{ "count": 59, "next": null, "previous": null, "results": [ { "id": 14954, "url": "https://svs.gsfc.nasa.gov/14954/", "result_type": "Produced Video", "release_date": "2026-01-23T09:00:00-05:00", "title": "NASA's Illuminate Series (2026)", "description": "NASA's Illuminate is a video series about out-of-this-world images that shine light on our Sun and solar system. || ", "hits": 202 }, { "id": 14895, "url": "https://svs.gsfc.nasa.gov/14895/", "result_type": "Produced Video", "release_date": "2025-09-17T10:00:00-04:00", "title": "Mapping the Boundaries of Our Home in Space with NASA’s IMAP Mission", "description": "NASA’s new Interstellar Mapping and Acceleration Probe, or IMAP, will explore and map the very boundaries of our heliosphere — a huge bubble created by the Sun's wind that encapsulates our solar system — and study how that boundary interacts with the local galactic neighborhood beyond.As a modern-day celestial cartographer, IMAP will chart the vast range of particles in interplanetary space, helping to investigate two of the most important overarching issues in heliophysics — the energization of charged particles from the Sun, and the interaction of the solar wind with interstellar space. Additionally, IMAP will support near real-time observations of the solar wind and energetic particles, which can produce hazardous conditions in the space environment near Earth. IMAP is launching no earlier than Sept. 23, 2025, aboard a SpaceX Falcon 9 rocket from Launch Complex 39A at NASA’s Kennedy Space Center in Florida.Learn more about IMAP science: https://science.nasa.gov/missions/nasas-imap-mission-to-study-boundaries-of-our-home-in-space/Find out more about the IMAP mission: https://science.nasa.gov/mission/imap/ || ", "hits": 119 }, { "id": 14862, "url": "https://svs.gsfc.nasa.gov/14862/", "result_type": "Produced Video", "release_date": "2025-07-14T11:00:00-04:00", "title": "NASA’s TRACERS Studies Magnetic Explosions Above Earth", "description": "NASA's TRACERS mission, or the Tandem Reconnection and Cusp Electrodynamics Reconnaissance Satellites, will fly in low Earth orbit through the polar cusps, funnel-shaped holes in the magnetic field, to study magnetic reconnection and its effects in Earth's atmosphere. Magnetic reconnection is a mysterious process that happens when the solar wind, made of electrically charged particles and magnetic fields from the Sun, collides with Earth's magnetic shield, causing magnetic field lines to violently snap and explosively fling away particles at high speeds. This process has huge impacts on Earth, from causing breathtaking auroras to disrupting communications and power grids on Earth. TRACERS is launching no earlier than summer 2025 aboard a SpaceX Falcon 9 rocket from Space Launch Complex 4 East at Vandenberg Space Force Base in California.Find out more about the TRACERS mission and how it will help us better understand the ways space weather affects us on Earth: https://science.nasa.gov/mission/tracers/ || ", "hits": 152 }, { "id": 5524, "url": "https://svs.gsfc.nasa.gov/5524/", "result_type": "Interactive", "release_date": "2025-05-22T08:00:59-04:00", "title": "\"Snap It!\" Solar Eclipse Photography Game", "description": "The Traveler needs your help! They have come to Earth to study an event we call a total solar eclipse. Can you help the Traveler snap photos of an eclipse?", "hits": 74 }, { "id": 14736, "url": "https://svs.gsfc.nasa.gov/14736/", "result_type": "Produced Video", "release_date": "2024-12-16T09:00:00-05:00", "title": "NASA's #3point8 Challenge", "description": "On Dec. 24, 2024, NASA's Parker Solar Probe will fly approximately 3.8 million miles from the solar surface — the closest solar approach in history — while traveling about 430,000 miles per hour — the fastest any human-made object ever has traveled.To celebrate, join Parker's journey with a digital quest of your own: Each day from Dec. 17 - 24, 2024, we're hiding a new custom \"3.8\" digital sticker on a secret NASA webpage. Solve our puzzles to find them! || ", "hits": 96 }, { "id": 14688, "url": "https://svs.gsfc.nasa.gov/14688/", "result_type": "Produced Video", "release_date": "2024-09-26T12:00:00-04:00", "title": "5 Ways NASA Uses Solar Power", "description": "From studying life on Earth to powering spacecraft across the Solar System, NASA uses solar power to explore near and far. In September 2024, the Heliophysics Big Year theme is Environment and Sustainability. The Heliophysics Big Year is a global celebration of the Sun’s influence on Earth and the entire solar system. From October 14, 2023, to December 24, 2024, the Heliophysics Big Year celebrates under a theme, sharing opportunities to participate in many solar science events and activities. During the Heliophysics Big Year, participation isn’t limited to science – NASA invites everyone to celebrate the Sun with as many Sun-related activities as they can.To learn more about NASA’s history with solar power, visit: https://science.nasa.gov/sun/how-nasa-uses-and-improves-solar-power/ || ", "hits": 141 }, { "id": 14593, "url": "https://svs.gsfc.nasa.gov/14593/", "result_type": "Produced Video", "release_date": "2024-05-16T10:00:00-04:00", "title": "Continuing Strong Solar Flares: May 15-16, 2024", "description": "During the week of May 10 to May 16, 2024, NASA’s Solar Dynamics Observatory (SDO) observed nine X-class solar flares erupting from the Sun, including the largest in this solar cycle to date on May 14 that peaked at X8.7.This video shows these flares using SDO observations in two wavelengths of extreme ultraviolet light, 131 angstroms (colorized as teal) and 171 angstroms (colorized as gold).These flares originated primarily from an active region on the Sun called AR 13664. This region, along with another called AR 13663, was responsible for the majority of strong solar flares from May 3 through May 9.Watch this video on the NASA Goddard YouTube channel.Music credit: \"Collab Alert\" by Ellis Kent [PRS] from Universal Production Music || Thumbnail02.jpg (1280x720) [818.1 KB] || 14593_X-ClassFlaresDominateSunInMay_1080_YouTube.mp4 (1920x1080) [221.9 MB] || XClassFlares.en_US.srt [1.4 KB] || XClassFlares.en_US.vtt [1.3 KB] || 14593_X-ClassFlaresDominateSunInMay_4K_Facebook.mp4 (3840x2160) [328.8 MB] || 14593_X-ClassFlaresDominateSunInMay_4K_YouTube.mp4 (3840x2160) [539.4 MB] || 14593_X-ClassFlaresDominateSunInMay_4K_ProRes_.mov (3840x2160) [7.2 GB] || ", "hits": 131 }, { "id": 14557, "url": "https://svs.gsfc.nasa.gov/14557/", "result_type": "Produced Video", "release_date": "2024-03-21T10:00:00-04:00", "title": "How to Photograph a Total Solar Eclipse", "description": "On April 8, 2024, a total solar eclipse will soar over the heads of more than 30 million people across North America. This astronomical event is a unique opportunity for scientists studying in the shadow of the Moon, but it’s also a perfect opportunity to capture unforgettable images. Whether you’re an amateur photographer or a selfie master, try out these tips for photographing the eclipse. To learn more about eclipses visit science.nasa.gov/eclipses || ", "hits": 136 }, { "id": 14362, "url": "https://svs.gsfc.nasa.gov/14362/", "result_type": "Produced Video", "release_date": "2023-06-13T12:00:00-04:00", "title": "High Above Down Under Series", "description": "Around a different star, Earth may never have developed life at all. So what makes a star friendly to life? We joined two rocket teams as they traveled to the remote Northern Territory of Australia to capture light from our closest stellar neighbors to help reveal the answer. Follow their journey in the 6-part video series High Above Down Under. Episodes released weekly starting June 27, 2023. || ", "hits": 66 }, { "id": 14299, "url": "https://svs.gsfc.nasa.gov/14299/", "result_type": "Produced Video", "release_date": "2023-03-10T10:00:00-05:00", "title": "What is Plasma?", "description": "Plasma makes up 99.9% of the visible universe, but what is it? This video discusses what plasma is, where it lives, and how NASA studies it. || ", "hits": 890 }, { "id": 14164, "url": "https://svs.gsfc.nasa.gov/14164/", "result_type": "Produced Video", "release_date": "2022-06-07T19:00:00-04:00", "title": "Australia Sounding Rocket Campaign Press Kit", "description": "NASA will launch three suborbital sounding rockets in June and July 2022 from the Arnhem Space Center in Australia’s Northern Territory to conduct astrophysics studies that can only be done from the Southern Hemisphere. The three missions will focus on α Centauri A and B, two of the three-star α Centauri system that are the closest stars to our Sun, and X-rays emanating from the interstellar medium, clouds of gases and particles between stars.The three sounding rocket night-time missions will be launched between June 26 and July 12 on two-stage Black Brant IX sounding rockets, from the Arnhem Space Center, which is owned and operated by Equatorial Launch Australia or ELA. The Arnhem Space Center is a commercial space launch facility, located on the Dhupuma Plateau near Nhulunbuy. The NASA missions will be the first launches from Arnhem.Learn more: Australia Sounding Rocket Fact SheetWatch more: Sounding Rockets: Cutting Edge Science, 15 Minutes at a TimeWhat Is a Sounding Rocket?Riding Along with a NASA Sounding Rocket || ", "hits": 142 }, { "id": 4987, "url": "https://svs.gsfc.nasa.gov/4987/", "result_type": "Visualization", "release_date": "2022-04-28T11:00:00-04:00", "title": "Fast Magnetic Reconnection and the Hall Effect", "description": "Magnetic reconnection is one of the most complex processes known for converting energy from magnetic fields to particle motion. It takes place in solar flares and regions of planetary (and stellar) magnetospheres. Having been studied since the 1950s, many details of the process are still undergoing study.One of the key components in magnetic reconnection is the collision of two magnetic field regions with opposite-directed field lines, imbedded in a plasma. The field and plasma combination forms an X-shaped configuration at their closest, and most intense point.These visualizations are plotted from a reconnection model generated by VPIC (Vector Particle-In-Cell) code. Quantities are plotted in 'dimensionless' coordinates, that are normalized to the ion inertial length (di). || ", "hits": 137 }, { "id": 20363, "url": "https://svs.gsfc.nasa.gov/20363/", "result_type": "Animation", "release_date": "2022-03-09T18:00:00-05:00", "title": "Animation: Heliosphere", "description": "The sun sends out a constant flow of charged particles called the solar wind, which ultimately travels past all the planets to some three times the distance to Pluto before being impeded by the interstellar medium. This forms a giant bubble around the sun and its planets, known as the heliosphere. NASA studies the heliosphere to better understand the fundamental physics of the space surrounding us - which, in turn, provides information regarding space throughout the rest of the universe, as well as regarding what makes planets habitable.The solar wind is a gas of charged particles known as plasma, a state of matter governed by its own set physical laws just as the more common solids, liquids, and gases are. As the solar wind sweeps out into space, it creates a space environment filled with radiation as well as magnetic fields that trail all the way back to the sun. This space environment is augmented by interstellar cosmic rays and occasional concentrated clouds of solar material that burst off the sun, known as coronal mass ejections.This complex environment surrounds the planets and ultimately has a crucial effect on the formation, evolution, and destiny of planetary systems. For one thing, our heliosphere acts as a giant shield, protecting the planets from galactic cosmic radiation. Earth is additionally shielded by its own magnetic field, the magnetosphere, which protects us not only from solar and cosmic particle radiation but also from erosion of the atmosphere by the solar wind. Planets without a shielding magnetic field, such as Mars and Venus, are exposed to such processes and have evolved differently.NASA's studies of the heliosphere include research into: how the solar wind behaves near Earth; what causes and sustains magnetic and electric fields around other planets; how does the heliosphere interact with the interstellar medium; what do the boundaries of the heliosphere look like; what is the origin and evolution of the solar wind and the interstellar cosmic rays; and what contributes to the habitability of exoplanets.The field is, therefore, intensely cross-disciplinary. Heliospheric research often works hand in hand with planetary scientists, astrophysicists, astrobiologists, and space weather researchers.NASA heliophysics missions contributing to heliospheric research are: the Advanced Composition Explorer; NOAA's Deep Space Climate Observatory, the Interstellar Boundary Explorer, the Solar Terrestrial Relations Observatory; Voyager, and Wind. || ", "hits": 423 }, { "id": 14095, "url": "https://svs.gsfc.nasa.gov/14095/", "result_type": "Produced Video", "release_date": "2022-02-09T09:00:00-05:00", "title": "NASA’s New Views of Venus’ Surface From Space", "description": "NASA’s Parker Solar Probe has taken its first visible light images of the surface of Venus from space. Smothered in thick clouds, Venus’ surface is usually shrouded from sight. But in two recent flybys of the planet, Parker used its Wide-Field Imager, or WISPR, to image the entire nightside in wavelengths of the visible spectrum – the type of light that the human eye can see – and extending into the near-infrared.The images, combined into a video, reveal a faint glow from the surface that shows distinctive features like continental regions, plains, and plateaus. A luminescent halo of oxygen in the atmosphere can also be seen surrounding the planet.Link to NASA.gov feature.Link to associated research paper. || ", "hits": 1040 }, { "id": 4957, "url": "https://svs.gsfc.nasa.gov/4957/", "result_type": "Visualization", "release_date": "2021-12-14T12:00:00-05:00", "title": "Parker Solar Probe: The Origins of Switchbacks", "description": "Most of the magnetic field measured at Parker during this time is directed sunward (blue field lines and vectors). A switchback occurs when the field changes direction almost 180 degrees for a short period of time. FIELDS instrument magnetic vector data are projected from the spacecraft position as arrows. The arrows are colored deep blue for sunward vectors, deep red for anti-sunward, and in between for directions off from this line. The heliospheric magnetic field lines are represented as gold. || ParkerSP.ChaseCloseupAft.Switchbacks20181106A.FIELDS.clockSlate_EarthTarget.HD1080.00990_print.jpg (1024x576) [114.9 KB] || ParkerSP.ChaseCloseupAft.Switchbacks20181106A.FIELDS.clockSlate_EarthTarget.HD1080.00990_searchweb.png (320x180) [71.7 KB] || ParkerSP.ChaseCloseupAft.Switchbacks20181106A.FIELDS.clockSlate_EarthTarget.HD1080.00990_thm.png (80x40) [4.5 KB] || Switchbacks20181106A (1920x1080) [0 Item(s)] || ParkerSP.ChaseCloseupAft.Switchbacks20181106A.FIELDS.HD1080_p30.mp4 (1920x1080) [25.7 MB] || ParkerSP.ChaseCloseupAft.Switchbacks20181106A.FIELDS.HD1080_p30.webm (1920x1080) [4.4 MB] || Switchbacks20181106A (3840x2160) [0 Item(s)] || ParkerSP.ChaseCloseupAft.Switchbacks20181106A.FIELDS.UHD3840_2160p30.mp4 (3840x2160) [100.2 MB] || ParkerSP.ChaseCloseupAft.Switchbacks20181106A.FIELDS.HD1080_p30.mp4.hwshow [229 bytes] || ", "hits": 151 }, { "id": 4958, "url": "https://svs.gsfc.nasa.gov/4958/", "result_type": "Visualization", "release_date": "2021-12-14T12:00:00-05:00", "title": "Parker Solar Probe: Crossing the Alfven Surface", "description": "Split window view illustrating the orbit of Parker with the orbit trail colored based on the Mach number of the solar wind and the magnetic field lines (represented as gold) connecting back to the Sun. The Mach number drops below unity (one) when a field line transitions between two different coronal hole regions (the blue and red regions marked on the Sun). || Parker_SolarCloseup.combo.HD1080.00480_print.jpg (1024x576) [121.9 KB] || Parker_SolarCloseup.combo.HD1080.00480_searchweb.png (320x180) [74.1 KB] || Parker_SolarCloseup.combo.HD1080.00480_thm.png (80x40) [5.2 KB] || Parker_SolarCloseup.combo.HD1080 (1920x1080) [0 Item(s)] || Parker_SolarCloseup.combo.HD1080_p30.mp4 (1920x1080) [45.8 MB] || Parker_SolarCloseup.combo.HD1080_p30.webm (1920x1080) [5.6 MB] || Parker_SolarCloseup.combo.UHD2160 (3840x2160) [0 Item(s)] || Parker_SolarCloseup.combo.UHD2160_p30.mp4 (3840x2160) [124.5 MB] || Parker_SolarCloseup.combo.HD1080_p30.mp4.hwshow [202 bytes] || ", "hits": 186 }, { "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": 164 }, { "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": 378 }, { "id": 13859, "url": "https://svs.gsfc.nasa.gov/13859/", "result_type": "Produced Video", "release_date": "2021-06-18T12:00:00-04:00", "title": "Why Does NASA Observe The Sun in Different Colors?", "description": "The Solar Dynamics Observatory, or SDO, was launched on Feb. 11, 2010, and began collecting science data a few months later. With two imaging instruments – the Atmospheric Imaging Assembly and the Helioseismic and Magnetic Imager, which were designed in concert to provide complementary views of the Sun – SDO sees the Sun in more than 10 distinct wavelengths of light, showing solar material at different temperatures. SDO also measures the Sun’s magnetic field and the motion of solar material at its surface, and, using a technique called helioseismology, allows scientists to probe deep into the Sun's interior, where the Sun’s complex magnetic fields sprout from. And with more than a decade of observation under its belt, SDO has provided scientists with hundreds of millions of images of our star. || ", "hits": 257 }, { "id": 13869, "url": "https://svs.gsfc.nasa.gov/13869/", "result_type": "Produced Video", "release_date": "2021-06-07T15:00:00-04:00", "title": "The key to understanding solar explosions", "description": "Music credit: Universal Music Production“Early Birds,” Edwards Tschuggnall || ROSETTASTONE_THUMB.png (1920x1080) [1.0 MB] || ROSETTASTONE_THUMB_print.jpg (1024x576) [63.6 KB] || ROSETTASTONE_THUMB_searchweb.png (320x180) [56.1 KB] || ROSETTASTONE_THUMB_thm.png (80x40) [5.4 KB] || 0607_ROSETTASTONE_VIDEOFINAL.mp4 (1920x1080) [273.3 MB] || 0607_ROSETTASTONE_VIDEOFINAL.webm (1920x1080) [17.0 MB] || ROSETTASTONE_CAPTION.en_US.srt [2.5 KB] || ROSETTASTONE_CAPTION.en_US.vtt [2.5 KB] || ", "hits": 22 }, { "id": 13698, "url": "https://svs.gsfc.nasa.gov/13698/", "result_type": "Produced Video", "release_date": "2020-08-20T00:00:00-04:00", "title": "Small Flare Seen on the Sun, August 16, 2020", "description": "NASA’s Solar Dynamics Observatory observes the Aug. 16, 2020, B-class flare at 131, 171, and 193 angstroms. Credit: NASA/SDO || SDO_8-16-2020_Eruption_Triptych_ProRes_1080.00121_print.jpg (1024x576) [196.4 KB] || SDO_8-16-2020_Eruption_Triptych_ProRes_1080.00121_searchweb.png (320x180) [91.4 KB] || SDO_8-16-2020_Eruption_Triptych_ProRes_1080.00121_thm.png (80x40) [6.2 KB] || SDO_8-16-2020_Eruption_Triptych_ProRes_1080.mov (1920x1080) [129.8 MB] || SDO_8-16-2020_Eruption_Triptych_1080.mp4 (1920x1080) [10.1 MB] || SDO_8-16-2020_Eruption_Triptych_1080.webm (1920x1080) [1.0 MB] || ", "hits": 118 }, { "id": 13688, "url": "https://svs.gsfc.nasa.gov/13688/", "result_type": "Produced Video", "release_date": "2020-08-17T11:45:00-04:00", "title": "NASA Explores Earth's Magnetic \"Dent\"", "description": "Music: \"Now We Wait\" by Kamal David Kamruddin [PRS]This video can be freely shared and downloaded. While the video in its entirety can be shared without permission, some individual imagery provided by pond5.com and Artbeats is obtained through permission and may not be excised or remixed in other products. Specific details on stock footage may be found here. For more information on NASA’s media guidelines, visit https://www.nasa.gov/multimedia/guidelines/index.html.Complete transcript available. || South_Atlantic_Anomaly_Still_2.jpg (1920x1080) [346.0 KB] || South_Atlantic_Anomaly_Still_2_print.jpg (1024x576) [139.2 KB] || South_Atlantic_Anomaly_Still_2_searchweb.png (320x180) [43.0 KB] || South_Atlantic_Anomaly_Still_2_web.png (320x180) [43.0 KB] || South_Atlantic_Anomaly_Still_2_thm.png (80x40) [4.8 KB] || 13688_South_Atlantic_Anomaly_Fine.mov (1920x1080) [2.6 GB] || 13688_South_Atlantic_Anomaly_Fine.webm (960x540) [65.7 MB] || 13688_South_Atlantic_Anomaly_Fine.mp4 (1920x1080) [292.9 MB] || 13688_South_Atlantic_Anomaly_Fine_lowres.mp4 (1280x720) [52.3 MB] || SAA.en_US.srt [3.5 KB] || SAA.en_US.vtt [3.5 KB] || ", "hits": 143 }, { "id": 13687, "url": "https://svs.gsfc.nasa.gov/13687/", "result_type": "Produced Video", "release_date": "2020-08-14T10:00:00-04:00", "title": "NASA Spacecraft Uncover Mystery Behind Auroral Beads", "description": "A special type of aurora, draped east-west across the night sky like a glowing pearl necklace, is helping scientists better understand the science of auroras and their powerful drivers out in space. Known as auroral beads, these lights often show up just before large auroral displays, which are caused by electrical storms in space called substorms. Until now, scientists weren’t sure if auroral beads are somehow connected to other auroral displays as a phenomenon in space that precedes substorms, or if they are caused by disturbances closer to Earth’s atmosphere.But powerful new computer models, combined with observations from NASA’s Time History of Events and Macroscale Interactions during Substorms – THEMIS – mission, have provided the first direct evidence of the events in space that lead to the appearance of these beads, and demonstrated the important role they play in our local space environment. || ", "hits": 87 }, { "id": 4776, "url": "https://svs.gsfc.nasa.gov/4776/", "result_type": "Visualization", "release_date": "2020-06-24T10:00:00-04:00", "title": "Ten Years of Solar Dynamics Observatory", "description": "Ten years of SDO AIA 171 angstrom data with day time stamp overlay. Frames are sampled approximately one image every hour. || SDOat10_AIA171_stand.UHD2160.01500_print.jpg (1024x576) [47.4 KB] || SDOat10_AIA171_stand.UHD2160.01500_searchweb.png (320x180) [40.9 KB] || SDOat10_AIA171_stand.UHD2160.01500_thm.png (80x40) [4.0 KB] || SDOat10_AIA171.1080p30.webm (1920x1080) [348.5 MB] || SDOat10_AIA171.baseimage (3840x2160) [0 Item(s)] || SDOat10_AIA171.1080p30.mp4 (1920x1080) [3.9 GB] || SDOat10_AIA171.UHD2160_p30.mp4 (3840x2160) [13.0 GB] || SDOat10_AIA171.1080p30.mp4.hwshow [188 bytes] || ", "hits": 105 }, { "id": 13641, "url": "https://svs.gsfc.nasa.gov/13641/", "result_type": "Produced Video", "release_date": "2020-06-24T10:00:00-04:00", "title": "A Decade of Sun", "description": "This 10-year time lapse of the Sun at 17.1nm shows the rise and fall of the solar cycle and notable events, like transiting planets and solar eruptions. Music: \"Solar Observer\" written and produced for this video by Lars Leonhard.Credit: NASA's Goddard Space Flight Center/SDOWatch this video on the NASA Goddard YouTube channel.Complete transcript available. || SDO_Year10_Poster_1080.png (1920x1080) [7.5 MB] || SDO_Year10_Poster_1080.jpg (1920x1080) [519.0 KB] || SDO_Year10_Poster_4k.jpg (3840x2160) [972.4 KB] || SDO_Year10_Poster_4k.png (3840x2160) [27.2 MB] || SDO_10_Year_Sun_1080_15mbps.mp4 (1920x1080) [6.5 GB] || SDO_Year_10_FINAL_720FB.mp4 (1280x720) [7.3 GB] || SDO_10_Year_Sun_1080_15mbps.webm (1920x1080) [482.2 MB] || SDO_10_Year_Sun_ProRes_3840x2160_24.mov (3840x2160) [191.6 GB] || SDO_10_Year_Sun_4k_100mbps.mp4 (3840x2160) [42.9 GB] || SDO_10_Year_Sun_4k_20mbps.mp4 (3840x2160) [8.7 GB] || SDO_10_Year_Sun_SRT_Captions.en_US.srt [2.7 KB] || SDO_10_Year_Sun_SRT_Captions.en_US.vtt [2.8 KB] || ", "hits": 456 }, { "id": 13524, "url": "https://svs.gsfc.nasa.gov/13524/", "result_type": "Produced Video", "release_date": "2020-02-11T10:00:00-05:00", "title": "SDO Celebrates its Tenth Launch Anniversary", "description": "Capturing an image in ten different wavelengths of light every 12 seconds, NASA’s Solar Dynamics Observatory — SDO — has provided an unprecedentedly clear picture of how massive explosions on the Sun grow and erupt ever since its launch on Feb. 11, 2010. The imagery is also captivating, allowing one to watch the constant ballet of solar material through the Sun's atmosphere, the corona. This year marks the tenth anniversary of SDO's launch and the start of its decade watching the Sun.Music: \"Encompass\" from Universal Production MusicWatch this video on the NASA Goddard YouTube channel.Complete transcript available. || PROMO_FINAL.00_01_04_08.Still001.jpg (1920x1080) [489.9 KB] || PROMO_FINAL.00_01_04_08.Still001_searchweb.png (320x180) [80.6 KB] || PROMO_FINAL.00_01_04_08.Still001_thm.png (80x40) [6.0 KB] || SDO_10th_Promo_ProRes_1920x1080_2997.mov (1920x1080) [981.6 MB] || SDO_10th_Promo_Best_1080.mp4 (1920x1080) [363.3 MB] || SDO_10th_Promo_Good_1080.mp4 (1920x1080) [141.7 MB] || SDO_10th_Promo_Best_1080.webm (1920x1080) [10.2 MB] || SDO_10th_Promo_SRT_Captions.en_US.srt [820 bytes] || SDO_10th_Promo_SRT_Captions.en_US.vtt [833 bytes] || ", "hits": 41 }, { "id": 4761, "url": "https://svs.gsfc.nasa.gov/4761/", "result_type": "Visualization", "release_date": "2019-12-17T10:00:00-05:00", "title": "New sites for magnetic reconnection", "description": "HD and UHD movie views of the plasma flowing along magnetic fields lines visible at 171Å. || May2012_Reconn_171A_stand.HD1080i.00951_print.jpg (1024x576) [52.0 KB] || May2012_Reconn_171A_stand.HD1080i.00951_searchweb.png (320x180) [43.5 KB] || May2012_Reconn_171A_stand.HD1080i.00951_thm.png (80x40) [4.2 KB] || AIA171A (1920x1080) [0 Item(s)] || May2012_Reconn_171A.HD1080i_p30.mp4 (1920x1080) [21.9 MB] || May2012_Reconn_171A.HD1080i_p30.webm (1920x1080) [7.0 MB] || AIA171A (3840x2160) [0 Item(s)] || May2012_Reconn_171A_2160p30.mp4 (3840x2160) [107.3 MB] || May2012_Reconn_171A.HD1080i_p30.mp4.hwshow [197 bytes] || ", "hits": 36 }, { "id": 13422, "url": "https://svs.gsfc.nasa.gov/13422/", "result_type": "Produced Video", "release_date": "2019-12-17T10:00:00-05:00", "title": "A New Kind of Explosion on the Sun", "description": "Complete transcript available.Watch this video on the NASA Goddard YouTube channel.Music Credit: Light Hearted Angst by Dewey Dellay || ReconnThumb.jpg (1920x1080) [156.1 KB] || ReconnThumb_searchweb.png (320x180) [100.6 KB] || ReconnThumb_thm.png (80x40) [7.3 KB] || ForcedReconnV2_Twitter.mp4 (1920x1080) [29.6 MB] || ForcedReconnV2.webm (1920x1080) [14.8 MB] || ForcedReconnV2.mp4 (1920x1080) [134.9 MB] || ForcedReconnV2_FB.mp4 (1920x1080) [155.5 MB] || ForcedReconnV2_YouTube.mp4 (1920x1080) [207.3 MB] || ForcedReconnV2.en_US.srt [2.6 KB] || ForcedReconnV2.en_US.vtt [2.6 KB] || ForcedReconnV2.mov (1920x1080) [1.7 GB] || ", "hits": 84 }, { "id": 4699, "url": "https://svs.gsfc.nasa.gov/4699/", "result_type": "Visualization", "release_date": "2018-11-30T14:00:00-05:00", "title": "The CME Heard 'Round the Solar System", "description": "As the CMEs and SIRs move through the solar system, we include graphs of particle fluxes measured at Earth, Mars, and STEREO-A. || SEPsAtMars.topfixed.UHDframes.clockSlate_HAE.UHD3840.01000_print.jpg (1024x576) [100.6 KB] || SEPsAtMars.topfixed.UHDframes.clockSlate_HAE.UHD3840.01000_thm.png (80x40) [6.5 KB] || SEPsAtMars.topfixed.UHDframes.clockSlate_HAE.UHD3840.01000_searchweb.png (320x180) [87.5 KB] || SEPsAtMars.topfixed_HAE.HD1080i_p30.mp4 (1920x1080) [19.4 MB] || 1920x1080_16x9_30p (1920x1080) [0 Item(s)] || SEPsAtMars.topfixed_HAE.HD1080i_p30.webm (1920x1080) [3.0 MB] || SEPsAtMars.topfixed_HAE_2160p30.mp4 (3840x2160) [61.6 MB] || 3840x2160_16x9_30p (3840x2160) [0 Item(s)] || ", "hits": 110 }, { "id": 12943, "url": "https://svs.gsfc.nasa.gov/12943/", "result_type": "Produced Video", "release_date": "2018-09-24T12:00:00-04:00", "title": "Explorer 1", "description": "60 years ago we launched humanity’s first science satellite, Explorer 1. || explorer_history.jpg (1258x708) [283.4 KB] || explorer_history_1024x576.jpg (1024x576) [219.6 KB] || explorer_history_1024x576_searchweb.png (320x180) [34.1 KB] || explorer_history_1024x576_thm.png (80x40) [3.2 KB] || ", "hits": 87 }, { "id": 13073, "url": "https://svs.gsfc.nasa.gov/13073/", "result_type": "Produced Video", "release_date": "2018-09-20T14:00:00-04:00", "title": "Rare Electric Blue Clouds Observed By NASA Balloon", "description": "On the cusp of our atmosphere live a thin group of seasonal electric blue clouds. Forming fifty miles above the poles in summer, these clouds are known as noctilucent clouds or polar mesospheric clouds — PMCs. A recent NASA long-duration balloon mission observed these clouds over the course of five days at their home in the mesosphere. The resulting photos, which scientists have just begun to analyze, will help us better understand turbulence in the atmosphere, as well as in oceans, lakes, and other planetary atmospheres, and may even improve weather forecasting.For more information: https://www.nasa.gov/feature/goddard/2018/nasa-balloon-mission-captures-electric-blue-clouds || ", "hits": 82 }, { "id": 4664, "url": "https://svs.gsfc.nasa.gov/4664/", "result_type": "Visualization", "release_date": "2018-07-27T00:00:00-04:00", "title": "Jupiter's Magnetosphere", "description": "Jupiter's magnetosphere - a basic view. || Jupiter_JupiterBasic_Dayside.slate_BaseRig.HD1080i.1000_print.jpg (1024x576) [245.3 KB] || Jupiter_JupiterBasic_Dayside.slate_BaseRig.HD1080i.1000_searchweb.png (320x180) [132.5 KB] || Jupiter_JupiterBasic_Dayside.slate_BaseRig.HD1080i.1000_thm.png (80x40) [8.3 KB] || JupiterBasic-noglyph (1920x1080) [0 Item(s)] || Jupiter_JupiterBasic_Dayside.HD1080i_p30.webm (1920x1080) [32.8 MB] || Jupiter_JupiterBasic_Dayside.HD1080i_p30.mp4 (1920x1080) [406.6 MB] || JupiterBasic-noglyph (3840x2160) [0 Item(s)] || Jupiter_JupiterBasic_Dayside_2160p30.mp4 (3840x2160) [984.8 MB] || Jupiter_JupiterBasic_Dayside.HD1080i_p30.mp4.hwshow [206 bytes] || ", "hits": 182 }, { "id": 4665, "url": "https://svs.gsfc.nasa.gov/4665/", "result_type": "Visualization", "release_date": "2018-07-27T00:00:00-04:00", "title": "Saturn's Magnetosphere", "description": "A basic view of Saturn's magnetosphere. || Saturn_SaturnBasic_Dayside.slate_BaseRig.HD1080i.1500_print.jpg (1024x576) [186.2 KB] || Saturn_SaturnBasic_Dayside.slate_BaseRig.HD1080i.1500_searchweb.png (320x180) [107.8 KB] || Saturn_SaturnBasic_Dayside.slate_BaseRig.HD1080i.1500_thm.png (80x40) [7.1 KB] || SaturnBasic-noglyph (1920x1080) [0 Item(s)] || Saturn_SaturnBasic_Dayside.HD1080i_p30.webm (1920x1080) [22.1 MB] || Saturn_SaturnBasic_Dayside.HD1080i_p30.mp4 (1920x1080) [365.5 MB] || SaturnBasic-noglyph (3840x2160) [0 Item(s)] || Saturn_SaturnBasic_Dayside_2160p30.mp4 (3840x2160) [938.9 MB] || Saturn_SaturnBasic_Dayside.HD1080i_p30.mp4.hwshow || ", "hits": 151 }, { "id": 4666, "url": "https://svs.gsfc.nasa.gov/4666/", "result_type": "Visualization", "release_date": "2018-07-27T00:00:00-04:00", "title": "Uranus' Magnetosphere", "description": "A basic view of the Uranian magnetosphere when the rotation axis is perpendicular to the Uranus-Sun line and days and nights are of equal duration. || Uranus_UranusEquinox_Dayside.slate_BaseRig.HD1080i.1500_print.jpg (1024x576) [197.1 KB] || Uranus_UranusEquinox_Dayside.slate_BaseRig.HD1080i.1500_searchweb.png (320x180) [107.3 KB] || Uranus_UranusEquinox_Dayside.slate_BaseRig.HD1080i.1500_thm.png (80x40) [6.8 KB] || UranusEquinox-noglyph (1920x1080) [0 Item(s)] || Uranus_UranusEquinox_Dayside.HD1080i_p30.webm (1920x1080) [20.9 MB] || Uranus_UranusEquinox_Dayside.HD1080i_p30.mp4 (1920x1080) [308.1 MB] || UranusEquinox-noglyph (3840x2160) [0 Item(s)] || Uranus_UranusEquinox_Dayside_2160p30.mp4 (3840x2160) [758.5 MB] || Uranus_UranusEquinox_Dayside.HD1080i_p30.mp4.hwshow [206 bytes] || ", "hits": 204 }, { "id": 4667, "url": "https://svs.gsfc.nasa.gov/4667/", "result_type": "Visualization", "release_date": "2018-07-27T00:00:00-04:00", "title": "Neptune's Magnetosphere", "description": "A basic view of the Neptunian magnetosphere when the southern side of the rotation axis is directed sunward (southern summer) || Neptune_NeptuneSouthSummer_Dayside.slate_BaseRig.HD1080i.1500_print.jpg (1024x576) [195.5 KB] || Neptune_NeptuneSouthSummer_Dayside.slate_BaseRig.HD1080i.1500_searchweb.png (320x180) [108.2 KB] || Neptune_NeptuneSouthSummer_Dayside.slate_BaseRig.HD1080i.1500_thm.png (80x40) [6.8 KB] || NeptuneSouthSummer-noglyph (1920x1080) [0 Item(s)] || Neptune_NeptuneSouthSummer_Dayside.HD1080i_p30.webm (1920x1080) [21.4 MB] || Neptune_NeptuneSouthSummer_Dayside.HD1080i_p30.mp4 (1920x1080) [328.8 MB] || NeptuneSouthSummer-noglyph (3840x2160) [0 Item(s)] || Neptune_NeptuneSouthSummer_Dayside_2160p30.mp4 (3840x2160) [820.2 MB] || Neptune_NeptuneSouthSummer_Dayside.HD1080i_p30.mp4.hwshow [212 bytes] || ", "hits": 129 }, { "id": 4649, "url": "https://svs.gsfc.nasa.gov/4649/", "result_type": "Visualization", "release_date": "2018-05-29T10:00:00-04:00", "title": "Plasma Zoo: Gyroresonant Scattering", "description": "In a background magnetic field, represented by the cyan arrows, two electrons are propagating to the right, executing identical gyromotion. A circularly polarized electromagnetic wave approaches the upper electron from the left. || GyroresonanceV3_RideAlong_inertial.HD1080i.0150_print.jpg (1024x576) [85.3 KB] || GyroresonanceV3_RideAlong_inertial.HD1080i.0150_searchweb.png (320x180) [55.9 KB] || GyroresonanceV3_RideAlong_inertial.HD1080i.0150_thm.png (80x40) [4.3 KB] || RideAlong (1920x1080) [0 Item(s)] || GyroresonanceV3_RideAlong.HD1080i_p30.mp4 (1920x1080) [17.2 MB] || GyroresonanceV3_RideAlong.HD1080i_p30.webm (1920x1080) [2.3 MB] || GyroresonanceV3_RideAlong_inertial.HD1080i.0150.tif (1920x1080) [2.4 MB] || RideAlong (3840x2160) [0 Item(s)] || GyroresonanceV3_RideAlong.UHD3840_2160p30.mp4 (3840x2160) [49.4 MB] || GyroresonanceV3_RideAlong.HD1080i_p30.mp4.hwshow [203 bytes] || ", "hits": 68 }, { "id": 4639, "url": "https://svs.gsfc.nasa.gov/4639/", "result_type": "Visualization", "release_date": "2018-05-09T13:00:00-04:00", "title": "MMS Sees a New Type of Reconnection", "description": "The Magnetospheric Multiscale (MMS) mission consists of four identical satellites that traverse various regions of Earth's magnetosphere measuring the particles and electric and magnetic field which influence them.In the turbulent plasma between Earth's magnetopause and bow shock, a region called the magnetosheath, the MMS satellite constellation has measured multiple jets of energetic electrons between magnetic bubbles. This appears to be a new 'flavor' of magnetic reconnection based on electrons and occuring on smaller time and spatial scales than the standard model of magnetic reconnection with ions.In these data visualizations, the arrows represent the data collected by the spacecraft. To better comprehend changes as the spacecraft moves along, the data are allowed to 'echo' along the spacecraft trail. The length of the vectors represent the relative magnitude of the vector. However, the electron and proton vectors are scaled so equal velocities correspond to vectors of equal magnitude.Magenta represents the direction and magnitude of the magnetic field at the spacecraft position.Green represents the direction and magnitude of the net electric current created by the motion of the electrons and ions measured at the spacecraft position.The four MMS spacecraft are represented by colored spheres, corresponding to the plotted data lines in the lower graphicMMS1MMS2MMS3MMS4The clocks on MMS are synchronized for the TAI (International Atomic Time) system provided through the Global Positioning System (GPS) satellites. It provides a high-precision time reference for comparing MMS measurements to other datasets. || ", "hits": 94 }, { "id": 12901, "url": "https://svs.gsfc.nasa.gov/12901/", "result_type": "Produced Video", "release_date": "2018-05-09T13:00:00-04:00", "title": "NASA Spacecraft Finds New Magnetic Process in Turbulent Space", "description": "Though close to home, the space immediately around Earth is full of hidden secrets and invisible processes. In a new discovery reported in the journal Nature, scientists working with NASA’s Magnetospheric Multiscale spacecraft — MMS — have uncovered a new type of magnetic event in our near-Earth environment by using an innovative technique to squeeze extra information out of the data.Magnetic reconnection is one of the most important processes in the space — filled with charged particles known as plasma — around Earth. This fundamental process dissipates magnetic energy and propels charged particles, both of which contribute to a dynamic space weather system that scientists want to better understand, and even someday predict, as we do terrestrial weather. Reconnection occurs when crossed magnetic field lines snap, explosively flinging away nearby particles at high speeds. The new discovery found reconnection where it has never been seen before — in turbulent plasma. || ", "hits": 107 }, { "id": 12543, "url": "https://svs.gsfc.nasa.gov/12543/", "result_type": "Produced Video", "release_date": "2018-04-30T12:00:00-04:00", "title": "The Electron Beltway", "description": "NASA's Van Allen Probes reveal how electrons move through the radiation belts that surround Earth. || 12249_1280.jpg (1280x720) [576.4 KB] || 12249_1280_1024x576.jpg (1024x576) [386.3 KB] || ", "hits": 196 }, { "id": 12618, "url": "https://svs.gsfc.nasa.gov/12618/", "result_type": "Produced Video", "release_date": "2018-04-02T12:00:00-04:00", "title": "How Plasma Transports Energy", "description": "For the first time, NASA scientists see how energy is transported in a plasma. || Story_Cover_AlfvenWaveParticles.Kinetic.MediumGyro.vzAlfvenDG4_staticXclose_inertial.HD1080i.0200_print.jpg (1024x576) [142.6 KB] || Story_Cover_AlfvenWaveParticles.Kinetic.MediumGyro.vzAlfvenDG4_staticXclose_inertial.HD1080i.0200_print_print.jpg (1024x576) [139.9 KB] || Story_Cover_AlfvenWaveParticles.Kinetic.MediumGyro.vzAlfvenDG4_staticXclose_inertial.HD1080i.0200_print_searchweb.png (320x180) [84.0 KB] || Story_Cover_AlfvenWaveParticles.Kinetic.MediumGyro.vzAlfvenDG4_staticXclose_inertial.HD1080i.0200_print_thm.png (80x40) [6.2 KB] || ", "hits": 101 }, { "id": 4595, "url": "https://svs.gsfc.nasa.gov/4595/", "result_type": "Visualization", "release_date": "2017-11-27T10:00:00-05:00", "title": "Mapping Particle Injections in Earth's Magnetosphere", "description": "A view from above the northern hemisphere of particle injection propagation constructed from their respective satellite detections. Distinct injections, and their detection by satellites, are represented by different colors. || MagnetosphereMultiMission.top.GSE.AU.clockSlate_EarthTarget.HD1080i.01200_print.jpg (1024x576) [115.4 KB] || MagnetosphereMultiMission.top.GSE.AU.clockSlate_EarthTarget.HD1080i.01200_searchweb.png (320x180) [82.7 KB] || MagnetosphereMultiMission.top.GSE.AU.clockSlate_EarthTarget.HD1080i.01200_thm.png (80x40) [6.3 KB] || TopView (1920x1080) [0 Item(s)] || MagnetosphereMultiMission.top.HD1080i_p30.mp4 (1920x1080) [29.7 MB] || MagnetosphereMultiMission.top.HD1080i_p30.webm (1920x1080) [6.1 MB] || TopView (3840x2160) [0 Item(s)] || MagnetosphereMultiMission.top.UHD3840_2160p30.mp4 (3840x2160) [93.0 MB] || MagnetosphereMultiMission.top.HD1080i_p30.mp4.hwshow [207 bytes] || ", "hits": 48 }, { "id": 12704, "url": "https://svs.gsfc.nasa.gov/12704/", "result_type": "Produced Video", "release_date": "2017-08-31T12:00:00-04:00", "title": "NASA Eclipse Imagery", "description": "As millions of people across the United States experienced a total eclipse as the umbra, or Moon’s shadow passed over them, only six people witnessed the umbra from space. Viewing the eclipse from orbit were NASA’s Randy Bresnik, Jack Fischer and Peggy Whitson, ESA (European Space Agency’s) Paolo Nespoli, and Roscosmos’ Commander Fyodor Yurchikhin and Sergey Ryazanskiy. The space station crossed the path of the eclipse three times as it orbited above the continental United States at an altitude of 250 miles. Credit: NASA || iss052e056122.jpg (4928x3280) [844.0 KB] || ", "hits": 323 }, { "id": 12179, "url": "https://svs.gsfc.nasa.gov/12179/", "result_type": "Produced Video", "release_date": "2017-07-25T09:30:00-04:00", "title": "NASA Jets Chase The Total Solar Eclipse", "description": "For most viewers, the Aug. 21, 2017, total solar eclipse will last less than two and half minutes. But for one team of NASA-funded scientists, the eclipse will last over seven minutes. Their secret? Following the shadow of the Moon in two retrofitted WB-57F jet planes. Amir Caspi of the Southwest Research Institute in Boulder, Colorado, and his team will use two of NASA’s WB-57F research jets to chase the darkness across America on Aug. 21. Taking observations from twin telescopes mounted on the noses of the planes, Caspi will capture the clearest images of the Sun’s outer atmosphere — the corona — to date and the first-ever thermal images of Mercury, revealing how temperature varies across the planet’s surface. || ", "hits": 102 }, { "id": 4143, "url": "https://svs.gsfc.nasa.gov/4143/", "result_type": "Visualization", "release_date": "2017-07-12T10:01:00-04:00", "title": "Saturn's Magnetosphere", "description": "Earth's magnetic field creates a 'bubble' around Earth that helps protect our planet from some of the more harmful effects of energetic particles streaming out from the sun in the solar wind. Some of the earliest hints of this interaction go back to the 1850s with the work of Richard Carrington, and in the early 1900s with the work of Kristian Birkeland and Carl Stormer. That this field might form a type of 'bubble' around Earth was hypothesized by Sidney Chapman and Vincent Ferraro in the 1930s. The term 'magnetosphere' was applied to magnetic bubble by Thomas Gold in 1959. But it wasn't until the Space Age, when we sent the first probes to other planets, that we found clear evidence of their magnetic fields (though there were hints of a magnetic field for Jupiter in the 1950s, due to observations from radio telescopes). The Voyager program , two spacecraft launched in 1977, and successors to the Pioneer 10 and 11 missions, completed flybys of the giant outer planets. They became the implementation of the 'Grand Tour' of the outer planets originally proposed in the late 1960s. The Voyagers provided some of the first detailed measurments of the strength, extent and diversity of the magnetospheres of the outer planets.In these visualizations, we present simplified models of these planetary magnetospheres, designed to illustrate their scale, and basic features of their structure and impacts of the magnetic axes offset from the planetary rotation axes. For these visualizations, the magnetic field structure is represented by gold/copper lines. Some additional glyphs are provided to indicate some key directions in the field model.The Yellow arrow points towards the sun. The magnetotail is pointed in the opposite direction.The Cyan arrow represents the magnetic axis, usually tilted relative to the rotation axis. The arrow indicates the NORTH magnetic pole (convention has field lines moving north to south as the north pole of bar magnet (and compass pointer) points to the south magnetic pole).The Blue arrow represents the north rotation axis. It is part of the 3-D axis glyph (red, green, and blue arrows) included to make the planetary rotation more apparent.The semi-transparent grey mesh in the distance represents the boundary of the magnetosphere.Major satellites of the planetary system are also included. When appropriate for the time window of the visualization, the Voyager flyby trajectories are indicated.The models are constructed by combining the fields of a simple magnetic dipole, a current sheet (whose intensity is tuned match the scale of the magnetotail), and occasionally a ring current. This is a variation of the simple Luhmann-Friesen magnetosphere model. They are meant to be representative of the basic characteristics of the planetary magnetic fields. Some features NOT included are longitudes of magnetic poles to a standard planetary coordinate system and offsets of the dipole center from the planetary center. ReferencesT. Gold, Motions in the Magnetosphere of the EarthLuhmann & Friesen, A simple model of the magnetosphereLASP: Polarity of planetary magnetic fieldsWikipedia: The Solar Storm of 1859Wikipedia: Kristian BirkelandWikipedia: Carl StørmerSpecial thanks to Arik Posner (NASA/HQ) and Gina DiBraccio (UMBC/GSFC) for helpful pointers on orientation of planetary rotation and magnetic axes. || ", "hits": 120 }, { "id": 4142, "url": "https://svs.gsfc.nasa.gov/4142/", "result_type": "Visualization", "release_date": "2017-07-12T10:00:00-04:00", "title": "Jupiter's Magnetosphere", "description": "Earth's magnetic field creates a 'bubble' around Earth that helps protect our planet from some of the more harmful effects of energetic particles streaming out from the sun in the solar wind. Some of the earliest hints of this interaction go back to the 1850s with the work of Richard Carrington, and in the early 1900s with the work of Kristian Birkeland and Carl Stormer. That this field might form a type of 'bubble' around Earth was hypothesized by Sidney Chapman and Vincent Ferraro in the 1930s. The term 'magnetosphere' was applied to magnetic bubble by Thomas Gold in 1959. But it wasn't until the Space Age, when we sent the first probes to other planets, that we found clear evidence of their magnetic fields (though there were hints of a magnetic field for Jupiter in the 1950s, due to observations from radio telescopes). The Voyager program , two spacecraft launched in 1977, and successors to the Pioneer 10 and 11 missions, completed flybys of the giant outer planets. They became the implementation of the 'Grand Tour' of the outer planets originally proposed in the late 1960s. The Voyagers provided some of the first detailed measurments of the strength, extent and diversity of the magnetospheres of the outer planets.In these visualizations, we present simplified models of these planetary magnetospheres, designed to illustrate their scale, and basic features of their structure and impacts of the magnetic axes offset from the planetary rotation axes. The volcanic activity on Jupiter's moon Io launches a large amount of sulfur-based compounds along its orbit, which is subsequently ionized by solar ultraviolet radiation. This is represented in the visualization by the yellowish structure along the orbit of Io. This creates a plasma torus and ring current around Jupiter, which alters the planet's magnetic field, forming some of the perturbations in Jupiter's magnetic field along the orbit of Io.For these visualizations, the magnetic field structure is represented by gold/copper lines. Some additional glyphs are provided to indicate some key directions in the field model.The Yellow arrow points towards the sun. The magnetotail is pointed in the opposite direction.The Cyan arrow represents the magnetic axis, usually tilted relative to the rotation axis. The arrow indicates the NORTH magnetic pole (convention has field lines moving north to south as the north pole of bar magnet (and compass pointer) points to the south magnetic pole).The Blue arrow represents the north rotation axis. It is part of the 3-D axis glyph (red, green, and blue arrows) included to make the planetary rotation more apparent.The semi-transparent grey mesh in the distance represents the boundary of the magnetosphere.Major satellites of the planetary system are also included. When appropriate for the time window of the visualization, the Voyager flyby trajectories are indicated.The models are constructed by combining the fields of a simple magnetic dipole, a current sheet (whose intensity is tuned match the scale of the magnetotail), and occasionally a ring current. This is a variation of the simple Luhmann-Friesen magnetosphere model. They are meant to be representative of the basic characteristics of the planetary magnetic fields. Some features NOT included are longitudes of magnetic poles to a standard planetary coordinate system and offsets of the dipole center from the planetary center. ReferencesT. Gold, Motions in the Magnetosphere of the EarthLuhmann and Friesen, A simple model of the magnetosphereLASP: Polarity of planetary magnetic fieldsWikipedia: The Solar Storm of 1859Wikipedia: Kristian BirkelandWikipedia: Carl StørmerSpecial thanks to Arik Posner (NASA/HQ) and Gina DiBraccio (UMBC/GSFC) for helpful pointers on orientation of planetary rotation and magnetic axes. || ", "hits": 203 }, { "id": 4144, "url": "https://svs.gsfc.nasa.gov/4144/", "result_type": "Visualization", "release_date": "2017-07-12T10:00:00-04:00", "title": "Uranus' Magnetosphere", "description": "Earth's magnetic field creates a 'bubble' around Earth that helps protect our planet from some of the more harmful effects of energetic particles streaming out from the sun in the solar wind. Some of the earliest hints of this interaction go back to the 1850s with the work of Richard Carrington, and in the early 1900s with the work of Kristian Birkeland and Carl Stormer. That this field might form a type of 'bubble' around Earth was hypothesized by Sidney Chapman and Vincent Ferraro in the 1930s. The term 'magnetosphere' was applied to magnetic bubble by Thomas Gold in 1959. But it wasn't until the Space Age, when we sent the first probes to other planets, that we found clear evidence of their magnetic fields (though there were hints of a magnetic field for Jupiter in the 1950s, due to observations from radio telescopes). The Voyager program , two spacecraft launched in 1977, and successors to the Pioneer 10 and 11 missions, completed flybys of the giant outer planets. They became the implementation of the 'Grand Tour' of the outer planets originally proposed in the late 1960s. The Voyagers provided some of the first detailed measurments of the strength, extent and diversity of the magnetospheres of the outer planets.In these visualizations, we present simplified models of these planetary magnetospheres, designed to illustrate their scale, and basic features of their structure and impacts of the magnetic axes offset from the planetary rotation axes. The rotation axis of Uranus is tilted over ninety degrees relative to the revolution axis of the solar system, placing it roughly in the plane of the solar system. In addition, the magnetic axis has a large tilt relative to the rotation axis. These effects combine to not only give Uranus a more a more variable magnetosphere, but suggest the planet's magnetic field may be generated by a different mechanism than that of Earth, Jupiter and Saturn.For these visualizations, the magnetic field structure is represented by gold/copper lines. Some additional glyphs are provided to indicate some key directions in the field model.The Yellow arrow points towards the sun. The magnetotail is pointed in the opposite direction.The Cyan arrow represents the magnetic axis, usually tilted relative to the rotation axis. The arrow indicates the NORTH magnetic pole (convention has field lines moving north to south as the north pole of bar magnet (and compass pointer) points to the south magnetic pole).The Blue arrow represents the north rotation axis. It is part of the 3-D axis glyph (red, green, and blue arrows) included to make the planetary rotation more apparent.The semi-transparent grey mesh in the distance represents the boundary of the magnetosphere.Major satellites of the planetary system are also included. When appropriate for the time window of the visualization, the Voyager flyby trajectories are indicated.The models are constructed by combining the fields of a simple magnetic dipole, a current sheet (whose intensity is tuned match the scale of the magnetotail), and occasionally a ring current. This is a variation of the simple Luhmann-Friesen magnetosphere model. They are meant to be representative of the basic characteristics of the planetary magnetic fields. Some features NOT included are longitudes of magnetic poles to a standard planetary coordinate system and offsets of the dipole center from the planetary center. ReferencesT. Gold, Motions in the Magnetosphere of the EarthLuhmann & Friesen, A simple model of the magnetosphereMagnetic reconnection at Uranus' magnetopauseLASP: Polarity of planetary magnetic fieldsWikipedia: The Solar Storm of 1859Wikipedia: Kristian BirkelandWikipedia: Carl StørmerSpecial thanks to Arik Posner (NASA/HQ) and Gina DiBraccio (UMBC/GSFC) for helpful pointers on orientation of planetary rotation and magnetic axes. || ", "hits": 310 }, { "id": 4145, "url": "https://svs.gsfc.nasa.gov/4145/", "result_type": "Visualization", "release_date": "2017-07-12T10:00:00-04:00", "title": "Neptune's Magnetosphere", "description": "Earth's magnetic field creates a 'bubble' around Earth that helps protect our planet from some of the more harmful effects of energetic particles streaming out from the sun in the solar wind. Some of the earliest hints of this interaction go back to the 1850s with the work of Richard Carrington, and in the early 1900s with the work of Kristian Birkeland and Carl Stormer. That this field might form a type of 'bubble' around Earth was hypothesized by Sidney Chapman and Vincent Ferraro in the 1930s. The term 'magnetosphere' was applied to magnetic bubble by Thomas Gold in 1959. But it wasn't until the Space Age, when we sent the first probes to other planets, that we found clear evidence of their magnetic fields (though there were hints of a magnetic field for Jupiter in the 1950s, due to observations from radio telescopes). The Voyager program , two spacecraft launched in 1977, and successors to the Pioneer 10 and 11 missions, completed flybys of the giant outer planets. They became the implementation of the 'Grand Tour' of the outer planets originally proposed in the late 1960s. The Voyagers provided some of the first detailed measurments of the strength, extent and diversity of the magnetospheres of the outer planets.In these visualizations, we present simplified models of these planetary magnetospheres, designed to illustrate their scale, and basic features of their structure and impacts of the magnetic axes offset from the planetary rotation axes. The rotation axis of Neptune is highly tilted relative to the revolution axis of the solar system, but nowhere near as extreme as Uranus. It's magnetic axis also has a large tilt relative to the rotation axis. These effects combine to not only give Uranus a more a more variable magnetosphere, but suggest the planet's magnetic field may be generated by a different mechanism than that of Earth, Jupiter and Saturn.For these visualizations, the magnetic field structure is represented by gold/copper lines. Some additional glyphs are provided to indicate some key directions in the field model.The Yellow arrow points towards the sun. The magnetotail is pointed in the opposite direction.The Cyan arrow represents the magnetic axis, usually tilted relative to the rotation axis. The arrow indicates the NORTH magnetic pole (convention has field lines moving north to south as the north pole of bar magnet (and compass pointer) points to the south magnetic pole).The Blue arrow represents the north rotation axis. It is part of the 3-D axis glyph (red, green, and blue arrows) included to make the planetary rotation more apparent.The semi-transparent grey mesh in the distance represents the boundary of the magnetosphere.Major satellites of the planetary system are also included. When appropriate for the time window of the visualization, the Voyager flyby trajectories are indicated.The models are constructed by combining the fields of a simple magnetic dipole, a current sheet (whose intensity is tuned match the scale of the magnetotail), and occasionally a ring current. This is a variation of the simple Luhmann-Friesen magnetosphere model. They are meant to be representative of the basic characteristics of the planetary magnetic fields. Some features NOT included are longitudes of magnetic poles to a standard planetary coordinate system and offsets of the dipole center from the planetary center. ReferencesT. Gold, Motions in the Magnetosphere of the EarthLuhmann & Friesen, A simple model of the magnetosphereMagnetic reconnection at Neptune's magnetopauseLASP: Polarity of planetary magnetic fieldsWikipedia: The Solar Storm of 1859Wikipedia: Kristian BirkelandWikipedia: Carl StørmerSpecial thanks to Arik Posner (NASA/HQ) and Gina DiBraccio (UMBC/GSFC) for helpful pointers on orientation of planetary rotation and magnetic axes. || ", "hits": 227 }, { "id": 4580, "url": "https://svs.gsfc.nasa.gov/4580/", "result_type": "Visualization", "release_date": "2017-07-07T14:00:00-04:00", "title": "Electromagnetic Waves and Polarization", "description": "Representations of electromagnetic waves of different polarizations: Right circular polarization (upper/right); Linear polarization (middle); and Left circular polarization (lower/left). Yellow arrows are the electric field, green arrows are the magnetic field. || EMWaveTrains_tourX2Oblique_inertial.HD1080i.0900_print.jpg (1024x576) [110.0 KB] || EMWaveTrains_tourX2Oblique_inertial.HD1080i.0900_searchweb.png (320x180) [66.5 KB] || EMWaveTrains_tourX2Oblique_inertial.HD1080i.0900_thm.png (80x40) [4.1 KB] || ThreeWaves (1920x1080) [0 Item(s)] || EMWaveTrains_tourX2Oblique.HD1080i_p30.mp4 (1920x1080) [51.5 MB] || EMWaveTrains_tourX2Oblique.HD1080i_p30.webm (1920x1080) [4.7 MB] || ThreeWaves (3840x2160) [0 Item(s)] || EMWaveTrains_tourX2Oblique_2160p30.mp4 (3840x2160) [165.4 MB] || EMWaveTrains_tourX2Oblique.HD1080i_p30.mp4.hwshow [204 bytes] || ", "hits": 405 }, { "id": 4568, "url": "https://svs.gsfc.nasa.gov/4568/", "result_type": "Visualization", "release_date": "2017-05-18T10:00:00-04:00", "title": "Exploring Reconnection - Guide Field Off", "description": "This visualization shows an oblique view of the reconnection region. Magnetic field direction is represented by the cyan lines. The color trail represents an electron moving in the field. Color of the particle trail represents a dimensionless speed of the particle, with blue for slow and red for fast. || GuideFieldOff_oblique_inertial.HD1080i.0300_print.jpg (1024x576) [118.2 KB] || GuideFieldOff_oblique_inertial.HD1080i.0300_searchweb.png (320x180) [70.8 KB] || GuideFieldOff_oblique_inertial.HD1080i.0300_thm.png (80x40) [4.4 KB] || GuideFieldOff_oblique (1920x1080) [0 Item(s)] || GuideFieldOff_oblique_inertial.HD1080i_p30.mp4 (1920x1080) [6.3 MB] || GuideFieldOff_oblique_inertial.HD1080i_p30.webm (1920x1080) [776.5 KB] || GuideFieldOff_oblique_inertial.HD1080i_p30.mp4.hwshow [208 bytes] || ", "hits": 44 }, { "id": 4569, "url": "https://svs.gsfc.nasa.gov/4569/", "result_type": "Visualization", "release_date": "2017-05-18T10:00:00-04:00", "title": "Exploring Reconnection - Guide Field On", "description": "This visualization shows an oblique view of the reconnection region. Magnetic field direction is represented by the cyan lines. The color trail represents an electron moving in the field. Color of the particle trail represents a dimensionless speed of the particle, with blue for slow and red for fast. || GuideFieldOn_oblique_inertial.HD1080i.0300_print.jpg (1024x576) [129.7 KB] || GuideFieldOn_oblique_inertial.HD1080i.0300_searchweb.png (320x180) [76.2 KB] || GuideFieldOn_oblique_inertial.HD1080i.0300_thm.png (80x40) [4.6 KB] || GuideFieldOn_oblique (1920x1080) [0 Item(s)] || GuideFieldOn_oblique.HD1080i_p30.mp4 (1920x1080) [6.5 MB] || GuideFieldOn_oblique.HD1080i_p30.webm (1920x1080) [761.3 KB] || GuideFieldOn_oblique.HD1080i_p30.mp4.hwshow [198 bytes] || ", "hits": 41 }, { "id": 12591, "url": "https://svs.gsfc.nasa.gov/12591/", "result_type": "Produced Video", "release_date": "2017-05-17T11:00:00-04:00", "title": "NASA's Van Allen Probes Find Human-Made Bubble Shrouding Earth", "description": "Music: Alternate and Parallel by Richard BirkinComplete transcript available. || 12591_VLF_bubbleV3.01194_print.jpg (1024x608) [101.5 KB] || 12591_VLF_bubbleV3.01194_searchweb.png (320x180) [58.6 KB] || 12591_VLF_bubbleV3.01194_thm.png (80x40) [5.6 KB] || 12591_VLF_bubbleV3_appletv.m4v (1280x720) [40.3 MB] || 12591_VLF_bubbleV3_appletv_subtitles.m4v (1280x720) [40.3 MB] || 12591_VLF_bubbleV3_prores.mov (1280x720) [555.6 MB] || 12591_VLF_bubbleV2.en_US.srt [1.3 KB] || 12591_VLF_bubbleV2.en_US.vtt [1.3 KB] || 12591_VLF_bubbleV3.webm (4000x2376) [12.6 MB] || 12591_VLF_bubbleV3_ipod_sm.mp4 (320x240) [15.1 MB] || 12591_VLF_bubbleV3.mov (4000x2376) [3.6 GB] || ", "hits": 65 }, { "id": 12593, "url": "https://svs.gsfc.nasa.gov/12593/", "result_type": "Produced Video", "release_date": "2017-05-17T11:00:00-04:00", "title": "Human Activity Impacted Space Weather", "description": "Music: Hybrid Technology by Le Fat Club [SACEM] Complete transcript available. || 12593_Anthropogenic_Space_WeatherV1_prores.00751_print.jpg (1024x576) [140.4 KB] || 12593_Anthropogenic_Space_WeatherV1_prores.00751_searchweb.png (320x180) [66.5 KB] || 12593_Anthropogenic_Space_WeatherV1_prores.00751_thm.png (80x40) [5.6 KB] || 12593_Anthropogenic_Space_WeatherV1_appletv.m4v (1280x720) [38.4 MB] || 12593_Anthropogenic_Space_WeatherV1_appletv_subtitles.m4v (1280x720) [38.5 MB] || 12593_Anthropogenic_Space_WeatherV1_prores.mov (1280x720) [607.9 MB] || 12593_Anthropogenic_Space_WeatherV1.mp4 (3908x2304) [84.0 MB] || 12593_Anthropogenic_Space_WeatherV1.en_US.srt [1.4 KB] || 12593_Anthropogenic_Space_WeatherV1.en_US.vtt [1.4 KB] || 12593_Anthropogenic_Space_WeatherV1_prores.webm [0 bytes] || 12593_Anthropogenic_Space_WeatherV1_youtube_hq.mov (4032x2376) [578.4 MB] || 12593_Anthropogenic_Space_WeatherV1_ipod_sm.mp4 (320x240) [14.0 MB] || 12593_Anthropogenic_Space_WeatherV1.mov (4032x2376) [4.4 GB] || ", "hits": 49 }, { "id": 4560, "url": "https://svs.gsfc.nasa.gov/4560/", "result_type": "Visualization", "release_date": "2017-03-31T09:00:00-04:00", "title": "Alfvén Waves - Basic", "description": "Alfven waves represented by undulation in the magnetic field vector. || AlfvenWaveBasic_staticXwide_inertial.HD1080i.0300_print.jpg (1024x576) [158.5 KB] || AlfvenWaveBasic_staticXwide_inertial.HD1080i.0300_thm.png (80x40) [4.6 KB] || AlfvenWaveBasic_staticXwide_inertial.HD1080i.0300_web.png (320x180) [71.9 KB] || WavesOnly (1920x1080) [128.0 KB] || AlfvenWaveBasic_staticXwide.HD1080i_p30.mp4 (1920x1080) [34.0 MB] || AlfvenWaveBasic_staticXwide.HD1080i_p30.webm (1920x1080) [4.9 MB] || ", "hits": 251 }, { "id": 4561, "url": "https://svs.gsfc.nasa.gov/4561/", "result_type": "Visualization", "release_date": "2017-03-31T09:00:00-04:00", "title": "Alfvén Waves - Kinetic", "description": "Kinetic Alfven waves represented by undulation in the magnetic field vector. || AlfvenWaveKinetic_staticXwide_inertial.HD1080i.0300_print.jpg (1024x576) [155.7 KB] || WavesOnly (1920x1080) [128.0 KB] || AlfvenWaveKinetic_staticXwide.HD1080i_p30.mp4 (1920x1080) [37.9 MB] || AlfvenWaveKinetic_staticXwide.HD1080i_p30.webm (1920x1080) [4.9 MB] || ", "hits": 82 }, { "id": 12512, "url": "https://svs.gsfc.nasa.gov/12512/", "result_type": "Produced Video", "release_date": "2017-03-31T09:00:00-04:00", "title": "Observations Reshape Basic Plasma Wave Physics", "description": "Music credit: Coolheaded by Jeff CardoniComplete transcript available. || 12512_Observations_Reshape_Basic_Plasma_Wave_Physics_V5_prores.00282_print.jpg (1024x576) [26.7 KB] || 12512_Observations_Reshape_Basic_Plasma_Wave_Physics_V5_prores.00282_searchweb.png (320x180) [16.4 KB] || 12512_Observations_Reshape_Basic_Plasma_Wave_Physics_V5_prores.00282_thm.png (80x40) [2.5 KB] || 12512_Observations_Reshape_Basic_Plasma_Wave_Physics_V5.webm (960x540) [31.9 MB] || 12512_Observations_Reshape_Basic_Plasma_Wave_Physics_V5_appletv.m4v (1280x720) [46.8 MB] || 12512_Observations_Reshape_Basic_Plasma_Wave_Physics_V5_large.mp4 (1920x1080) [83.0 MB] || 12512_Observations_Reshape_Basic_Plasma_Wave_Physics_V5_prores.mov (1280x720) [1.0 GB] || 12512_Observations_Reshape_Basic_Plasma_Wave_Physics_V5_youtube_hq.mov (1920x1080) [141.1 MB] || 12512_Observations_Reshape_Basic_Plasma_Wave_Physics_V5_appletv_subtitles.m4v (1280x720) [46.9 MB] || 12512_Observations_Reshape_Basic_Plasma_Wave_Physics_V3.en_US.srt [1.6 KB] || 12512_Observations_Reshape_Basic_Plasma_Wave_Physics_V3.en_US.vtt [1.6 KB] || 12512_Observations_Reshape_Basic_Plasma_Wave_Physics_V5_ipod_sm.mp4 (320x240) [15.0 MB] || ", "hits": 43 }, { "id": 12550, "url": "https://svs.gsfc.nasa.gov/12550/", "result_type": "Produced Video", "release_date": "2017-03-30T09:00:00-04:00", "title": "Rossby Waves on the Sun Could Aid in Space Weather Prediction", "description": "Music: Grand Design by Michael ConnComplete transcript available. || 12550_Rossby_Waves_MASTER_prores.00696_print.jpg (1024x576) [127.0 KB] || 12550_Rossby_Waves_MASTER_prores.00696_searchweb.png (320x180) [53.3 KB] || 12550_Rossby_Waves_MASTER_prores.00696_thm.png (80x40) [4.8 KB] || 12550_Rossby_Waves_MASTER_prores.mov (1280x720) [656.3 MB] || 12550_Rossby_Waves_MASTER_youtube_hq.mov (1920x1080) [165.2 MB] || 12550_Rossby_Waves_MASTER_appletv.m4v (1280x720) [19.9 MB] || 12550_Rossby_Waves_MASTER.mpeg (1280x720) [158.7 MB] || 12550_Rossby_Waves_MASTER_appletv_subtitles.m4v (1280x720) [20.0 MB] || 12550_Rossby_Waves_MASTER_youtube_hq.en_US.srt [763 bytes] || 12550_Rossby_Waves_MASTER_youtube_hq.en_US.vtt [776 bytes] || 12550_Rossby_Waves_MASTER_ipod_sm.mp4 (320x240) [7.4 MB] || 12550_Rossby_Waves_MASTER_prores.webm [0 bytes] || ", "hits": 21 }, { "id": 4557, "url": "https://svs.gsfc.nasa.gov/4557/", "result_type": "Visualization", "release_date": "2017-03-15T10:00:00-04:00", "title": "Leaky Radiation Belts", "description": "This visualization opens with a full view of the radiation belt of trapped electrons circling Earth. We open a slice of the belts, to display a cross-section for clarity and move the camera to a more equatorial view. Earth rotation and solar motion have been turned off for this visualization to reduce distracting additional motions. || LeakyBelts_FullData_ObliqueIntro.slate_CRTT.HD1080i.0600_print.jpg (1024x576) [113.8 KB] || LeakyBelts_FullData_ObliqueIntro.slate_CRTT.HD1080i.0600_searchweb.png (180x320) [83.0 KB] || LeakyBelts_FullData_ObliqueIntro.slate_CRTT.HD1080i.0600_thm.png (80x40) [6.0 KB] || ObliqueIntro (1920x1080) [0 Item(s)] || LeakyBelts_FullData_ObliqueIntro.HD1080i_p30.mp4 (1920x1080) [77.0 MB] || LeakyBelts_FullData_ObliqueIntro.HD1080i_p30.webm (1920x1080) [5.5 MB] || ObliqueIntro (3840x2160) [0 Item(s)] || LeakyBelts_FullData_ObliqueIntro.UHD2160_p30.mp4 (3840x2160) [279.0 MB] || LeakyBelts_FullData_ObliqueIntro.HD1080i_p30.mp4.hwshow [210 bytes] || ", "hits": 66 }, { "id": 4549, "url": "https://svs.gsfc.nasa.gov/4549/", "result_type": "Visualization", "release_date": "2017-02-09T10:00:00-05:00", "title": "MMS Phase 2b: Transitioning to Magnetosphere Science on the Darkside", "description": "Visualization of the spacecraft orbit transition from apogee at the dayside magnetopause to the nightside magnetopause. || MMSPhase2b_Pole_Jan2May2017_RE_GSE.slate_GSEtour.UHD3840.3660_print.jpg (1024x576) [103.1 KB] || MMSPhase2b_Pole_Jan2May2017_RE_GSE.slate_GSEtour.UHD3840.3660_searchweb.png (320x180) [72.9 KB] || MMSPhase2b_Pole_Jan2May2017_RE_GSE.slate_GSEtour.UHD3840.3660_thm.png (80x40) [5.2 KB] || MMSPhase2b_Pole_Jan2May2017_Fast.HD1080i_p30.webm (1920x1080) [23.0 MB] || FastVersion (1920x1080) [0 Item(s)] || MMSPhase2b_Pole_Jan2May2017_Fast.HD1080i_p30.mp4 (1920x1080) [140.4 MB] || FastVersion (3840x2160) [0 Item(s)] || MMSPhase2b_Pole_Jan2May2017.UHD3840_2160p30.mp4 (3840x2160) [449.6 MB] || MMSPhase2b_Pole_Jan2May2017_Fast.HD1080i_p30.mp4.hwshow [210 bytes] || ", "hits": 32 }, { "id": 4513, "url": "https://svs.gsfc.nasa.gov/4513/", "result_type": "Visualization", "release_date": "2016-11-14T13:00:00-05:00", "title": "Shock Drift Acceleration (SDA)", "description": "This visualization of particle acceleration across a shock is a simplied representation of shock drift acceleration (SDA) showing the motion of electrons (yellow) and protons (blue). It is presented with the same color table designations as other critters in our Plasma Zoo. || SDAShock_tour_inertial.HD1080i.1000_print.jpg (1024x576) [124.6 KB] || SDAShock_tour_inertial.HD1080i.1000_searchweb.png (320x180) [83.0 KB] || SDAShock_tour_inertial.HD1080i.1000_thm.png (80x40) [5.3 KB] || StandardVersion (1920x1080) [0 Item(s)] || SDAShock_tour_standard.HD1080i_p30.mp4 (1920x1080) [72.8 MB] || SDAShock_tour_standard.HD1080i_p30.webm (1920x1080) [7.1 MB] || StandardVersion (3840x2160) [0 Item(s)] || SDAShock_tour_standard.UHD3840_2160p30.mp4 (3840x2160) [232.9 MB] || SDAShock_tour_standard.HD1080i_p30.mp4.hwshow [200 bytes] || ", "hits": 99 } ] }