept. 21, 2020, reports on the first ever clear images of nanojets — bright, thin lights that travel perpendicular to magnetic structures in the solar atmosphere called the corona — in a process that reveals the existence of one of the potential coronal heating candidates: nanoflares. || ", "hits": 58 }, { "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": 48 }, { "id": 4854, "url": "https://svs.gsfc.nasa.gov/4854/", "result_type": "Visualization", "release_date": "2020-09-15T10:00:00-04:00", "title": "Coronal Holes at Solar Minimum and Solar Maximum", "description": "A sample of solar coronal holes around the time of the maximum of sunspot activity (April 2014). Note the polar regions are devoid of coronal holes but a large hole appears in the southern hemisphere. || CoronalHoleMax_AIA193_00150_print.jpg (1024x1024) [173.1 KB] || CoronalHoleMax_AIA193_00150_searchweb.png (320x180) [89.6 KB] || CoronalHoleMax_AIA193_00150_thm.png (80x40) [7.4 KB] || CoronalHoleMax_AIA193_2048p30.mp4 (2048x2048) [61.7 MB] || CoronalHoleMax_AIA193_2048p30.webm (2048x2048) [2.9 MB] || AIA193-Time (4096x4096) [64.0 KB] || AIA193-Frames (4096x4096) [64.0 KB] || CoronalHoleMax_Timestamp (600x100) [64.0 KB] || ", "hits": 188 }, { "id": 13664, "url": "https://svs.gsfc.nasa.gov/13664/", "result_type": "Produced Video", "release_date": "2020-07-16T08:00:00-04:00", "title": "ESA and NASA Release First Images From Solar Orbiter Mission", "description": "Scientists from ESA (European Space Agency) and NASA will present the first images captured by Solar Orbiter, the joint ESA/NASA mission to study the Sun, during an online news briefing at 8 a.m. EDT Thursday, July 16. Launched on Feb. 9, 2020, Solar Orbiter turned on all 10 of its instruments together for the first time in mid-June as it made its first close pass of the Sun. The flyby captured the closest images ever taken of the Sun. During the briefing, mission experts will discuss what these closeup images reveal about our star, including what we can learn from Solar Orbiter’s new measurements of particles and magnetic fields flowing from the Sun.The briefing will stream live at:https://www.nasa.gov/solarorbiterfirstlight/Participants in the call include:•Daniel Müller – Solar Orbiter Project Scientist at ESA•Holly R. Gilbert – Solar Orbiter Project Scientist at NASA•José Luis Pellón Bailón – Solar Orbiter Deputy Spacecraft Operations Manager at ESA•David Berghmans – Principal investigator of the Extreme Ultraviolet Imager (EUI) at the Royal Observatory of Belgium•Sami Solanki – Principal investigator of the Polarimetric and Helioseismic Imager (PHI) and director of the Max Planck Institute for Solar System Research•Christopher J. Owen – Principal investigator of the Solar Wind Analyser (SWA) at Mullard Space Science Laboratory, University College London•ESA’s first light images•ESA press release •NASA feature story || ", "hits": 247 }, { "id": 4715, "url": "https://svs.gsfc.nasa.gov/4715/", "result_type": "Visualization", "release_date": "2019-06-07T00:00:00-04:00", "title": "Swedish Solar Telescope: Solar Closeups", "description": "Close-up of Active Region 12593 through the 400 nm filter of the Swedish Solar Telescope. SDO/HMI provides the background image. || Sept2016_CHROMIS4000A_stand.HD1080i.00100_print.jpg (1024x576) [200.8 KB] || Sept2016_CHROMIS4000A_stand.HD1080i.00100_searchweb.png (180x320) [136.4 KB] || Sept2016_CHROMIS4000A_stand.HD1080i.00100_thm.png (80x40) [9.1 KB] || SwedishST (1920x1080) [0 Item(s)] || Sept2016_CHROMIS4000A.HD1080i_p30.mp4 (1920x1080) [19.4 MB] || Sept2016_CHROMIS4000A.HD1080i_p30.webm (1920x1080) [1.5 MB] || SwedishST (3840x2160) [0 Item(s)] || Sept2016_CHROMIS4000A.UHD3840_2160p30.mp4 (3840x2160) [50.6 MB] || Sept2016_CHROMIS4000A.HD1080i_p30.mp4.hwshow [199 bytes] || ", "hits": 163 }, { "id": 13166, "url": "https://svs.gsfc.nasa.gov/13166/", "result_type": "Produced Video", "release_date": "2019-04-09T17:00:00-04:00", "title": "Heliophysics Overview", "description": "Heliophysics is the study of the Sun, and how it influences the very nature of space — and, in turn, the atmospheres of planets and the technology that exists there. Space is not, as is often believed, completely empty; instead, we live in the extended atmosphere of an active star. Our Sun sends out a steady outpouring of particles and energy -- the solar wind – as well as a constantly writhing magnetic system. This extensive, dynamic solar atmosphere surrounds the Sun, Earth, the planets, and extends far out into the solar system.Studying this system not only helps us understand fundamental information about how the universe works, but also helps protect our technology and astronauts in space. NASA seeks knowledge of near-Earth space, because -- when extreme -- space weather can interfere with our communications, satellites and power grids. The study of the Sun and space can also teach us more about how stars contribute to the habitability of planets throughout the universe.Mapping out this interconnected system requires a holistic study of the Sun’s influence on space, Earth and other planets.  NASA has a fleet of spacecraft strategically placed throughout our heliosphere -- from Parker Solar Probe at the Sun observing the very start of the solar wind, to satellites around Earth, to the farthest human-made object, Voyager, which is sending back observations on interstellar space. Each mission is positioned at a critical, well-thought out vantage point to observe and understand the flow of energy and particles throughout the solar system -- all helping us untangle the effects of the star we live with. || ", "hits": 79 }, { "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": 60 }, { "id": 40355, "url": "https://svs.gsfc.nasa.gov/gallery/sdo/", "result_type": "Gallery", "release_date": "2018-08-31T00:00:00-04:00", "title": "SDO – Solar Dynamics Observatory", "description": "Since its launch on Feb. 11, 2010, the Solar Dynamics Observatory (SDO) has studied the solar atmosphere to help us understand the Sun’s influence on Earth. Every 12 seconds, SDO images the Sun in 10 wavelengths of ultraviolet light, each of which reveals different solar features. These images help us explain where the Sun's energy comes from, how the inside of the Sun works, and how the Sun’s atmosphere stores and releases energy in dramatic eruptions that can influence Earth.\n\nLearn more: https://science.nasa.gov/mission/sdo/", "hits": 571 }, { "id": 12903, "url": "https://svs.gsfc.nasa.gov/12903/", "result_type": "Produced Video", "release_date": "2018-07-25T14:00:00-04:00", "title": "Discovering the Sun’s Mysteriously Hot Atmosphere", "description": "Something mysterious is going on at the Sun. In defiance of all logic, its atmosphere gets much, much hotter the farther it stretches from the Sun’s blazing surface.Temperatures in the corona — the tenuous, outermost layer of the solar atmosphere — spike upwards of 2 million degrees Fahrenheit, while just 1,000 miles below, the underlying surface simmers at a balmy 10,000 F. How the Sun manages this feat remains one of the greatest unanswered questions in astrophysics; scientists call it the coronal heating problem. A new, landmark mission, NASA’s Parker Solar Probe — scheduled to launch no earlier than Aug. 11, 2018 — will fly through the corona itself, seeking clues to its behavior and offering the chance for scientists to solve this mystery.From Earth, as we see it in visible light, the Sun’s appearance — quiet, unchanging — belies the life and drama of our nearest star. Its turbulent surface is rocked by eruptions and intense bursts of radiation, which hurl solar material at incredible speeds to every corner of the solar system. This solar activity can trigger space weather events that have the potential to disrupt radio communications, harm satellites and astronauts, and at their most severe, interfere with power grids.Above the surface, the corona extends for millions of miles and roils with plasma, gases superheated so much that they separate into an electric flow of ions and free electrons. Eventually, it continues outward as the solar wind, a supersonic stream of plasma permeating the entire solar system. And so, it is that humans live well within the extended atmosphere of our Sun. To fully understand the corona and all its secrets is to understand not only the star that powers life on Earth, but also, the very space around us.Read more on NASA.gov. || ", "hits": 320 }, { "id": 12978, "url": "https://svs.gsfc.nasa.gov/12978/", "result_type": "Produced Video", "release_date": "2018-07-20T13:00:00-04:00", "title": "Parker Solar Probe--Mission Overview", "description": "Parker Solar Probe will swoop to within 4 million miles of the sun's surface, facing heat and radiation like no spacecraft before it. Launching in 2018, Parker Solar Probe will provide new data on solar activity and make critical contributions to our ability to forecast major space-weather events that impact life on Earth.In order to unlock the mysteries of the corona, but also to protect a society that is increasingly dependent on technology from the threats of space weather, we will send Parker Solar Probe to touch the Sun.In 2017, the mission was renamed for Eugene Parker, the S. Chandrasekhar Distinguished Service Professor Emeritus, Department of Astronomy and Astrophysics at the University of Chicago. In the 1950s, Parker proposed a number of concepts about how stars—including our Sun—give off energy. He called this cascade of energy the solar wind, and he described an entire complex system of plasmas, magnetic fields, and energetic particles that make up this phenomenon. Parker also theorized an explanation for the superheated solar atmosphere, the corona, which is – contrary to what was expected by physics laws -- hotter than the surface of the sun itself. This is the first NASA mission that has been named for a living individual. || a012978_ParkerThumbnail_print.jpg (1024x576) [115.8 KB] || a012978_ParkerThumbnail.png (2327x1311) [5.5 MB] || a012978_ParkerThumbnail_thm.png (80x40) [6.6 KB] || a012978_ParkerThumbnail_searchweb.png (320x180) [83.0 KB] || SVS_12978_PSP_OVERVIEW_PKG_FINAL_Version_twitter_720.mp4 (1920x1080) [58.8 MB] || SVS_12978_PSP_OVERVIEW_PKG_FINAL_Version_youtube_1080.webm (1920x1080) [103.7 MB] || 12978_PSP_Overview_MASTER_appletv_subtitles.m4v (1280x720) [151.8 MB] || 12978_PSP_Overview_MASTER_appletv.m4v (1280x720) [151.7 MB] || SVS_12978_PSP_OVERVIEW_PKG_FINAL_Version_large_mp4.mp4 (1920x1080) [261.7 MB] || SVS_12978_PSP_OVERVIEW_PKG_FINAL_Version_youtube_720.mp4 (1920x1080) [330.9 MB] || SVS_12978_PSP_OVERVIEW_PKG_FINAL_Version_youtube_1080.mp4 (1920x1080) [444.0 MB] || PSP_CC.en_US.srt [5.0 KB] || PSP_CC.en_US.vtt [5.0 KB] || 12978_PSP_Overview_MASTER_ipod_sm.mp4 (320x240) [46.0 MB] || SVS_12978_PSP_OVERVIEW_PKG_FINAL_Version_lowres.mp4 (480x272) [34.8 MB] || CH28_12978_PSP_Overview_MASTER_ch28.mov (1280x720) [2.3 GB] || SVS_12978_PSP_OVERVIEW_PKG_FINAL_Version.mov (1920x1080) [6.8 GB] || ", "hits": 234 }, { "id": 12992, "url": "https://svs.gsfc.nasa.gov/12992/", "result_type": "Produced Video", "release_date": "2018-07-05T11:00:00-04:00", "title": "Cutting-Edge Heat Shield Installed on NASA’s Parker Solar Probe", "description": "The launch of Parker Solar Probe, the mission that will get closer to the Sun than any human-made object has ever gone, is quickly approaching, and on June 27, 2018, Parker Solar Probe’s heat shield – called the Thermal Protection System, or TPS – was installed on the spacecraft. A mission sixty years in the making, Parker Solar Probe will make a historic journey to the Sun’s corona, a region of the solar atmosphere. With the help of its revolutionary heat shield, now permanently attached to the spacecraft in preparation for its August 2018 launch, the spacecraft’s orbit will carry it to within 4 million miles of the Sun's fiercely hot surface, where it will collect unprecedented data about the inner workings of the corona. The eight-foot-diameter heat shield will safeguard everything within its umbra, the shadow it casts on the spacecraft. At Parker Solar Probe’s closest approach to the Sun, temperatures on the heat shield will reach nearly 2,500 degrees Fahrenheit, but the spacecraft and its instruments will be kept at a relatively comfortable temperature of about 85 degrees Fahrenheit. The heat shield is made of two panels of superheated carbon-carbon composite sandwiching a lightweight 4.5-inch-thick carbon foam core. The Sun-facing side of the heat shield is also sprayed with a specially formulated white coating to reflect as much of the Sun’s energy away from the spacecraft as possible. The heat shield itself weighs only about 160 pounds – here on Earth, the foam core is 97% air. Because Parker Solar Probe travels so fast – 430,000 miles per hour at its closest approach to the Sun, fast enough to travel from Philadelphia to Washington, D.C., in about one second – the shield and spacecraft have to be light to achieve the needed orbit. The reinstallation of the Thermal Protection System – which was briefly attached to the spacecraft during testing at the Johns Hopkins Applied Physics Lab in Laurel, Maryland, in fall 2017 – marks the first time in months that Parker Solar Probe has been fully integrated. The heat shield and spacecraft underwent testing and evaluation separately at NASA’s Goddard Space Flight Center in Greenbelt, Maryland, before shipping out to Astrotech Space Operations in Titusville, Florida, in April 2018. With the recent reunification, Parker Solar Probe inches closer to launch and toward the Sun. Parker Solar Probe is part of NASA’s Living with a Star Program, or LWS, to explore aspects of the Sun-Earth system that directly affect life and society. LWS is managed by NASA Goddard for the Heliophysics Division of NASA’s Science Mission Directorate in Washington, D.C. The Johns Hopkins Applied Physics Laboratory manages the Parker Solar Probe mission for NASA. APL designed and built the spacecraft and will also operate it. || ", "hits": 179 }, { "id": 4653, "url": "https://svs.gsfc.nasa.gov/4653/", "result_type": "Visualization", "release_date": "2018-06-05T10:00:00-04:00", "title": "Parker Solar Probe and Solar Orbiter Trajectories", "description": "This visualization opens near Earth for the launch of Parker Solar Probe August 12, 2018. Then the camera moves around the Sun to match of with Earth again for the launch of Solar Orbiter in 2020. After that, the camera moves in a slow drift around the Sun as the orbits evolve. The Parker Solar Probe orbit fades out after the nominal end of mission in 2025. This version has longer orbit trails to better view orbit changes, and the red along the orbits indicate the nominal science operations portions of the missions. || ParkerAndSolarOrbiter.InnerTourDeluxe.HAE.AU.clockSlate_EarthTarget.HD1080i.02000_print.jpg (1024x576) [100.7 KB] || DeluxeTour (1920x1080) [0 Item(s)] || ParkerAndSolarOrbiter.InnerTourDeluxe.HD1080i_p30.webm (1920x1080) [17.6 MB] || ParkerAndSolarOrbiter.InnerTourDeluxe.HD1080i_p30.mp4 (1920x1080) [179.8 MB] || DeluxeTour (3840x2160) [0 Item(s)] || ParkerAndSolarOrbiter.InnerTourDeluxe_2160p30.mp4 (3840x2160) [489.0 MB] || ParkerAndSolarOrbiter.InnerTourDeluxe.HD1080i_p30.mp4.hwshow [270 bytes] || ParkerAndSolarOrbiter.InnerTourDeluxe_2160p30.mp4.hwshow [211 bytes] || ", "hits": 222 }, { "id": 12792, "url": "https://svs.gsfc.nasa.gov/12792/", "result_type": "Produced Video", "release_date": "2017-12-05T15:00:00-05:00", "title": "NASA's TSIS-1: Tracking Sun’s Power to Earth (Prelaunch Media Roll-Ins)", "description": "We live on a solar-powered planet. As we wake up in morning, the Sun peeks out over the horizon to shed light on us, blankets us with warmth, and provides cues to start our day. At the same time, the Sun’s energy drives our planet’s ocean currents, seasons, weather, and climate. Without the Sun, life on Earth would not exist. || ", "hits": 160 }, { "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": 52 }, { "id": 12706, "url": "https://svs.gsfc.nasa.gov/12706/", "result_type": "Produced Video", "release_date": "2017-09-06T11:00:00-04:00", "title": "A Powerful Sequence of Flares Start September 2017", "description": "Short video showing the sequence of M and X flares starting on September 4, 2017 and culminating with an X9.3 flare — the largest of the solar cycle.Music: \"Networked\" from Killer TracksWatch this video on the NASA Goddard YouTube channel.Complete transcript available. || SDO_Flare_Still_3.jpg (1920x1080) [326.8 KB] || 12706_SDO_September_2017_Flares_ProRes_1920x1080_2997.mov (1920x1080) [2.9 GB] || 12706_SDO_September_2017_Flares_H264_Best_1080.mov (1920x1080) [1.1 GB] || 12706_SDO_September_2017_Flares_H264_Good_1080.m4v (1920x1080) [223.8 MB] || 12706_SDO_September_2017_Flares_Compatible.m4v (960x540) [90.1 MB] || 12706_SDO_September_2017_Flares_Compatible.webm (960x540) [23.8 MB] || 12706_SDO_September_2017_Flares_SRT_Captions.en_US.srt [2.4 KB] || 12706_SDO_September_2017_Flares_SRT_Captions.en_US.vtt [2.3 KB] || ", "hits": 130 }, { "id": 12414, "url": "https://svs.gsfc.nasa.gov/12414/", "result_type": "Produced Video", "release_date": "2016-12-14T17:30:00-05:00", "title": "AGU 2017 Eclipse Press Conference", "description": "Graphic depicting the geometry of a total solar eclipse. Credit: NASA || Eclipse_Geometry.png (1158x548) [180.5 KB] || ", "hits": 40 }, { "id": 12390, "url": "https://svs.gsfc.nasa.gov/12390/", "result_type": "Produced Video", "release_date": "2016-10-17T16:00:00-04:00", "title": "NASA's STEREO Solar Probes 10th Anniversary Live Shots", "description": "B-roll that corresponds with the live shots. || B-Roll_2.00001_print.jpg (1024x576) [130.4 KB] || B-Roll_2.00001_searchweb.png (320x180) [78.8 KB] || B-Roll_2.00001_web.png (320x180) [78.8 KB] || B-Roll_2.00001_thm.png (80x40) [6.6 KB] || B-Roll.webm (1280x720) [19.6 MB] || B-Roll_2.webm (1280x720) [19.5 MB] || B-Roll_2.mov (1280x720) [3.1 GB] || ", "hits": 108 }, { "id": 12379, "url": "https://svs.gsfc.nasa.gov/12379/", "result_type": "Produced Video", "release_date": "2016-09-28T10:00:00-04:00", "title": "Space Radiation Highlights", "description": "A collection of space radiation highlights featuring:NASA's Van Allen ProbesNASA's CubeSats || ", "hits": 91 }, { "id": 12142, "url": "https://svs.gsfc.nasa.gov/12142/", "result_type": "Produced Video", "release_date": "2016-02-04T11:00:00-05:00", "title": "The Storm That Missed Earth", "description": "The big solar storm of 2012 was one for the record books. || c-1920.jpg (1920x1080) [858.4 KB] || c-1280.jpg (1280x720) [493.8 KB] || c-1024.jpg (1024x576) [333.3 KB] || c-1024_print.jpg (1024x576) [348.1 KB] || c-1024_searchweb.png (320x180) [115.4 KB] || c-1024_web.png (320x180) [115.4 KB] || c-1024_thm.png (80x40) [20.0 KB] || ", "hits": 334 }, { "id": 12074, "url": "https://svs.gsfc.nasa.gov/12074/", "result_type": "Produced Video", "release_date": "2015-12-03T13:00:00-05:00", "title": "20 Years In Space", "description": "The sun-observing SOHO spacecraft celebrates two decades of space-based science. || cf-1024.jpg (1024x576) [113.9 KB] || cf-1024_print.jpg (1024x576) [119.4 KB] || cf-1024_searchweb.png (320x180) [70.6 KB] || cf-1024_web.png (320x180) [70.6 KB] || cf-1024_thm.png (80x40) [16.1 KB] || ", "hits": 51 }, { "id": 4288, "url": "https://svs.gsfc.nasa.gov/4288/", "result_type": "Visualization", "release_date": "2015-06-10T00:00:00-04:00", "title": "The 2015 Earth-Orbiting Heliophysics Fleet", "description": "Movie showing the heliosphysics missions from near Earth orbit out to the orbit of the Moon.This video is also available on our YouTube channel. || Helio2015A.MMStour.slate_RigRHS.HD1080i.0500_print.jpg (1024x576) [112.6 KB] || Helio2015A.MMStour.HD1080.webm (1920x1080) [6.7 MB] || WithoutTimeStamp (1920x1080) [128.0 KB] || Helio2015A.MMStour.HD1080.mov (1920x1080) [196.3 MB] || Helio2015_4288.pptx [198.6 MB] || Helio2015_4288.key [201.3 MB] || ", "hits": 60 }, { "id": 11795, "url": "https://svs.gsfc.nasa.gov/11795/", "result_type": "Produced Video", "release_date": "2015-03-11T12:30:00-04:00", "title": "MMS L-1 Media Briefing", "description": "On March 12 from Cape Canaveral Florida, NASA is scheduled to launch the Magnetospheric Multiscale, or MMS, mission, which will provide unprecedented detail on a phenomenon called magnetic reconnection. The process of reconnection involves the explosive release of energy when the magnetic fields around Earth connect and disconnect. These fields help protect Earth from harmful effects of solar storms and cosmic rays. Magnetic reconnection also occurs throughout the universe and can accelerate particles up to nearly the speed of light.By studying reconnection in this local, natural laboratory, MMS helps us understand reconnection elsewhere as well, such as in the atmosphere of the Sun and other stars, in the vicinity of black holes and neutron stars, and at the boundary between our solar system’s heliosphere and interstellar space.MMS consists of four identical observatories that will provide the first three-dimensional view of magnetic reconnection. The four MMS observatories will fly through reconnection regions in a tight formation in well under a second, so key sensors on each spacecraft are designed to measure the space environment at rates faster than any previous mission.For additional visuals regarding the MMS mission and science, please see our MMS Pre-launch Gallery.Briefing participants include:Jeff Newmark, interim director, Heliophysics DivisionNASA Headquarters, WashingtonJim Burch, principal investigator, MMS instrument suite science teamSouthwest Research Institute, San AntonioRoy Torbert, MMS FIELDS investigation leadUniversity of New Hampshire, Durham, New HampshireCraig Pollock, lead co-investigator, MMS Fast Plasma Investigation Goddard Space Flight Center, Greenbelt, MarylandPaul Cassak, associate professorWest Virginia University, Morgantown || ", "hits": 28 }, { "id": 11737, "url": "https://svs.gsfc.nasa.gov/11737/", "result_type": "Produced Video", "release_date": "2015-02-05T11:00:00-05:00", "title": "Tracking Solar Eruptions", "description": "Explore how scientists trace the journey of material exploding from the sun. || c-1024.jpg (1024x576) [129.9 KB] || c-1920.jpg (1920x1080) [290.2 KB] || c-1280.jpg (1280x720) [181.0 KB] || c-1024_print.jpg (1024x576) [126.9 KB] || c-1024_searchweb.png (320x180) [78.3 KB] || c-1024_print_thm.png (80x40) [14.7 KB] || ", "hits": 107 }, { "id": 11739, "url": "https://svs.gsfc.nasa.gov/11739/", "result_type": "Produced Video", "release_date": "2015-01-20T11:00:00-05:00", "title": "Telescope on NASA's SDO Collects Its 100 Millionth Image", "description": "100 million images of the sun: The Advanced Imaging Assembly on NASA's Solar Dynamics Observatory captured its 100 millionth image of the sun on Jan. 19, 2015. The image shows the glow in the solar atmosphere of gases at about 1.5 million Kelvin. Credit: NASA/SDO/AIA/LMSAL || SDO_AIA_193_100Millionth_print.jpg (1024x1024) [168.6 KB] || SDO_AIA_193_100Millionth.jpeg (4096x4096) [2.4 MB] || SDO_AIA_193_100Millionth_web.jpg (320x320) [27.3 KB] || SDO_AIA_193_100Millionth_searchweb.png (320x180) [95.6 KB] || SDO_AIA_193_100Millionth_thm.png (80x40) [10.2 KB] || ", "hits": 104 }, { "id": 11708, "url": "https://svs.gsfc.nasa.gov/11708/", "result_type": "Produced Video", "release_date": "2014-10-16T14:00:00-04:00", "title": "NASA's IRIS Helps Explain Mysterious Heat of the Solar Atmosphere", "description": "This movie shows succeeding images from NASA’s IRIS of the same area of the sun in different wavelengths.  Each image carries information about how fast the solar material is moving, which has shown scientists that a series of loops are twisting in the sun’s lower atmosphere.Credit: NASA/IRIS/Pereira || S3_still.png (1534x1154) [1.1 MB] || S3_still_web.jpg (319x240) [22.4 KB] || S3_still_searchweb.png (320x180) [67.4 KB] || S3_still_thm.png (80x40) [8.5 KB] || S3.mov (768x576) [2.8 MB] || S3.webmhd.webm (960x540) [1.8 MB] || ", "hits": 113 }, { "id": 11642, "url": "https://svs.gsfc.nasa.gov/11642/", "result_type": "Produced Video", "release_date": "2014-09-23T11:45:00-04:00", "title": "Solar Edge", "description": "How big is the sun’s atmosphere? In a word: huge. Like Earth, the sun’s atmosphere consists of multiple layers. It has a lower atmosphere, called the chromosphere, and a significantly larger upper atmosphere, called the corona. Although the exact boundaries of these regions are fuzzy, the outer limit of the corona is marked by the place where the sun’s solar wind breaks free. Using NASA’s STEREO spacecraft, scientists have found the extent of the corona is greater than previously thought, stretching some five million miles from the surface. The distance is equivalent to approximately six times the sun's length. Knowing this information will help guide the planning of future sun-observing missions. Watch the video to see solar material streaming from the sun. || ", "hits": 32 }, { "id": 11613, "url": "https://svs.gsfc.nasa.gov/11613/", "result_type": "Produced Video", "release_date": "2014-08-01T10:00:00-04:00", "title": "EUNIS Sees Evidence for Nanoflare Heating", "description": "Scientists have recently gathered some of the strongest evidence to date to explain what makes the sun's outer atmosphere so much hotter than its surface. The new observations show temperatures in the atmosphere so hot that only one current theory explains them: something called nanoflares – a constant peppering of impulsive bursts of heating, none of which can be individually detected — provide the mysterious extra heat. These new observations come from just six minutes worth of data from one of NASA's least expensive type of missions, a sounding rocket. The EUNIS mission, short for Extreme Ultraviolet Normal Incidence Spectrograph, launched on April 23, 2013, gathering a new snapshot of data every 1.3 seconds to track the properties of material over a wide range of temperatures in the complex solar atmosphere. The unique capabilities of EUNIS enabled researchers to obtain these results. The spectrograph was able to clearly and unambiguously distinguish the observations representing the extremely hot material – emission lines showing light with a wavelength of 592.6 angstrom, where an angstrom is the size of an atom — from a very nearby light wavelength of 592.2 angstroms. || ", "hits": 55 }, { "id": 11586, "url": "https://svs.gsfc.nasa.gov/11586/", "result_type": "Produced Video", "release_date": "2014-07-15T11:00:00-04:00", "title": "Black Hole Sun", "description": "The sun’s magnetic field wreaks havoc on the solar atmosphere. At times the magnetic field lines that rise and fall from the surface in giant arcs can become detached at one end. When this happens, a ghostly patch develops in the sun’s upper atmosphere creating what’s known as a coronal hole. Viewed at certain wavelengths, the hole appears black as if it were empty. But, in fact, these holes are a source of strong solar wind, where streams of energized particles shoot out into space. If a hole points toward Earth, a bombardment of particles will reach the planet within two or three days, sometimes resulting in aurorae. NASA’s Solar Dynamics Observatory, or SDO, spacecraft has observed many coronal holes since its launch in 2010. Watch the video for a close look at one discovered in May 2014. || ", "hits": 939 }, { "id": 11537, "url": "https://svs.gsfc.nasa.gov/11537/", "result_type": "Produced Video", "release_date": "2014-05-22T00:00:00-04:00", "title": "Journey Of Light", "description": "The light that illuminates our planet is made deep inside the sun and takes some 40,000 years to travel through the sun’s layers. Particles of light form from atoms undergoing nuclear fusion in the sun’s innermost layer known as the core. The light then flows through the sun’s interior for millennia, slowly bubbling up like water in a boiling pot. It eventually bursts past the sun’s surface, called the photosphere, and rises into the solar atmosphere. Once in the atmosphere—made up of the chromosphere and corona—the light streams out through the solar system. Watch the video to see how light travels from the sun's interior to the surface. || ", "hits": 492 }, { "id": 11522, "url": "https://svs.gsfc.nasa.gov/11522/", "result_type": "Produced Video", "release_date": "2014-05-07T12:00:00-04:00", "title": "The Best Observed X-class Flare", "description": "On March 29, 2014 the sun released an X-class flare. It was observed by NASA's Interface Region Imaging Spectrograph, or IRIS; NASA's Solar Dynamics Observatory, or SDO; NASA's Reuven Ramaty High Energy Solar Spectroscopic Imager, or RHESSI; the Japanese Aerospace Exploration Agency's Hinode; and the National Solar Observatory's Dunn Solar Telescope located at Sacramento Peak in New Mexico. To have a record of such an intense flare from so many observatories is unprecedented. Such research can help scientists better understand what catalyst sets off these large explosions on the sun. Perhaps we may even some day be able to predict their onset and forewarn of the radio blackouts solar flares can cause near Earth – blackouts that can interfere with airplane, ship and military communications. || ", "hits": 87 }, { "id": 4164, "url": "https://svs.gsfc.nasa.gov/4164/", "result_type": "Visualization", "release_date": "2014-05-07T10:00:00-04:00", "title": "A Multi-Mission View of a Solar Flare: Optical to Gamma-rays", "description": "To improve our understanding of complex phenomena such as solar flares, a wide variety of tools are needed. In the case of astronomy, those tools enable us to analyze the light in many different wavelengths and many different ways.Many different instruments are observing the Sun almost continuously, both from space and on the surface of the Earth. On March 29, 2014, the Dunn Solar Telescope at Sacramento Peak, New Mexico was observing a solar active region and requested other observatories to watch as well. As a result of this coordination, the region was being observed by a large number of different instruments, ground and space-based, when it subsequently erupted with an X-class flare. This visualization presents various combinations of the datasets collected during this effort. The color text represents the dominant color of the dataset in the imagery.Solar Dynamics Observatory (SDO): HMI (617.1nm). This data represents the Sun is visible light similar to how we see it from the ground.Solar Dynamics Observatory (SDO): AIA (17.1nm). Solar ultraviolet emission, which can only be seen from space, reveals plasma flowing, and escaping, along magnetic fields.IRIS Slit-Jaw Imager: 140.0nm. This high-resolution imager also contains a slit (the dark vertical line in the center of the field) which directs the light to an ultraviolet spectrometer which is used to extract even more information about the light. The imager slews back-and-forth across the region, providing spectra over a larger area of the Sun.Hinode/X-ray Telescope: x-ray band. Indicates very hot plasma.RHESSI: 50-100 keV. High-energy gamma-ray emission. Emission from these locations represent the very highest energy photons from the flare event.Dunn Solar Telescope: G-band filter. This filter, showing much of the solar surface (photosphere) in visible light, provides a detailed view of the sunspots and convection cells. The view moves because the instrument was repointed several times during the observation.Dunn Solar Telescope: IBIS ( Hydrogen alpha, 656.3nm; Calcium 854.2 nm; Iron 630.15nm). This is the small rectangular view within the Dunn Solar Telescope G-band view. This instrument can tune the wavelength during the observation, which provides views of the solar atmosphere at different depths. || ", "hits": 38 }, { "id": 11136, "url": "https://svs.gsfc.nasa.gov/11136/", "result_type": "Produced Video", "release_date": "2014-01-07T16:00:00-05:00", "title": "Sun unleashes first X-class flare of 2014", "description": "The sun emitted a significant solar flare peaking at 1:32 p.m. EST on Jan.7, 2014. This is the first significant flare of 2014, and follows on the heels of mid-level flare earlier in the day. Each flare was centered over a different area of a large sunspot group currently situated at the center of the sun, about half way through its 14-day journey across the front of the disk along with the rotation of the sun. This flare is classified as an X1.2-class flare. X-class denotes the most intense flares, while the number provides more information about its strength. An X2 is twice as intense as an X1, an X3 is three times as intense, etc. || ", "hits": 67 }, { "id": 4128, "url": "https://svs.gsfc.nasa.gov/4128/", "result_type": "Visualization", "release_date": "2013-12-24T00:00:00-05:00", "title": "Solar Dynamics Observatory - Argo view - Slices of SDO", "description": "Argos (or Argus Panoptes) was the 100-eyed giant in Greek mythology (wikipedia).While the Solar Dynamics Observatory (SDO) has significantly less than 100 eyes, (see \"SDO Jewelbox: The Many Eyes of SDO\"), seeing connections in the solar atmosphere through the many filters of SDO presents a number of interesting challenges. This visualization experiment illustrates a mechanism for highlighting these connections. This visualization is a variation of the original Solar Dynamics Observatory - Argo view. In this case, the different wavelength filters are presented in three sets around the Sun at full 4Kx4K resolution. This enables monitoring of changes in time over all wavelengths at any location around the limb of the Sun. The wavelengths presented are: 617.3nm optical light from SDO/HMI. From SDO/AIA we have 170nm (pink), then 160nm (green), 33.5nm (blue), 30.4nm (orange), 21.1nm (violet), 19.3nm (bronze), 17.1nm (gold), 13.1nm (aqua) and 9.4nm (green).We've locked the camera to rotate the view of the Sun so each wedge-shaped wavelength filter passes over a region of the Sun. As the features pass from one wavelength to the next, we can see dramatic differences in solar structures that appear in different wavelengths.Filaments extending off the limb of the Sun which are bright in 30.4 nanometers, appear dark in many other wavelengths.Sunspots which appear dark in optical wavelengths, are festooned with glowing ribbons in ultraviolet wavelengths.small flares, invisible in optical wavelengths, are bright ribbons in ultraviolet wavelengths.if we compare the visible light limb of the Sun with the 170 nanometer filter on the left, with the visible light limb and the 9.4 nanometer filter on the right, we see that the 'edge' is at different heights. This effect is due to the different amounts of absorption, and emission, of the solar atmosphere in ultraviolet light.in far ultraviolet light, the photosphere is dark since the black-body spectrum at a temperature of 5700 Kelvin emits very little light in this wavelength. || ", "hits": 71 }, { "id": 4117, "url": "https://svs.gsfc.nasa.gov/4117/", "result_type": "Visualization", "release_date": "2013-12-17T10:00:00-05:00", "title": "Solar Dynamics Observatory - Argo view", "description": "Argos (or Argus Panoptes) was the 100-eyed giant in Greek mythology (wikipedia).While the Solar Dynamics Observatory (SDO) has significantly less than 100 eyes, (see \"SDO Jewelbox: The Many Eyes of SDO\"), seeing connections in the solar atmosphere through the many filters of SDO presents a number of interesting challenges. This visualization experiment illustrates a mechanism for highlighting these connections.The wavelengths presented are: 617.3nm optical light from SDO/HMI. From SDO/AIA we have 170nm (pink), then 160nm (green), 33.5nm (blue), 30.4nm (orange), 21.1nm (violet), 19.3nm (bronze), 17.1nm (gold), 13.1nm (aqua) and 9.4nm (green).We've locked the camera to rotate the view of the Sun so each wedge-shaped wavelength filter passes over a region of the Sun. As the features pass from one wavelength to the next, we can see dramatic differences in solar structures that appear in different wavelengths.Filaments extending off the limb of the Sun which are bright in 30.4 nanometers, appear dark in many other wavelengths.Sunspots which appear dark in optical wavelengths, are festooned with glowing ribbons in ultraviolet wavelengths.Small flares, invisible in optical wavelengths, are bright ribbons in ultraviolet wavelengths.If we compare the visible light limb of the Sun with the 170 nanometer filter on the left, with the visible light limb and the 9.4 nanometer filter on the right, we see that the 'edge' is at different heights. This effect is due to the different amounts of absorption, and emission, of the solar atmosphere in ultraviolet light.In far ultraviolet light, the photosphere is dark since the black-body spectrum at a temperature of 5700 Kelvin emits very little light in this wavelength. || ", "hits": 214 }, { "id": 4127, "url": "https://svs.gsfc.nasa.gov/4127/", "result_type": "Visualization", "release_date": "2013-12-16T12:00:00-05:00", "title": "The 2013 Earth-Orbiting Heliophysics Fleet", "description": "There've been a few changes since the 2012 Earth-Orbiting Heliophysics Fleet. As of Fall of 2013, here's a tour of the NASA Near-Earth Heliophysics fleet, covering the space from near-Earth orbit out to the orbit of the Moon.The satellite orbits are color coded for their observing program:Magenta: TIM (Thermosphere, Ionosphere, Mesosphere) observationsYellow: solar observations and imageryCyan: Geospace and magnetosphereViolet: Heliospheric observationsNear-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 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. SORCE: Monitors solar intensity across a broad range of the electromagnetic spectrum.AIM: Images and measures noctilucent clouds. SVS pageVan Allen Probes: Two probes moving along the same orbit esigned to study the impact of space weather on Earth's radiation belts. SVS pageTWINS: Two Wide-Angle Imaging Neutral-Atom Spectrometers (TWINS) are two probes observing the Earth with neutral atom imagers.IRIS: Interface Region Imaging Spectrograph is designed to take high-resolution spectra and images of the region between the solar photosphere and solar atmosphere.Geosynchronous Fleet:SDO: Solar Dynamics Observatory keeps the Sun under continuous observation at 16 megapixel resolution.GOES: The newest GOES satellites include a solar X-ray imager operated by NOAA.Geospace 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 three satellites to study how magnetospheric instabilities produce substorms. Two of the original five satellites were moved into lunar orbit to become ARTEMIS. SVS page IBEX: The Interstellar Boundary Explorer measures the flux of neutral atoms from the heliopause.Lunar Orbiting FleetARTEMIS: Two of the THEMIS satellites were moved into lunar orbit to study the interaction of the Earth's magnetosphere with the Moon. || ", "hits": 89 }, { "id": 11422, "url": "https://svs.gsfc.nasa.gov/11422/", "result_type": "Produced Video", "release_date": "2013-11-22T11:00:00-05:00", "title": "NASA's Solar Observing Fleet Watch Comet ISON's Journey Around the Sun", "description": "After several days of continued observations, scientists continue to work to determine and to understand the fate of Comet ISON: There's no doubt that the comet shrank in size considerably as it rounded the sun and there's no doubt that something made it out on the other side to shoot back into space. The question remains as to whether the bright spot seen moving away from the sun was simply debris, or whether a small nucleus of the original ball of ice was still there. Regardless, it is likely that it is now only dust. The comet was visible in instruments on NASA's Solar Terrestrial Relations Observatory, or STEREO, and the joint European Space Agency/NASA Solar and Heliospheric Observatory, or SOHO, via images called coronagraphs.Watch this video on the NASA Goddard YouTube channel.Credit:NASA/STEREO/ESA/SOHO/SDOGSFC || STEREO_A_Cor2_Still.jpg (1280x720) [494.6 KB] || STEREO_A_Cor2_Still_web.png (320x180) [67.2 KB] || ISON_Full_FINAL_1280x720.wmv (1280x720) [49.4 MB] || ISON_Full_FINAL_appletv.m4v (960x540) [46.4 MB] || ISON_Full_H264_1280x720_30.mov (1280x720) [43.1 MB] || ISON_Full_MPEG4_1280X720_29.97.mp4 (1280x720) [28.0 MB] || ISON_Full_FINAL_appletv.webmhd.webm (960x540) [16.6 MB] || ISON_Full_FINAL_ipod_lg.m4v (640x360) [17.5 MB] || ISON_Full_FINAL.mp4 (320x240) [8.3 MB] || ISON_Full_FINAL_ipod_sm.mp4 (320x240) [8.3 MB] || ISON_Full_ProRes_1280x720_29.97.mov (1280x720) [810.6 MB] || ISON_Full_H264_Best_1280x720_29.97.mov (1280x720) [517.2 MB] || ISON_Full_H264_Good_1280x720_29.97.mov (1280x720) [124.1 MB] || ISON_Full_FINAL_youtube_hq.mov (1280x720) [124.1 MB] || ", "hits": 77 }, { "id": 11384, "url": "https://svs.gsfc.nasa.gov/11384/", "result_type": "Produced Video", "release_date": "2013-11-21T14:00:00-05:00", "title": "How to Cook a Comet", "description": "A comet's journey through the solar syste is perilous and violent. Before it reaches Mars - at some 230 million miles away from the sun - the radiation of the sun begins to cook off the frozen water ice directly into gas. This is called sublimation. It is the first step toward breaking the comet apart. If it survives this, the intense radiation and pressure closer to the sun could destroy it altogether.Animators at NASA's Goddard Space Flight Center in Greenbelt, Md. created this short movie showing how the sun can cook a comet. Such a journey is currently being made by Comet ISON. It began its trip from the Oort cloud region of our solar system and is now traveling toward the sun. The comet will reach its closest approach to the sun on Thanksgiving Day — Nov. 28, 2013 — skimming just 730,000 miles above the sun’s surface. If it comes around the sun without breaking up, the comet will be visible in the Northern Hemisphere with the naked eye, and from what we see now, ISON is predicted to be a particularly bright and beautiful comet. Even if the comet does not survive, tracking its journey will help scientists understand what the comet is made of, how it reacts to its environment, and what this explains about the origins of the solar system. Closer to the sun, watching how the comet and its tail interact with the vast solar atmosphere can teach scientists more about the sun itself. || ", "hits": 62 }, { "id": 30081, "url": "https://svs.gsfc.nasa.gov/30081/", "result_type": "Hyperwall Visual", "release_date": "2013-10-10T00:00:00-04:00", "title": "Stereo Captures Eruption and CME", "description": "On May 1, 2013, NASA's Solar Terrestrial Relations Observatory Ahead (STEREO-A) satellite along with its twin STEREO Behind (STEREO-B), observed an active region (right) of the sun erupt. This eruption, called a coronal mass ejection, or CME, sent plasma streaming out through the solar system. STEREO has an extreme ultraviolet camera similar to the Solar Dynamics Observatory (SDO) satellite, but it also has coronagraph telescopes like the European Space Agency/NASA Solar and Heliospheric Observatory (SOHO) where the bright sun is blocked by a disk so it does not overpower the fainter solar atmosphere. As a result, using its two inner coronagraphs, STEREO was able to track the CME from the solar surface out to 6.3 million miles. || ", "hits": 58 }, { "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": 11313, "url": "https://svs.gsfc.nasa.gov/11313/", "result_type": "Produced Video", "release_date": "2013-07-19T09:00:00-04:00", "title": "IRIS Launch", "description": "NASA's Interface Region Imaging Spectrograph (IRIS) solar observatory separated from its Pegasus rocket and is in the proper orbit. This followed a successful launch by the Orbital Sciences Pegasus XL rocket from Vandenberg Air Force Base, Calif. It was the final Pegasus launch currently manifested by NASA. NASA's Launch Services Program at the agency's Kennedy Space Center in Florida managed the countdown and launch.IRIS is a NASA Small Explorer Mission to observe how solar material moves, gathers energy and heats up as it travels through a little-understood region in the sun's lower atmosphere. This interface region between the sun's photosphere and corona powers its dynamic million-degree atmosphere and drives the solar wind.NASA's Interface Region Imaging Spectrograph (IRIS) spacecraft launched Wednesday at 7:27 p.m. PDT (10:27 p.m. EDT) from Vandenberg Air Force Base, Calif. The mission to study the solar atmosphere was placed in orbit by an Orbital Sciences Corporation Pegasus XL rocket. || ", "hits": 56 }, { "id": 11256, "url": "https://svs.gsfc.nasa.gov/11256/", "result_type": "Produced Video", "release_date": "2013-06-19T07:00:00-04:00", "title": "IRIS: Studying the Energy Flow that Powers the Solar Atmosphere", "description": "In late June 2013, the Interface Region Imaging Spectrograph, or IRIS, will launch from Vandenberg Air Force Base, Calif. IRIS will tease out the rules governing the lowest layers of the solar atmosphere — historically some of the hardest to untangle. Known as the solar interface region, this is one of the most complex areas in the sun's atmosphere: all the energy that drives solar activity travels through it. The interface region lies between the sun’s 6,000-degree, white-hot, visible surface, the photosphere, and the much hotter multi-million-degree upper corona. Interactions between the violently moving plasma and the sun’s magnetic field in this area may well be the source of the energy that heats the corona to its million-degree temperatures, some hundreds and occasionally thousands of times hotter than the sun's surface. The chromosphere is also considered a candidate as the origin for giant explosions on the sun such as solar flares and coronal mass ejections. IRIS will use high-resolution images, data and advanced computer models to unravel how solar gases move, gather energy and heat up through the lower solar atmosphere. Outfitted with state-of-the-art tools, IRIS will be able to tease apart what's happening in the solar interface region better than ever before. || ", "hits": 79 }, { "id": 11286, "url": "https://svs.gsfc.nasa.gov/11286/", "result_type": "Produced Video", "release_date": "2013-06-04T12:00:00-04:00", "title": "IRIS L-14 Media Briefing", "description": "Lying just above the sun's surface is an enigmatic region of the solar atmosphere called the interface region. A relatively thin region, just 3,000 to 6,000 miles thick, it pulses with movement: zones of different temperature and density are scattered throughout, while energy and heat course through the solar material. Understanding how the energy travels through this region – energy that helps heat the upper layer of the atmosphere, the corona, to temperatures of 1,000,000 kelvins, some thousand times hotter than the sun’s surface itself – is the goal of NASA's Interface Region Imaging Spectrograph, or IRIS, scheduled to launch on June 26, 2013 from California's Vandenberg Air Force Base. Scientists wish to understand the interface region in exquisite detail, since energy flowing through this region has an effect on so many aspects of near-Earth space. For one thing, despite the intense amount of energy deposited into the interface region, only a fraction leaksthrough, but this fraction drives the solar wind, the constant stream of particles that flows out to fill the entire solar system. The interface region is also the source of most of the sun's ultraviolet emission, which impacts both the near-Earth space environment and Earth's climate. IRIS's capabilities are uniquely tailored to unravel the interface region by providing both high-resolution images and a kind of data known as spectra, which can see many wavelengths at once. For its high-resolution images, IRIS will capture data on about one percent of the sun at a time. While these are relatively small snapshots, IRIS will be able to see very fine features, as small as 150 miles across. || ", "hits": 64 }, { "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": 108 }, { "id": 11257, "url": "https://svs.gsfc.nasa.gov/11257/", "result_type": "Produced Video", "release_date": "2013-04-26T16:00:00-04:00", "title": "CMEs Galore", "description": "On April 20, 2013, at 2:54 a.m. EDT, the sun erupted with a coronal mass ejection (CME), a solar phenomenon that can send billions of tons of solar particles into space that can affect electronic systems in satellites. Experimental NASA research models show that the CME left the sun at 500 miles per second and is not Earth-directed. However, it may pass by NASA's Messenger and STEREO-A satellites, and their mission operators have been notified. There is, however, no particle radiation associated with this event, which is what would normally concern operators of interplanetary spacecraft since the particles can trip computer electronics on board. When warranted, NASA operators can put spacecraft into safe mode to protect the instruments from the solar material. The same region of the sun erupted with another coronal mass ejection (CME) at 3:54 a.m. on April 21, 2013. Experimental NASA research models show the CME left the sun at speeds of 550 miles per second. The models show that the CME will also pass by NASA's Messenger and the flank of the CME may graze STEREO-A.Another coronal mass ejection (CME) has erupted from the sun, headed toward Mercury and NASA's Messenger spacecraft. The CME began at 12:39 p.m. EDT on April 21, 2013. Experimental NASA research models show that the CME left the sun at 625 miles per second and that it will catch up to the CME from earlier on April 21 before the combined CMEs pass Messenger. There is also chance that the combined CMEs will give a glancing blow to STEREO-A. || ", "hits": 224 }, { "id": 11183, "url": "https://svs.gsfc.nasa.gov/11183/", "result_type": "Produced Video", "release_date": "2013-02-07T00:00:00-05:00", "title": "Sharper Image", "description": "On July 11, 2012, NASA launched a sounding rocket that carried a solar telescope on a 620-second flight to space and back. About a minute into the ride, the rocket—called Hi-C, for High-Resolution Coronal imager—reached an altitude where Earth's atmosphere no longer blocked the extreme ultraviolet light the telescope was designed to observe. From this vantage point, Hi-C snapped images that revealed the dynamic structure of the super-hot solar atmosphere in five times sharper detail than ever before. Hi-C captured details 135 miles across; the previous record-holder, NASA's Solar Dynamics Observatory (SDO), captures details about 675 miles across. Watch the video to see a side-by-side comparison of imagery from Hi-C and SDO. || ", "hits": 36 }, { "id": 11145, "url": "https://svs.gsfc.nasa.gov/11145/", "result_type": "Produced Video", "release_date": "2013-02-06T10:00:00-05:00", "title": "Counting Comets", "description": "As comets orbit the sun, many come too close and evaporate completely. Others survive the journey, but their orbits gradually move closer to the sun. Ultimately, the heat of the solar atmosphere melts the ice that binds a comet together and breaks it apart into smaller bodies that follow similar orbits. These are the sungrazers, and scientists and amateur astronomers are seeing more of them than ever. As of 1979, we only knew of a dozen. Nearing the end of 2012, thanks to better observation tools, we have now seen 3,000. The bulk of the sungrazers are known as Kreutz comets, and are likely derived from a single original comet observed as early as 371 AD. Watch the videos to learn more about and see NASA satellite footage of sungrazing comets. || ", "hits": 42 }, { "id": 11150, "url": "https://svs.gsfc.nasa.gov/11150/", "result_type": "Produced Video", "release_date": "2013-01-01T00:00:00-05:00", "title": "Space Weather Forecast", "description": "The sun goes through a natural cycle approximately every 11 years, hitting peaks and valleys of solar activity. The cycle is marked by the increase and decrease of sunspots—visible as dark blemishes on the sun's surface and connected to eruptions such as solar flares and coronal mass ejections. The largest number of sunspots in any given solar cycle is designated as \"solar maximum,\" and this next peak of activity is predicted to occur in 2013. The eruptions that occur during solar maximum can't harm humans on Earth. But scientists observe this activity, what they call space weather, because it can affect satellites in orbit and disrupt power grids on the ground. Watch the movie to see the kind of gigantic, and often beautiful, eruptions we expect to see more of in 2013. || ", "hits": 49 }, { "id": 11072, "url": "https://svs.gsfc.nasa.gov/11072/", "result_type": "Produced Video", "release_date": "2012-11-26T10:00:00-05:00", "title": "SDO Solar Comparison October 2010 to October 2012", "description": "The sun goes through a natural solar cycle approximately every 11 years. The cycle is marked by the increase and decrease of sunspots — visible as dark blemishes on the sun's surface, or photosphere. The greatest number of sunspots in any given solar cycle is designated as \"solar maximum.\" The lowest number is \"solar minimum.\" The solar cycle provides more than just increased sunspots, however. In the sun's atmosphere, or corona, bright active regions appear, which are rooted in the lower sunspots. Scientists track the active regions since they are often the origin of eruptions on the sun such as solar flares or coronal mass ejections. The most recent solar minimum occurred in 2008, and the sun began to ramp up in January 2010, with an M-class flare (a flare that is 10 times less powerful than the largest flares, labeled X-class). The sun has continued to get more active, with the next solar maximum predicted for 2013. The journey toward solar maximum is evident in current images of the sun, showing a marked difference from those of 2010, with bright active regions dotted around the star. || ", "hits": 80 }, { "id": 11089, "url": "https://svs.gsfc.nasa.gov/11089/", "result_type": "Produced Video", "release_date": "2012-10-18T14:00:00-04:00", "title": "IRIS Launch, Deploy and Beauty Passes", "description": "Understanding the interface between the photosphere and corona remains a fundamental challenge in solar and heliospheric science. The Interface Region Imaging Spectrograph (IRIS) mission opens a window of discovery into this crucial region by tracing the flow of energy and plasma through the chromosphere and transition region into the corona using spectrometry and imaging. IRIS is designed to provide significant new information to increase our understanding of energy transport into the corona and solar wind and provide an archetype for all stellar atmospheres. The unique instrument capabilities, coupled with state of the art 3-D modeling, will fill a large gap in our knowledge of this dynamic region of the solar atmosphere. The mission will extend the scientific output of existing heliophysics spacecraft that follow the effects of energy release processes from the sun to Earth.IRIS will provide key insights into all these processes, and thereby advance our understanding of the solar drivers of space weather from the corona to the far heliosphere, by combining high-resolution imaging and spectroscopy for the entire chromosphere and adjacent regions. IRIS will resolve in space, time, and wavelength the dynamic geometry from the chromosphere to the low-temperature corona to shed much-needed light on the physics of this magnetic interface region. || ", "hits": 44 }, { "id": 11112, "url": "https://svs.gsfc.nasa.gov/11112/", "result_type": "Produced Video", "release_date": "2012-10-18T12:00:00-04:00", "title": "Gradient Sun", "description": "Watching a particularly beautiful movie of the sun helps show how the lines between science and art can sometimes blur. But there is more to the connection between the two disciplines: science and art techniques are often quite similar, indeed one may inform the other or be improved based on lessons from the other arena. One such case is a technique known as a \"gradient filter\" — recognizable to many people as an option available on a photo-editing program. Gradients are, in fact, a mathematical description that highlights the places of greatest physical change in space. A gradient filter, in turn, enhances places of contrast, making them all the more obviously different, a useful tool when adjusting photos. Scientists, too, use gradient filters to enhance contrast, using them to accentuate fine structures that might otherwise be lost in the background noise. On the sun, for example, scientists wish to study a phenomenon known as coronal loops, which are giant arcs of solar material constrained to travel along that particular path by the magnetic fields in the sun's atmosphere. Observations of the loops, which can be more or less tangled and complex during different phases of the sun's 11-year activity cycle, can help researchers understand what's happening with the sun's complex magnetic fields, fields that can also power great eruptions on the sun such as solar flares or coronal mass ejections. The images here show an unfiltered image from the sun next to one that has been processed using a gradient filter. Note how the coronal loops are sharp and defined, making them all the more easy to study. On the other hand, gradients also make great art. Watch the movie to see how the sharp loops on the sun next to the more fuzzy areas in the lower solar atmosphere provide a dazzling show. || ", "hits": 50 }, { "id": 3966, "url": "https://svs.gsfc.nasa.gov/3966/", "result_type": "Visualization", "release_date": "2012-09-20T00:00:00-04:00", "title": "Heliospheric Future: Parker Solar Probe (formerly Solar Probe Plus) & Solar Orbiter", "description": "Two future missions scheduled for detailed studies of the Sun and solar atmosphere are Parker Solar Probe and Solar Orbiter.Parker Solar Probe will move in a highly-elliptical orbit, using gravity-assists from Venus to move it closer to the Sun with each pass. The goal is to get the spacecraft to fly through the corona at a distance of 9.5 solar radii.Solar Orbiter will use Earth and Venus gravity assists to move into a relatively circular orbit, inside the orbit of Mercury for monitoring the Sun. || ", "hits": 64 }, { "id": 3965, "url": "https://svs.gsfc.nasa.gov/3965/", "result_type": "Visualization", "release_date": "2012-07-20T00:00:00-04:00", "title": "Impressionist Sun: SDO Source Images", "description": "A set of multi-wavelength views of the Sun from SDO provided source and context imagery for the Van Gogh Sun video. This video illustrates how imagery is converted into physical parameters teaching us more about the physical processes taking place in the solar atmosphere. || ", "hits": 43 }, { "id": 10990, "url": "https://svs.gsfc.nasa.gov/10990/", "result_type": "Produced Video", "release_date": "2012-05-23T14:00:00-04:00", "title": "Incandescent Sun", "description": "This video takes SDO images and applies additional processing to enhance the structures visible. While there is no scientific value to this processing, it does result in a beautiful, new way of looking at the sun. The original frames are in the 171 angstrom wavelength of extreme ultraviolet. This wavelength shows plasma in the solar atmosphere, called the corona, that is around 600,000 Kelvin. The loops represent plasma held in place by magnetic fields. They are concentrated in \"active regions\" where the magnetic fields are the strongest. These active regions usually appear in visible light as sunspots. The events in this video represent 24 hours of activity on September 25, 2011. || ", "hits": 48 }, { "id": 40115, "url": "https://svs.gsfc.nasa.gov/gallery/space-weather/", "result_type": "Gallery", "release_date": "2011-12-01T00:00:00-05:00", "title": "Space Weather", "description": "The term \"space weather\" was coined not long ago to describe the dynamic conditions in the Earth's outer space environment, in the same way that \"weather\" and \"climate\" refer to conditions in Earth's lower atmosphere. Space weather includes any and all conditions and events on the sun, in the solar wind, in near-Earth space and in our upper atmosphere that can affect space-borne and ground-based technological systems and through these, human life and endeavor. Heliophysics is the science of space weather.\r\n\r\nThis gallery organizes satellite footage, animations, visualizations, and edited videos produced at the Goddard Space Flight Center. Visualizations are different from pure animations because they are data-driven. They present a way of \"seeing\" the data. In the case of orbit visualizations, they are based on actual orbit information. Most of the animations and visualizations are available as frames and all the recent ones are HD quality. All videos are available in several formats and qualities including Apple ProRes for broadcast quality. Unless specifically marked otherwise, all these materials are public domain and free to use. For more infomation about NASA's media use guidelines see this page.\r\n\r\nThe content is organized in two ways. Under \"Facets of Space Weather\" you will find our visuals grouped by the subject they address. Under \"NASA Spacecraft\" you will find our visuals grouped by the satellite they were collected by, or that they refer to. This group also contains animations of the spacecraft themselves.\r\nFor breaking news solar events, go to this gallery.For frequently-asked-question interviews with NASA scientists, go here.", "hits": 162 }, { "id": 10817, "url": "https://svs.gsfc.nasa.gov/10817/", "result_type": "Produced Video", "release_date": "2011-09-07T12:00:00-04:00", "title": "SDO EVE Late Phase Flares", "description": "Scientists have been seeing just the tip of the iceberg when monitoring flares with X-rays. With the complete extreme ultraviolet (EUV) coverage by the SDO EUV Variability Experiment (EVE), they have observed enhanced EUV radiation that appears not only during the X-ray flare, but also a second time delayed by many minutes after the X-ray flare peak. These delayed, second peaks are referred to as the EUV Late Phase contribution to flares.The solar EUV radiation creates our Earth's ionosphere (plasma in our atmosphere), so solar flares disturb our ionosphere and consequently our communication and navigation technologies, such as Global Positioning System (GPS), that transmit through the ionosphere. For over 30 years, scientists have relied on the GOES X-ray monitor to tell them when to expect disturbances to our ionosphere. With these new SDO EVE results, they now recognize that additional ionospheric disturbances from these later EUV enhancements are also a concern. || ", "hits": 69 }, { "id": 3832, "url": "https://svs.gsfc.nasa.gov/3832/", "result_type": "Visualization", "release_date": "2011-08-02T00:00:00-04:00", "title": "Extreme Solar Eruption Caught On Camera", "description": "A massive spray of high-energy particles blasted from the sun and shot into space during a magnificent solar eruption captured by NASA's Solar Dynamics Observatory (SDO) satellite. The spectacular event took place on June 7, 2011 over a period of six hours when an M-2 class (medium-sized) solar flare, a large prominence eruption, and a coronal mass ejection were observed from sunspot complex 1226-1227. Scientists estimate hot plasma and powerful X-rays burst into the sun's atmosphere and exited the corona at speeds over 3 million mph. Trapped particles unable to reach escape velocity traversed the solar sky in evanescent arcs, some traveling more than 215,000 miles, and showered the surface in a speckled array of bright flashes as the fiery sphere reheated the slightly cooled material. The Atmospheric Imaging Assembly instrument on SDO recorded the event at multiple wavelengths using its extreme UV sensor and transmitted the images to Earth in awesome 16.8 mega-pixel resolution. Watch a time-lapse video of the eruption below and relive the moment. || ", "hits": 83 }, { "id": 10745, "url": "https://svs.gsfc.nasa.gov/10745/", "result_type": "Produced Video", "release_date": "2011-06-07T09:00:00-04:00", "title": "SDO Catches Surf Waves on the Sun", "description": "Scientists have spotted the iconic surfer's wave rolling through the atmosphere of the sun. This makes for more than just a nice photo-op: the waves hold clues as to how energy moves through that atmosphere, known as the corona. Since scientists know how these kinds of waves — initiated by a Kelvin-Helmholtz instability if you're being technical — disperse energy in the water, they can use this information to better understand the corona. This in turn, may help solve an enduring mystery of why the corona is thousands of times hotter than originally expected.Kelvin-Helmholtz instabilities occur when two fluids of different densities or different speeds flow by each other. In the case of ocean waves, that's the dense water and the lighter air. As they flow past each other, slight ripples can be quickly amplified into the giant waves loved by surfers. In the case of the solar atmosphere, which is made of a very hot and electrically charged gas called plasma, the two flows come from an expanse of plasma erupting off the sun's surface as it passes by plasma that is not erupting. The difference in flow speeds and densities across this boundary sparks the instability that builds into the waves. In order to confirm this description, the team developed a computer model to see what takes place in the region. Their model showed that these conditions could indeed lead to giant surfing waves rolling through the corona. Seeing the big waves suggests they can cascade down to smaller forms of turbulence too. Scientists believe that the friction created by turbulence — the simple rolling of material over and around itself — could help add heating energy to the corona. The analogy is the way froth at the top of a surfing wave provides friction that will heat up the wave. || ", "hits": 54 }, { "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": 110 }, { "id": 40062, "url": "https://svs.gsfc.nasa.gov/gallery/computer-modeling/", "result_type": "Gallery", "release_date": "2010-03-08T00:00:00-05:00", "title": "Computer Modeling", "description": "No description available.", "hits": 32 }, { "id": 40046, "url": "https://svs.gsfc.nasa.gov/gallery/nasas-heliophysics-gallery/", "result_type": "Gallery", "release_date": "2010-03-04T00:00:00-05:00", "title": "NASA's Heliophysics Gallery", "description": "Heliophysics studies the nature of the Sun and how it influences the very nature of space and the planets and the technology that exists there. Learn more at nasa.gov/sun.", "hits": 284 }, { "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": 35 }, { "id": 20118, "url": "https://svs.gsfc.nasa.gov/20118/", "result_type": "Animation", "release_date": "2007-09-10T00:00:00-04:00", "title": "The Solar Dynamics Observatory (SDO)", "description": "SDO is designed to help us understand the Sun's influence on Earth and Near-Earth space by studying the solar atmosphere on small scales of space and time and in many wavelengths simultaneously. || ", "hits": 100 }, { "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": 36 }, { "id": 111, "url": "https://svs.gsfc.nasa.gov/111/", "result_type": "Visualization", "release_date": "1996-12-12T12:00:00-05:00", "title": "Numerical Simulation of Magnetic Flux Emerging Through a Model Solar Atmosphere: Density", "description": "This animation is one of a series depicting the results of a two-dimensional ideal magnetohydrodynamic simulation of magnetic flux emerging through a solar atmosphere. The simulation has a resolution of 300x500 cells and a length scale of 16 Mm x 6.8 Mm. The simulation depicts 1730 seconds in the evolution of the model. || ", "hits": 60 }, { "id": 112, "url": "https://svs.gsfc.nasa.gov/112/", "result_type": "Visualization", "release_date": "1996-12-12T12:00:00-05:00", "title": "Numerical Simulation of Magnetic Flux Emerging Through a Model Solar Atmosphere: Density Gradient", "description": "This animation is one of a series depicting the results of a two-dimensional ideal magnetohydrodynamic simulation of magnetic flux emerging through a solar atmosphere. The simulation has a resolution of 300x500 cells and a length scale of 16 Mm x 6.8 Mm. The simulation depicts 1730 seconds in the evolution of the model. || ", "hits": 46 }, { "id": 113, "url": "https://svs.gsfc.nasa.gov/113/", "result_type": "Visualization", "release_date": "1996-12-12T12:00:00-05:00", "title": "Numerical Simulation of Magnetic Flux Emerging Through a Model Solar Atmosphere: Density, Magnetic Field, and Mach Number", "description": "This animation is one of a series depicting the results of a two-dimensional ideal magnetohydrodynamic simulation of magnetic flux emerging through a solar atmosphere. The simulation has a resolution of 300x500 cells and a length scale of 16 Mm x 6.8 Mm. The simulation depicts 1730 seconds in the evolution of the model. || ", "hits": 13 }, { "id": 114, "url": "https://svs.gsfc.nasa.gov/114/", "result_type": "Visualization", "release_date": "1996-12-12T12:00:00-05:00", "title": "Numerical Simulation of Magnetic Flux Emerging Through a Model Solar Atmosphere: Density Gradient, Magnetic Field, and Mach Number", "description": "This animation is one of a series depicting the results of a two-dimensional ideal magnetohydrodynamic simulation of magnetic flux emerging through a solar atmosphere. The simulation has a resolution of 300x500 cells and a length scale of 16 Mm x 6.8 Mm. The simulation depicts 1730 seconds in the evolution of the model. || ", "hits": 48 }, { "id": 115, "url": "https://svs.gsfc.nasa.gov/115/", "result_type": "Visualization", "release_date": "1996-12-12T12:00:00-05:00", "title": "Numerical Simulation of Magnetic Flux Emerging Through a Model Solar Atmosphere: Density Gradient and Velocities", "description": "This animation is one of a series depicting the results of a two-dimensional ideal magnetohydrodynamic simulation of magnetic flux emerging through a solar atmosphere. The simulation has a resolution of 300x500 cells and a length scale of 16 Mm x 6.8 Mm. The simulation depicts 1730 seconds in the evolution of the model. || ", "hits": 38 }, { "id": 107, "url": "https://svs.gsfc.nasa.gov/107/", "result_type": "Visualization", "release_date": "1996-05-21T12:00:00-04:00", "title": "High Resolution 2-D Numerical Simulation of Emergence of Magnetic Flux Through the Solar Atmosphere", "description": "This series of animations (animations 107, 1416, 1417, and 1418) show sheets of magnetic flux undergoing velocity perturbations. The conditions for each simulation are outlined within the video. || ", "hits": 45 }, { "id": 1416, "url": "https://svs.gsfc.nasa.gov/1416/", "result_type": "Visualization", "release_date": "1996-05-21T12:00:00-04:00", "title": "High Resolution 2-D Numerical Simulation of Emergence of Magnetic Flux Through the Solar Atmosphere", "description": "This series of animations (animations 107, 1416, 1417, and 1418) show sheets of magnetic flux undergoing velocity perturbations. The conditions for each simulation are outlined within the video. || ", "hits": 0 }, { "id": 1417, "url": "https://svs.gsfc.nasa.gov/1417/", "result_type": "Visualization", "release_date": "1996-05-21T12:00:00-04:00", "title": "High Resolution 2-D Numerical Simulation of Emergence of Magnetic Flux Through the Solar Atmosphere", "description": "This series of animations (animations 107, 1416, 1417, and 1418) show sheets of magnetic flux undergoing velocity perturbations. The conditions for each simulation are outlined within the video. || ", "hits": 8 }, { "id": 1418, "url": "https://svs.gsfc.nasa.gov/1418/", "result_type": "Visualization", "release_date": "1996-05-21T12:00:00-04:00", "title": "High Resolution 2-D Numerical Simulation of Emergence of Magnetic Flux Through the Solar Atmosphere", "description": "This series of animations (animations 107, 1416, 1417, and 1418) show sheets of magnetic flux undergoing velocity perturbations. The conditions for each simulation are outlined within the video. || ", "hits": 5 } ] }