{ "count": 82, "next": null, "previous": null, "results": [ { "id": 14907, "url": "https://svs.gsfc.nasa.gov/14907/", "result_type": "Produced Video", "release_date": "2025-09-30T14:00:00-04:00", "title": "What is space weather?", "description": "Though it is almost 100 million miles away from Earth, the Sun influences our daily lives in ways you may not realize.A farmer stops their planting operations due to poor GPS signal for their autonomous tractor. A power grid manager changes the configuration of their network to ensure a blackout doesn’t occur due to voltage instability. A pilot switches to back-up communication equipment due to loss of high-frequency radio. A commercial internet company providing service to the military must change the orbit of their spacecraft to avoid a collision due to increased atmospheric drag.These are a few examples of the ways the Sun influences our everyday lives. This is what we define as space weather – the conditions of the space environment driven by the Sun and its impacts on objects in the solar system. || ", "hits": 226 }, { "id": 5375, "url": "https://svs.gsfc.nasa.gov/5375/", "result_type": "Visualization", "release_date": "2025-08-07T14:00:00-04:00", "title": "Carrington Class Coronal Mass Ejection - ENLIL Simulation of A Series of CMEs", "description": "A series of visualizations of the simulation of a series of CMEs between July 2012 and August 2012, including a carrington class coronal mass ejection that hit STEREO-A.", "hits": 331 }, { "id": 14863, "url": "https://svs.gsfc.nasa.gov/14863/", "result_type": "Produced Video", "release_date": "2025-07-17T09:00:00-04:00", "title": "Quickshot: New NASA Mission Launching Soon To Study Earth’s Space Weather Shield", "description": "Scroll down page for advisory with suggested questions and anchor intro. You will also find the associated cut b-roll and pre-recorded soundbites below.Click here for more information about TRACERS || Live_Shot_Banner_TRACERS_final.jpg (1800x720) [256.8 KB] || Live_Shot_Banner_TRACERS_final_print.jpg (1024x409) [150.1 KB] || Live_Shot_Banner_TRACERS_final_searchweb.png (320x180) [82.8 KB] || Live_Shot_Banner_TRACERS_final_thm.png (80x40) [6.5 KB] || ", "hits": 98 }, { "id": 5555, "url": "https://svs.gsfc.nasa.gov/5555/", "result_type": "Visualization", "release_date": "2025-07-15T10:00:00-04:00", "title": "TRACERS through Earth's Polar Cusps", "description": "Visualization of the orbit of the twin TRACERS (Tandem Reconnection and Cusp Electrodynamics Reconnaissance Satellites) satellites that will explore the process of magnetic reconnection in Earth's polar regions and its effects on our atmosphere.", "hits": 166 }, { "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": 180 }, { "id": 5435, "url": "https://svs.gsfc.nasa.gov/5435/", "result_type": "Visualization", "release_date": "2024-12-12T12:00:00-05:00", "title": "Geomagnetic and Atmospheric Response to May 2024 Solar Storm", "description": "This visualization shows the Earth's magnetosphere being hit by a geomagnetic storm. The MAGE model simulates real events that happened throughout May 10-11, 2024.White orbit trails: All satellites orbiting Earth during the stormOrange orbits: Proposed orbits for six GDC spacecraftOrange-to-purple lines: Magnetic field lines around EarthBlue trails: Solar wind velocity tracersGreen clouds: Electric field current intensityCredit:NASA Scientific Visualization Studio and NASA DRIVE Science Center for Geospace Storms || multiField_11-25-2024b_magnetosphere_pc_anim_satellites_4k.00450_print.jpg (1024x576) [191.2 KB] || multiField_11-25-2024b_magnetosphere_pc_anim_satellites_4k.00450_searchweb.png (320x180) [102.0 KB] || multiField_11-25-2024b_magnetosphere_pc_anim_satellites_4k.00450_web.png (320x180) [102.0 KB] || multiField_11-25-2024b_magnetosphere_pc_anim_satellites_4k.00450_thm.png (80x40) [6.4 KB] || multiField_12-30-2024b_magnetosphere_pc_anim_satellites_1080p30.mp4 (1920x1080) [253.6 MB] || multiField_12-30-2024b_magnetosphere_pc_anim_satellites_3x3Hyperwall (5760x3240) [2880 Item(s)] || multiField_12-30-2024b_magnetosphere_pc_anim_satellites_3x3Hyperwall_2160p30.mp4 (3840x2160) [773.4 MB] || multiField_12-30-2024b_magnetosphere_pc_anim_satellites_3x3Hyperwall_3240p30_h265.mp4 (5760x3240) [779.4 MB] || ", "hits": 308 }, { "id": 14706, "url": "https://svs.gsfc.nasa.gov/14706/", "result_type": "Produced Video", "release_date": "2024-11-08T13:00:00-05:00", "title": "NASA's Illuminate Series (2024)", "description": "NASA's Illuminate is a video series about out-of-this-world images that shine light on our Sun and solar system. || ", "hits": 109 }, { "id": 31319, "url": "https://svs.gsfc.nasa.gov/31319/", "result_type": "Hyperwall Visual", "release_date": "2024-10-23T00:00:00-04:00", "title": "2025 NASA Science Calendar", "description": "Images from the 2025 NASA Science Calendar", "hits": 104 }, { "id": 5238, "url": "https://svs.gsfc.nasa.gov/5238/", "result_type": "Visualization", "release_date": "2024-06-27T11:00:00-04:00", "title": "Our Active Ionosphere", "description": "In this view of Earth on October 7, 2019, just past sunset, GOLD observed an X-shaped structure in the equatorial ionization anomaly. || GOLD_O5S_20191007.00034_print.jpg (1024x576) [76.3 KB] || GOLD_O5S_20191007 [0 Item(s)] || GOLD_O5S_20191007_1080p4.mp4 (1920x1080) [1.8 MB] || ", "hits": 158 }, { "id": 5214, "url": "https://svs.gsfc.nasa.gov/5214/", "result_type": "Visualization", "release_date": "2024-02-08T08:00:00-05:00", "title": "Geomagnetic Storm Causes Satellite Loss for Fulldome", "description": "In February 2022, a Coronal Mass Ejection led to 38 commercial satellites being lost. Solar plasma from a geomagnetic storm heated the atmosphere, causing denser gases to expand into the satellites’ orbit, which increased atmospheric drag on the satellites and caused them to de-orbit. Johns Hopkins APL-led Center for Geospace Storms (CGS) is building a Multiscale Atmosphere-Geospace Environment (MAGE) supercomputer model to predict space weather. The physics-based MAGE simulation reproduced the storm-time atmospheric density enhancement much better than empirical or standalone ionosphere-thermosphere models, emphasizing the need for fully-coupled whole-of-geospace models for predicting space weather events.This is 4k fulldome imagery intended for projection in a planetarium or other hemispherical dome theater. || ", "hits": 181 }, { "id": 5193, "url": "https://svs.gsfc.nasa.gov/5193/", "result_type": "Visualization", "release_date": "2023-12-11T09:00:00-05:00", "title": "Geomagnetic Storm Causes Satellite Loss", "description": "In February 2022, a Coronal Mass Ejection led to 38 commercial satellites being lost. Solar plasma from a geomagnetic storm heated the atmosphere, causing denser gases to expand into the satellites’ orbit, which increased atmospheric drag on the satellites and caused them to de-orbit. Johns Hopkins APL-led Center for Geospace Storms (CGS) is building a Multiscale Atmosphere-Geospace Environment (MAGE) supercomputer model to predict space weather. The physics-based MAGE simulation reproduced the storm-time atmospheric density enhancement much better than empirical or standalone ionosphere-thermosphere models, emphasizing the need for fully-coupled whole-of-geospace models for predicting space weather events. || ", "hits": 534 }, { "id": 40507, "url": "https://svs.gsfc.nasa.gov/gallery/hyperwall-power-playlist-heliophysics-focus/", "result_type": "Gallery", "release_date": "2023-08-28T00:00:00-04:00", "title": "Hyperwall Power Playlist - Heliophysics Focus", "description": "This is a collection of our most powerful, newsworthy, and frequently used Hyperwall-ready visualizations, along with several that haven't gotten the attention they deserve. They're especially great for more general or top-level science talks, or to \"set the scene\" before a deep dive into a more focused subject or dataset. We've tried to cover the subject areas our speakers focus on most. \n\nIf you're not seeing what you're looking for, there is a huge library of visualizations more localized or specialized in subject - please use the Search function above, and filter \"Result type\" for \"Hyperwall Visual.\"\n\n If you'd like to use one of these visualizations in your Hyperwall presentation, we'll need to know which element on which page. On the visualization's web page, below the visual you'd like to use, you'll see a Link icon next to the Download button. All we need is for you to click on that icon and include that link in your presentation Powerpoint/Keynote or visualization list. Additionally, please check our Hyperwall How-To Guide for tips on designing your Hyperwall presentation, file specifications, and Powerpoint/Keynote templates.", "hits": 186 }, { "id": 4917, "url": "https://svs.gsfc.nasa.gov/4917/", "result_type": "Visualization", "release_date": "2021-11-29T11:00:00-05:00", "title": "ICON Snaps a Peek at the Ionospheric Dynamo", "description": "Visualization of ICON in Earth orbit, camera ahead of the spacecraft looking back on spacecraft and limb of Earth. Magenta curves are lines of Earth's geomagnetic field. Field-of-view (FOV) of MIGHTI imagers (green frustums) and the longitudinal wind vectors (green arrows) it measures are shown. MIGHTI imagers FOV eventually fades out. Vertical plasma speed (red arrows) is measured at the spacecraft. Magnetic field lines turn yellow as measurements of winds by MIGHT provide a connection to influence the plasma velocity measured at the spacecraft, redirecting the plasma flow from upward to downward. || ICONDataView.ICONSyncView+x_.clockSlate_CRTT.HD1080i.000750_print.jpg (1024x576) [135.0 KB] || ICONDataView.ICONSyncView+x_.clockSlate_CRTT.HD1080i.000750_searchweb.png (320x180) [79.4 KB] || ICONDataView.ICONSyncView+x_.clockSlate_CRTT.HD1080i.000750_thm.png (80x40) [5.7 KB] || ICONSyncView+x (1920x1080) [0 Item(s)] || ICONDataView.ICONSyncView+x.HD1080i_p30.mp4 (1920x1080) [36.4 MB] || ICONDataView.ICONSyncView+x.HD1080i_p30.webm (1920x1080) [5.1 MB] || ICONSyncView+x (3840x2160) [0 Item(s)] || ICONDataView.ICONSyncView+x.2160p30.mp4 (3840x2160) [114.3 MB] || ICONDataView.ICONSyncView+x.HD1080i_p30.mp4.hwshow || ", "hits": 67 }, { "id": 4840, "url": "https://svs.gsfc.nasa.gov/4840/", "result_type": "Visualization", "release_date": "2020-08-17T11:00:00-04:00", "title": "South Atlantic Anomaly: 2015 through 2025", "description": "South Atlantic Anomaly from 2015 through 2025 showing the geomagnetic intensity at the Earth's surface and the core-mantle boundary. There are versions that include the dates and colorbars and versions without the date and colorbat.This video is also available on our YouTube channel. || saa_intensity_comp2160_p60.4898_print.jpg (1024x576) [58.0 KB] || saa_intensity_comp2160_p60.4898_print_searchweb.png (320x180) [49.9 KB] || saa_intensity_comp2160_p60.4898_print_thm.png (80x40) [3.8 KB] || saa_intensity_comp_1080p30.mp4 (1920x1080) [31.9 MB] || saa_intensity_comp_1080p60.mp4 (1920x1080) [34.4 MB] || saa_intensity_dataOnly_1080_p30.mp4 (1920x1080) [29.3 MB] || saa_intensity_dataOnly_1080_p60.mp4 (1920x1080) [31.3 MB] || saa_intensity_dataOnly_1080_p30.webm (1920x1080) [9.1 MB] || dataOnly (1920x1080) [0 Item(s)] || saa_intensity_comp2160_p30.mp4 (3840x2160) [86.1 MB] || saa_intensity_comp2160_p60.mp4 (3840x2160) [93.1 MB] || comp (3840x2160) [0 Item(s)] || captions_silent.29860.en_US.srt [43 bytes] || saa_intensity_dataOnly_1080_p30.mp4.hwshow [197 bytes] || ", "hits": 1163 }, { "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": 123 }, { "id": 13502, "url": "https://svs.gsfc.nasa.gov/13502/", "result_type": "Produced Video", "release_date": "2019-12-10T17:00:00-05:00", "title": "AGU 2019 — Postcards from the edge of space: New images, new phenomena, and new insights", "description": "In a Dec. 10 press event at the fall meeting of the American Geophysical Union in San Francisco, California, three scientists presented new images of the ionosphere, the dynamic region where Earth’s atmosphere meets space. Home to astronauts and everyday technology like radio and GPS, the ionosphere constantly responds to changes from space above and Earth below.The collection of images presented include the first images from NASA’s ICON, new science results from NASA’s GOLD, and observations of a fleeting, never-before-studied aurora. Together, they bring color to invisible processes that have widespread implications for the part of space that is closest to home.SPEAKERS:• Jennifer Briggs, Pepperdine University, Malibu, California, United States• Richard Eastes, University of Colorado Boulder, Boulder, Colorado, United States• Thomas Immel, University of California Berkeley, Berkeley, California, United States || ", "hits": 63 }, { "id": 4737, "url": "https://svs.gsfc.nasa.gov/4737/", "result_type": "Visualization", "release_date": "2019-07-17T11:00:00-04:00", "title": "Observing Earth's Ionosphere with GOLD", "description": "A visualization of GOLD data observing Earth's ionosphere in ultraviolet light around the wavelength of an atomic oxygen emission. || GOLDData201903.GOLDview_O5S.clockSlate_CRTT.UHD3840.000267_print.jpg (1024x576) [70.4 KB] || GOLD_March2019_animated.gif (1042x586) [5.5 MB] || GOLDData201903.GOLDview_O5S.clockSlate_CRTT.UHD3840.000267_searchweb.png (320x180) [72.3 KB] || GOLDData201903.GOLDview_O5S.clockSlate_CRTT.UHD3840.000267_thm.png (80x40) [5.4 KB] || GOLDData201903.GOLDview_O5S.HD1080i_p10.mp4 (1920x1080) [24.0 MB] || basic (1920x1080) [0 Item(s)] || GOLDData201903.GOLDview_O5S.HD1080i_p10.webm (1920x1080) [3.1 MB] || basic (3840x2160) [0 Item(s)] || GOLDData201903.GOLDview_O5S_2160p10.mp4 (3840x2160) [72.0 MB] || ", "hits": 83 }, { "id": 13221, "url": "https://svs.gsfc.nasa.gov/13221/", "result_type": "Produced Video", "release_date": "2019-06-10T10:00:00-04:00", "title": "NASA Tech on SpaceX Falcon Heavy Launch - Media Telecon Resources", "description": "NASA is sending four technology missions that will help improve future spacecraft design and performance into space on the next SpaceX Falcon Heavy rocket launch. Experts will discuss these technologies, and how they complement NASA’s Moon to Mars exploration plans, during a media teleconference Monday, June 10 at 1 p.m. EDT.Audio of the teleconference will be streamed live online at: https://www.nasa.gov/liveParticipants in the briefing will be:Jim Reuter, acting associate administrator of NASA’s Space Technology Mission Directorate, will discuss how technology drives exploration to the Moon and beyond.Jill Seubert, deputy principal investigator for the Deep Space Atomic Clock at NASA’s Jet Propulsion Laboratory, will discuss how to advance exploration in deep space with a miniaturized, ultra-precise, mercury-ion atomic clock that is orders of magnitude more stable than today’s best navigation clocks.Don Cornwell, director of the Advanced Communications and Navigation Division of NASA’s Space Communications and Navigation program, will discuss how a more stable, space-based atomic clock could benefit future missions to the Moon and Mars.Christopher McLean, principal investigator for NASA’s Green Propellant Infusion Mission (GPIM) at Ball Aerospace, will discuss the demonstration of a green alternative to conventional chemical propulsion systems for next-generation launch vehicles and spacecraft. Joe Cassady, executive director for space at Aerojet Rocketdyne, will discuss the five thrusters and propulsion system aboard GPIM.Nicola Fox, director of the Heliophysics Division of NASA’s Science Mission Directorate, will discuss Space Environment Testbeds and the importance of protecting satellites from space radiation.Richard Doe, payload program manager for the Enhanced Tandem Beacon Experiment at SRI International, will discuss how a pair of NASA CubeSats will work with six satellites of the National Oceanographic and Atmospheric Administration’s (NOAA’s) COSMIC-2 mission to study disruptions of signals that pass through Earth’s upper atmosphere.To participate in the teleconference, media must contact Clare Skelly at 202-358-4273 or clare.a.skelly@nasa.gov by 10 a.m. June 10. Media questions may be submitted on Twitter during the teleconference using the hashtag #askNASA.NASA’s four missions will share a ride on the Falcon Heavy with about 20 satellites from government and research institutions that make up the Department of Defense’s Space Test Program-2 (STP-2) mission. SpaceX and the U.S. Air Force Space and Missile Systems Center, which manages STP-2, are targeting 11:30 p.m. Saturday, June 22, for launch from historic Launch Complex 39A at NASA’s Kennedy Space Center in Florida.Charged with returning astronauts to the Moon within five years, NASA’s Artemis lunar exploration plans are based on a two-phase approach: the first is focused on speed – landing astronauts on the Moon by 2024 – while the second will establish a sustained human presence on and around the Moon by 2028. We will use what we learn on the Moon to prepare to send astronauts to Mars. The technology missions on this launch will advance a variety of future exploration missions.For more information about NASA’s Moon to Mars exploration plans, visit:https://www.nasa.gov/moontomarsFor more information about the NASA technologies aboard this launch, visit:https://www.nasa.gov/spacexLearn more about NASA’s Deep Space Atomic Clock: https://www.nasa.gov/mission_pages/tdm/clock/index.htmlLearn more about NASA’s Green Propellant Infusion Mission: https://www.nasa.gov/mission_pages/tdm/green/index.htmlSPACE TEST PROGRAM-2 || ", "hits": 98 }, { "id": 12986, "url": "https://svs.gsfc.nasa.gov/12986/", "result_type": "Produced Video", "release_date": "2018-07-23T11:00:00-04:00", "title": "Mars Proton Aurora", "description": "On Earth, the northern and southern lights occur when the solar wind (electrically charged particles from the Sun) follow our planet's geomagnetic field lines to the poles and collide with the upper atmosphere. Mars lacks a global magnetic field, so instead the solar wind piles up in front of Mars in a bow shock, which blocks charged particles from reaching the bulk of the atmosphere. However, in a process first observed by the MAVEN mission, some solar wind protons can slip past the bow shock by first bonding with electrons from the Mars upper atmosphere to form hydrogen atoms. Because these hydrogen atoms are electrically neutral, they can pass through the bow shock and go on to create an ultraviolet proton aurora on the dayside of Mars.Learn more about MAVEN's observation of a proton aurora at Mars. || ", "hits": 109 }, { "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": 427 }, { "id": 4617, "url": "https://svs.gsfc.nasa.gov/4617/", "result_type": "Visualization", "release_date": "2018-01-31T14:00:00-05:00", "title": "Interface to Space: The Equatorial Fountain", "description": "Visualization illustrating the Fountain Effect of ions in the near-Earth electric and magnetic fields. || IRIConceptual.Limb2PullOut_OionFountainIGRF.noslate_CRTT.HD1080i.000660_print.jpg (1024x576) [114.5 KB] || IRIConceptual.Limb2PullOut_OionFountainIGRF.noslate_CRTT.HD1080i.000660_searchweb.png (320x180) [87.8 KB] || IRIConceptual.Limb2PullOut_OionFountainIGRF.noslate_CRTT.HD1080i.000660_thm.png (80x40) [7.2 KB] || 1920x1080_16x9_30p (1920x1080) [0 Item(s)] || IRIConceptual.Limb2PullOut_OionFountainIGRF.HD1080i_p30.mp4 (1920x1080) [32.1 MB] || IRIConceptual.Limb2PullOut_OionFountainIGRF.HD1080i_p30.webm (1920x1080) [4.2 MB] || 3840x2160_16x9_30p (3840x2160) [0 Item(s)] || IRIConceptual.Limb2PullOut_OionFountainIGRF_2160p30.mp4 (3840x2160) [96.1 MB] || IRIConceptual.Limb2PullOut_OionFountainIGRF.HD1080i_p30.mp4.hwshow [221 bytes] || ", "hits": 90 }, { "id": 4610, "url": "https://svs.gsfc.nasa.gov/4610/", "result_type": "Visualization", "release_date": "2018-01-19T15:00:00-05:00", "title": "GOLD: Instrument Scanning Coverage", "description": "Visualization of GOLD orbiting Earth with image scanning. This version presents the singly-ionized oxygen density from the IRI model. || IRIGOLDscan.GOLDview3_Oion.clockSlate_CRTT.HD1080i.001400_print.jpg (1024x576) [90.3 KB] || IRIGOLDscan.GOLDview3_Oion.clockSlate_CRTT.HD1080i.001400_searchweb.png (320x180) [79.2 KB] || IRIGOLDscan.GOLDview3_Oion.clockSlate_CRTT.HD1080i.001400_thm.png (80x40) [6.1 KB] || 1920x1080_16x9_30p (1920x1080) [0 Item(s)] || IRIGOLDscan.GOLDview4_Oion.HD1080i_p30.mp4 (1920x1080) [38.5 MB] || IRIGOLDscan.GOLDview4_Oion.HD1080i_p30.webm (1920x1080) [10.0 MB] || IRIGOLDscan.GOLDview4_Oion.HD1080i_p30.mp4.hwshow [204 bytes] || ", "hits": 153 }, { "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": 82 }, { "id": 4594, "url": "https://svs.gsfc.nasa.gov/4594/", "result_type": "Visualization", "release_date": "2017-10-31T10:00:00-04:00", "title": "ICON Scans the Ionosphere", "description": "ICON orbits Earth at 575 kilometers altitude, measuring the composition and motions of the ionosphere. || IRIDaily.limbwICON_OionHwindIGRF.clockSlate_CRTT.HD1080i.000870_print.jpg (1024x576) [105.7 KB] || IRIDaily.limbwICON_OionHwindIGRF.clockSlate_CRTT.HD1080i.000870_searchweb.png (320x180) [63.8 KB] || IRIDaily.limbwICON_OionHwindIGRF.clockSlate_CRTT.HD1080i.000870_thm.png (80x40) [5.0 KB] || 1920x1080_16x9_30p (1920x1080) [0 Item(s)] || IRIDaily.limbwICON_OionHwindIGRF.HD1080i_p30.mp4 (1920x1080) [76.4 MB] || IRIDaily.limbwICON_OionHwindIGRF.HD1080i_p30.webm (1920x1080) [10.9 MB] || 3840x2160_16x9_30p (3840x2160) [0 Item(s)] || IRIDaily.limbwICON_OionHwindIGRF.UHD3840_2160p30.mp4 (3840x2160) [217.4 MB] || IRIDaily.limbwICON_OionHwindIGRF.HD1080i_p30.mp4.hwshow [210 bytes] || ", "hits": 113 }, { "id": 4539, "url": "https://svs.gsfc.nasa.gov/4539/", "result_type": "Visualization", "release_date": "2017-01-13T10:00:00-05:00", "title": "Exploring Earth's Ionosphere: Limb view with approach", "description": "Oxygen ion enhancements at 350km altitude, ionospheric winds at altitudes of 100 km (white) and 350 km (violet) and the low-latitude geomagnetic field. || IRIDaily.zoom2limb_OionHwindIGRF.clockSlate_CRTT.HD1080i.000400_print.jpg (1024x576) [92.1 KB] || IRIDaily.zoom2limb_OionHwindIGRF.clockSlate_CRTT.HD1080i.000400_searchweb.png (320x180) [58.1 KB] || IRIDaily.zoom2limb_OionHwindIGRF.clockSlate_CRTT.HD1080i.000400_thm.png (80x40) [4.9 KB] || IRIDaily.zoom2limb_OionHwindIGRF.HD1080i_p30.mp4 (1920x1080) [89.8 MB] || OionHwindIGRF (1920x1080) [0 Item(s)] || IRIDaily.zoom2limb_OionHwindIGRF.HD1080i_p30.webm (1920x1080) [8.6 MB] || OionHwindIGRF (3840x2160) [0 Item(s)] || IRIDaily.zoom2limb_OionHwindIGRF.2160p30.mp4 (3840x2160) [274.0 MB] || IRIDaily.zoom2limb_OionHwindIGRF.HD1080i_p30.mp4.hwshow [210 bytes] || ", "hits": 60 }, { "id": 4540, "url": "https://svs.gsfc.nasa.gov/4540/", "result_type": "Visualization", "release_date": "2017-01-13T10:00:00-05:00", "title": "Exploring Earth's Ionosphere: Limb view", "description": "This visualization presents data on the concentration of the singly-ionized oxygen atom (rainbow color table, red is highest concentration), the low-latitude geomagnetic field (gold field lines) and the ionospheric winds at two altitude levels, 100km (white) and 350 km (violet). || IRIDaily.limb_OionHwindIGRF.clockSlate_CRTT.HD1080i.000750_print.jpg (1024x576) [101.4 KB] || IRIDaily.limb_OionHwindIGRF.clockSlate_CRTT.HD1080i.000750_thm.png (80x40) [5.0 KB] || IRIDaily.limb_OionHwindIGRF.clockSlate_CRTT.HD1080i.000750_searchweb.png (320x180) [62.5 KB] || IRIDaily.limb_OionHwindIGRF.HD1080i_p30.mp4 (1920x1080) [88.3 MB] || OionHwindIGRF (1920x1080) [0 Item(s)] || OionHwindIGRF (3840x2160) [0 Item(s)] || IRIDaily.limb_OionHwindIGRF.2160p30.webm (3840x2160) [12.4 MB] || IRIDaily.limb_OionHwindIGRF.2160p30.mp4 (3840x2160) [274.0 MB] || IRIDaily.limb_OionHwindIGRF.HD1080i_p30.mp4.hwshow [205 bytes] || ", "hits": 67 }, { "id": 4541, "url": "https://svs.gsfc.nasa.gov/4541/", "result_type": "Visualization", "release_date": "2016-12-30T00:00:00-05:00", "title": "Ocean Tides and Magnetic Fields", "description": "Earth’s magnetic field is built up from many contributing sources ranging from the planet’s core to the magnetosphere in space. Untangling and identifying the different sources allows geomagnetic scientists to gather information about the individual processes that combine to create the full field.One contributor is the ocean. But how do the tides affect Earth’s magnetic field? Seawater is an electrical conductor, and therefore interacts with the magnetic field. As the tides cycle around the ocean basins, the ocean water essentially tries to pull the geomagnetic field lines along. Because the salty water is a good, but not great, conductor, the interaction is relatively weak. The strongest component is from the regular lunar tide that happens about twice per day (actually 12.42 hours). Other contributions come from ocean swell, eddies, and even tsunamis.The strength of the interaction also depends on the temperature of the ocean water. Scientists are now able to determine how much heat is being stored in the entire ocean, from wave top to sea floor by observations of the Earth's magnetic field. || ", "hits": 214 }, { "id": 4527, "url": "https://svs.gsfc.nasa.gov/4527/", "result_type": "Visualization", "release_date": "2016-12-14T14:00:00-05:00", "title": "ICON and GOLD: Instrument Scanning Coverage", "description": "Visualization of ICON and GOLD orbiting Earth with image scanning. This version presents several geospace models, including the singly-ionized oxygen density, the low-latitude geomagnetic field, and the high-altitude winds (100km and 350km altitudes). || IRIGOLDscan.GOLDview3_OionHwindIGRF.clockSlate_CRTT.UHD3840.001140_print.jpg (1024x576) [130.5 KB] || IRIGOLDscan.GOLDview3_OionHwindIGRF.clockSlate_CRTT.UHD3840.001140_searchweb.png (320x180) [85.0 KB] || IRIGOLDscan.GOLDview3_OionHwindIGRF.clockSlate_CRTT.UHD3840.001140_thm.png (80x40) [5.9 KB] || IRIGOLDscan.GOLDview3_OionHwindIGRF.HD1080i_p30.mp4 (1920x1080) [82.0 MB] || IRIGOLDscan.GOLDview3_OionHwindIGRF (1920x1080) [0 Item(s)] || IRIGOLDscan.GOLDview3_OionHwindIGRF.HD1080i_p30.webm (1920x1080) [7.6 MB] || IRIGOLDscan.GOLDview3_OionHwindIGRF (3840x2160) [0 Item(s)] || IRIGOLDscan.GOLDview3_OionHwindIGRF_2160p30.mp4 (3840x2160) [258.1 MB] || ", "hits": 61 }, { "id": 12457, "url": "https://svs.gsfc.nasa.gov/12457/", "result_type": "Produced Video", "release_date": "2016-12-14T12:00:00-05:00", "title": "AGU Ionosphere Press Conference", "description": "The ionosphere is a layer of charged particles in Earth’s atmosphere that extends from about 50 to 360 miles above the surface of Earth. Processes in the ionosphere also create bright swaths of color in the sky, known as airglow. Credit: NASA GSFC || AGUIonosphereV4_1.jpg (1280x960) [109.7 KB] || ", "hits": 56 }, { "id": 12450, "url": "https://svs.gsfc.nasa.gov/12450/", "result_type": "Produced Video", "release_date": "2016-12-12T18:30:00-05:00", "title": "Ocean Tides and Magnetic Fields", "description": "Seawater is an electrical conductor, and therefore interacts with the magnetic field. As the tides cycle around the ocean basins, the ocean water essentially tries to pull the geomagnetic field lines along.Because the salty water is a good, but not great, conductor, the interaction is relatively weak. Scientists at NASA Goddard Space Flight Center are developing improved methods to isolate the signal from ocean tides and use that information to determine the heat content of the ocean.Music: \"Memory Of A Lifetime\" by J Ehrlich [SESAC], Jean-Christophe Beck [BMI]Complete transcript available.Watch this video on the NASA Goddard YouTube channel. || 12450-Tidal-Magnetic-Animation-APR_large.00545_print.jpg (1024x576) [189.1 KB] || 12450-Tidal-Magnetic-Animation-APR_large.00545_searchweb.png (320x180) [93.6 KB] || 12450-Tidal-Magnetic-Animation-APR_large.00545_thm.png (80x40) [5.8 KB] || 12450-Tidal-Magnetic-Animation-APR.webm (960x540) [26.5 MB] || 12450-Tidal-Magnetic-Animation-APR_prores.mov (1280x720) [989.0 MB] || 12450-Tidal-Magnetic-Animation-APR_large.mp4 (1920x1080) [66.1 MB] || 12450-Tidal-Magnetic-Animation-APR_youtube_hq.mov (1920x1080) [1.0 GB] || 12450-Tidal-Magnetic-Animation-APR_appletv.m4v (1280x720) [32.1 MB] || 12450-Tidal-Magnetic-Animation-APR_appletv_subtitles.m4v (1280x720) [32.2 MB] || 1920x1080_16x9_30p (1920x1080) [128.0 KB] || 12450-Tidal-Magnetic-Animation.en_US.srt [1.4 KB] || 12450-Tidal-Magnetic-Animation.en_US.vtt [1.4 KB] || 12450-Tidal-Magnetic-Animation-APR_ipod_sm.mp4 (320x240) [11.5 MB] || ", "hits": 318 }, { "id": 4498, "url": "https://svs.gsfc.nasa.gov/4498/", "result_type": "Visualization", "release_date": "2016-10-27T14:00:00-04:00", "title": "ICON and GOLD: Exploring the Interface to Space", "description": "A basic view of the orbits for ICON (Ionospheric Connections Explorer) and GOLD (Global-scale Observations of the Limb and Disk). These missions will conduct measurements of ionospheric composition, ionization, and winds to better understand the connection between space weather and its terrestrial impacts.In this visualization, we present GOLD (in geostationary orbit around Earth) and ICON (in low Earth orbit). The colors over Earth represent model data from the IRI (International Reference Ionosphere) model of the density of the singly-ionized oxygen atom at an altitude of 350 kilometers. Red represents high density. The ion density is enhanced above and below the geomagnetic equator (not perfectly aligned with the geographic equator) on the dayside due to the ionizing effects of solar ultraviolet radiation combined with the effects of high-altitude winds and the geomagnetic field. || ", "hits": 43 }, { "id": 4503, "url": "https://svs.gsfc.nasa.gov/4503/", "result_type": "Visualization", "release_date": "2016-10-27T14:00:00-04:00", "title": "Exploring the Ionosphere: The View from GOLD", "description": "Closeup view of Earth from the perspective of the GOLD instrument. This version interpolates the IRI model to a higher time cadence for a smoother animation. || IRIDaily.GOLDview_O+ion_O+ionSlice.clockSlate_CRTT.UHD3840.001002_print.jpg (1024x576) [50.7 KB] || IRIDaily.GOLDview_O+ion_O+ionSlice.IRIinterp.HD1080i_p30.mp4 (1920x1080) [56.7 MB] || IRI.interpolate (1920x1080) [0 Item(s)] || IRIDaily.GOLDview_O+ion_O+ionSlice.IRIinterp.HD1080i_p30.webm (1920x1080) [17.1 MB] || IRI.interpolate (3840x2160) [0 Item(s)] || IRIDaily.GOLDview_O+ion_O+ionSlice.IRIinterp_4503.key [57.9 MB] || IRIDaily.GOLDview_O+ion_O+ionSlice.IRIinterp_4503.pptx [57.6 MB] || IRIDaily.GOLDview_O+ion_O+ionSlice.IRIinterp_2160p30.mp4 (3840x2160) [200.2 MB] || ", "hits": 48 }, { "id": 4504, "url": "https://svs.gsfc.nasa.gov/4504/", "result_type": "Visualization", "release_date": "2016-10-27T14:00:00-04:00", "title": "Exploring the Ionosphere: The Dayside Ionosphere", "description": "A view of the singly-ionizing oxygen atom on the dayside of Earth. This represents the variation of the enhancments due to variation in the geomagnetic field. This version interpolates the IRI model to a higher time cadence for a smoother animation. || IRIDaily.sunward_O+ion.clockSlate_CRTT.UHD3840.001001_print.jpg (1024x576) [58.1 KB] || IRIDaily.sunward_O+ion.IRIinterp.HD1080i_p30.mp4 (1920x1080) [50.1 MB] || IRI.interpolated (1920x1080) [0 Item(s)] || IRIDaily.sunward_O+ion.IRIinterp.HD1080i_p30.webm (1920x1080) [17.1 MB] || IRIDaily.sunward_O+ion.IRIinterp.UHD3840_2160p30.mp4 (3840x2160) [72.7 MB] || IRI.interpolated (3840x2160) [0 Item(s)] || IRIDaily.sunward_O+ion.IRIinterp_4504.key [51.9 MB] || IRIDaily.sunward_O+ion.IRIinterp_4504.pptx [51.6 MB] || exploring-the-ionosphere-the-dayside-ionosphere.hwshow [308 bytes] || ", "hits": 56 }, { "id": 4480, "url": "https://svs.gsfc.nasa.gov/4480/", "result_type": "Visualization", "release_date": "2016-08-15T14:00:00-04:00", "title": "Prompt Electron Acceleration in the Radiation Belts", "description": "Electrons gyrating along the lines of Earth's magnetic field make another orbit around Earth and strike the Van Allen Probe A AGAIN! || PromptAccel_EventCloseup_SlowOblique.slate_RigRHS.HD1080i.0540_print.jpg (1024x576) [139.2 KB] || PromptAccel_EventCloseup_SlowOblique.slate_RigRHS.HD1080i.0540_searchweb.png (320x180) [90.9 KB] || PromptAccel_EventCloseup_SlowOblique.slate_RigRHS.HD1080i.0540_thm.png (80x40) [6.0 KB] || 1920x1080_16x9_30p (1920x1080) [0 Item(s)] || PromptAccel.HD1080i_p30.mp4 (1920x1080) [48.5 MB] || PromptAccel.HD1080i_p30.webm (1920x1080) [3.1 MB] || PromptAccel_EventCloseup_SlowOblique.HD1080i_720p30.mp4 (1280x720) [24.1 MB] || 3840x2160_16x9_30p (3840x2160) [0 Item(s)] || PromptAccel_EventCloseup_SlowOblique_2160p30.mp4 (3840x2160) [141.9 MB] || PromptAccel.HD1080i_p30.mp4.hwshow [189 bytes] || ", "hits": 150 }, { "id": 4453, "url": "https://svs.gsfc.nasa.gov/4453/", "result_type": "Visualization", "release_date": "2016-05-12T14:00:00-04:00", "title": "Zoom in to MMS and Magnetopause Reconnection", "description": "The visualization starts with an overview of the MMS orbit. || MMSpursuit_Fly2Pursuit2Stop_Oct16data_RE_MMS.slate_RigRHS.HD1080i.0200_print.jpg (1024x576) [91.6 KB] || MMSpursuit_Fly2Pursuit2Stop_Oct16data_RE_MMS.slate_RigRHS.HD1080i.0200_searchweb.png (320x180) [71.3 KB] || MMSpursuit_Fly2Pursuit2Stop_Oct16data_RE_MMS.slate_RigRHS.HD1080i.0200_thm.png (80x40) [4.9 KB] || 1920x1080_16x9_30p (1920x1080) [0 Item(s)] || MMSpursuit_Fly2Pursuit2Stop_Oct16data_HD1080i_p30.mp4 (1920x1080) [81.6 MB] || MMSpursuit_Fly2Pursuit2Stop_Oct16data_HD1080i_p30.webm (1920x1080) [9.3 MB] || 3840x2160_16x9_30p (3840x2160) [0 Item(s)] || MMSpursuit_Fly2Pursuit2Stop_Oct16data.UHD3840p30.mp4 (3840x2160) [238.2 MB] || MMSpursuit_Fly2Pursuit2Stop_Oct16data_HD1080i_p30.mp4.hwshow [270 bytes] || ", "hits": 81 }, { "id": 4460, "url": "https://svs.gsfc.nasa.gov/4460/", "result_type": "Visualization", "release_date": "2016-05-12T14:00:00-04:00", "title": "Data Tour of MMS and Magnetopause Reconnection", "description": "A slow fly-around of the MMS tetrahedral formation to better view the 3-dimensional structure of the data. || MMSpursuit_DataTour_Oct16slow_RE_MMS.slate_RigRHS.HD1080i.1300_print.jpg (1024x576) [144.5 KB] || MMSpursuit_DataTour_Oct16slow_RE_MMS.slate_RigRHS.HD1080i.1300_searchweb.png (320x180) [84.0 KB] || MMSpursuit_DataTour_Oct16slow_RE_MMS.slate_RigRHS.HD1080i.1300_thm.png (80x40) [5.1 KB] || 1920x1080_16x9_30p (1920x1080) [0 Item(s)] || MMSpursuit_DataTour_Oct16slow_HD1080i_p30.mp4 (1920x1080) [94.0 MB] || MMSpursuit_DataTour_Oct16slow_HD1080i_p30.webm (1920x1080) [9.2 MB] || 3840x2160_16x9_30p (3840x2160) [0 Item(s)] || MMSpursuit_DataTour_Oct16slow.UHD3840p30.mp4 (3840x2160) [282.4 MB] || MMSpursuit_DataTour_Oct16slow_HD1080i_p30.mp4.hwshow [207 bytes] || ", "hits": 53 }, { "id": 20237, "url": "https://svs.gsfc.nasa.gov/20237/", "result_type": "Animation", "release_date": "2016-05-12T14:00:00-04:00", "title": "Beyond Earth - Earth's Geomagnetic Activity", "description": "Space is a better vacuum than any we can create on Earth, but it's nonetheless bustling with activity. It overflows with energy, particles and a complex system of magnetic field lines. This animation shows the busy-ness of near-Earth space, where the magnetic environment around Earth can trap electrons and charged particles. || beyondearth.jpg (1280x720) [261.9 KB] || beyondearth_searchweb.png (320x180) [136.2 KB] || beyondearth_thm.png (80x40) [22.8 KB] || BeyondEarthAnimatedGIFFinal30fpsv02.webm (1920x1080) [4.4 MB] || BeyondEarthAnimatedGIFFinal30fpsv02.mov (1920x1080) [429.8 MB] || BeyondEarthAnimatedGIFFinal60fpsv02.mov (1920x1080) [429.8 MB] || beyond-earth-earths-geomagnetic-activity.hwshow || ", "hits": 153 }, { "id": 12239, "url": "https://svs.gsfc.nasa.gov/12239/", "result_type": "Produced Video", "release_date": "2016-05-12T13:00:00-04:00", "title": "MMS First Results", "description": "This short video outlines the MMS mission and its first results. Since it launched, MMS has made more than 4,000 trips through the magnetic boundaries around Earth, each time gathering information about the way the magnetic fields and particles move. A surprising result was that at the moment of interconnection between the sun’s magnetic field lines and those of Earth the crescents turned abruptly so that the electrons flowed along the field lines. By watching these electron tracers, MMS made the first observation of the predicted breaking and interconnection of magnetic fields in space. Credit: NASA/GSFCWatch this video on the NASA Goddard YouTube channel. || mmsthumb.jpg (1280x720) [139.4 KB] || mmsthumb_print.jpg (1024x576) [161.8 KB] || mmsthumb_searchweb.png (320x180) [104.3 KB] || mmsthumb_web.png (320x180) [104.3 KB] || mmsthumb_thm.png (80x40) [6.8 KB] || 12239_MMS_First_ResultsV2_appletv.m4v (1280x720) [76.9 MB] || 12239_MMS_First_ResultsV2.webm (1920x1080) [18.1 MB] || 12239_MMS_First_ResultsV2_appletv_subtitles.m4v (1280x720) [77.0 MB] || 12239_MMS_First_ResultsV2.en_US.srt [3.0 KB] || 12239_MMS_First_ResultsV2.en_US.vtt [3.0 KB] || YOUTUBE_HQ_12239_MMS_First_ResultsV2_youtube_hq.mov (1920x1080) [1.1 GB] || 12239_MMS_First_ResultsV2_lowres.mp4 (480x272) [21.6 MB] || 12239_MMS_First_ResultsV2_ipod_sm.mp4 (320x240) [26.3 MB] || PRORES_B-ROLL_12239_MMS_First_ResultsV2_prores.mov (1280x720) [2.2 GB] || 12239_MMS_First_ResultsV2.mov (1920x1080) [4.2 GB] || YOUTUBE_HQ_12239_MMS_First_ResultsV2_youtube_hq.mov.hwshow [100 bytes] || ", "hits": 146 }, { "id": 12040, "url": "https://svs.gsfc.nasa.gov/12040/", "result_type": "Produced Video", "release_date": "2015-11-04T16:00:00-05:00", "title": "NASA Observes Auroras Across Canada", "description": "These aurora images were taken from the ground looking up with a network of all-sky cameras spread across Canada, studying auroras in collaboration with NASA’s Time History of Events and Macroscale Interactions during Substorms, or THEMIS, mission. Taking images of aurora from the ground in conjunction with satellite data taken from above the atmosphere gives scientists a more comprehensive picture of how and why the aurora form. The ground-based camera network is also observing this week’s auroras. The aurora data is provided courtesy of S. Mende at University California Berkeley and E. Donovan at the University of Calgary, logistical support in fielding and data retrieval from the ground-based stations is provided by the Canadian Space Agency. The array of aurora images is funded by NSF in support of GIMNAST through grant AGS-1004736.Credit: NASA/CSA/University of California, Berkeley/University of Calgary/NSF || Storm_0386.jpg (1944x1080) [1.4 MB] || Storm_0386_print.jpg (1024x568) [476.9 KB] || Storm_0386_searchweb.png (180x320) [150.3 KB] || Storm_0386_thm.png (80x40) [33.8 KB] || 1944x1080_16x9_20p (1944x1080) [128.0 KB] || Auroras_Across_Canada-MPEG4_1944x1080_24.mp4 (1944x1080) [54.0 MB] || Auroras_Across_Canada_ProRes_1944x1080_24.webm (1944x1080) [10.3 MB] || Auroras_Across_Canada_ProRes_1944x1080_24.mov (1944x1080) [1.4 GB] || Auroras_Across_Canada-H264_Best_1944x1080_24.mov (1944x1080) [658.5 MB] || Auroras_Across_Canada-H264_Good_1944x1080_24.mov (1944x1080) [130.4 MB] || Auroras_Across_Canada.hwshow [223 bytes] || ", "hits": 30 }, { "id": 40223, "url": "https://svs.gsfc.nasa.gov/gallery/heliophysics-education-resources/", "result_type": "Gallery", "release_date": "2015-01-16T00:00:00-05:00", "title": "Heliophysics Education Resources", "description": "Visualizations useful for illustrating key concepts.", "hits": 143 }, { "id": 4241, "url": "https://svs.gsfc.nasa.gov/4241/", "result_type": "Visualization", "release_date": "2014-11-26T13:00:00-05:00", "title": "Radiation Belts & Plasmapause", "description": "Visualization of the radiation belts with confined charged particles (blue & yellow) and plasmapause boundary (blue-green surface) || Earth_BeltsPlasmapauseParticles_Oblique.noslate_GSEmove.HD1080i.0400_print.jpg (1024x576) [136.6 KB] || Earth_BeltsPlasmapauseParticles_Oblique.noslate_GSEmove.HD1080i.0400_web.png (320x180) [96.2 KB] || Earth_BeltsPlasmapauseParticles_Oblique.noslate_GSEmove.HD1080i.0400_searchweb.png (320x180) [96.2 KB] || Earth_BeltsPlasmapauseParticles_Oblique.noslate_GSEmove.HD1080i.0400_thm.png (80x40) [6.9 KB] || BeltsPlasmapauseParticles_HD1080.mov (1920x1080) [28.3 MB] || Earth_BeltsPlasmapauseParticles_Oblique_HD1080.mp4 (1920x1080) [16.6 MB] || BeltsPlasmapauseParticles_HD720.mov (1280x720) [10.6 MB] || 1920x1080_16x9_30p (1920x1080) [0 Item(s)] || Earth_BeltsPlasmapauseParticles_Oblique_HD1080.webm (960x540) [2.3 MB] || BeltsPlasmapauseParticles_iPod.m4v (640x360) [3.7 MB] || radiation-belts--plasmapause.hwshow [342 bytes] || ", "hits": 139 }, { "id": 4217, "url": "https://svs.gsfc.nasa.gov/4217/", "result_type": "Visualization", "release_date": "2014-10-08T00:00:00-04:00", "title": "Coordinated Earth: Measuring Space in the Near-Earth Environment", "description": "When we operate satellites in space, they are often taking measurements along the locations of their travel. As with many measurements, they are only useful if they can be placed in the proper context - their relationship to other measurements at the same, and different, locations. To assemble these measurements within context, we also need to know where and when the measurements were taken, and to do that, we need to define a coordinate system.In three-dimensional space, we define a position with three numbers, relative to a point we define as the Origin of the coordinate system, defined as (0,0,0). Each number represents a distance from the origin along one of three directions. We usually defined these directions by axes, labelled X, Y, and Z, which are defined to be mutually perpendicular, each one is at right angles to the others.While all coordinate systems are equal, all coordinate systems are not equally convenient for a given problem of interest. Sometimes the data and mathematics we use for exploring different problems can be more complex in one coordinate system or another. To simplify this, we often define a number of different coordinate systems and ways to do transformations between them.In studying the space environment around Earth, we find five different coordinate systems of use. Geocentric (GEO): This is the coordinate system useful for measuring things close to Earth’s surface. The origin is chosen at the center of Earth. The x-axis points from the center of Earth through the Prime Meridian (by convention chosen as the meridian in Greenwich, London, UK (longitude = 0). The z-axis points towards the north geographic pole. Geocentric Earth Inertial (GEI): This coordinate system is fixed relative to the distant stars, so Earth rotates about the z-axis relative to it. The origin of this coordinate system is at the center of the Earth. The x-axis points to the first point in Aries (Wikipedia: Vernal Equinox) and the z-axis points to the north geographic & celestial pole. The direction of the celestial pole changes due to Earth’s rotational precession (Wikipedia). Geocentric Solar Ecliptic (GSE): The origin is at the center of the Earth. The x-axis is along the line between Earth and the Sun. The z-axis is the north ecliptic pole and is fixed in direction (but for slow changes due to Earth orbital changes). Solar Magnetic (SM): the origin is at the center of the Earth. The z-axis is chosen parallel to the Earth magnetic dipole axis. The y-axis is chosen to be perpendicular to the z-axis and the Earth-Sun line (pointing towards dusk). Geocentric Solar Magnetospheric (GSM): The origin is at the center of the Earth. The x-axis is defined as the Earth-Sun line (same as in GSE). The y-axis is defined to be perpendicular to the plane containing the x-axis and the magnetic dipole axis so the magnetic axis always lies in this plane.Similar coordinate systems are defined for the Sun and other planets of the Solar System.Development Note: This visualization was originally developed to test coordinate system transformations in the visualization framework.References:C. T. Russell. \"Geophysical coordinate transformations\". Cosmical Electrodynamics 2, 184-196 (1971). URL.M.A. Hapgood. \"Space Physics Coordinate Transformations: A User Guide\". Planetary & Space Science, 40, 711-717.(1992). URLSPENVIS Help Pages: Coordinate Systems and transformations || ", "hits": 178 }, { "id": 4188, "url": "https://svs.gsfc.nasa.gov/4188/", "result_type": "Visualization", "release_date": "2014-09-25T10:00:00-04:00", "title": "Comparative Magnetospheres: A Noteworthy Coronal Mass Ejection", "description": "In an effort to understand and predict the impact of space weather events on Earth, the Community-Coordinated Modeling Center (CCMC) at NASA Goddard Space Flight Center, routinely runs computer models of the many historical events. These model runs are then compared to actual data to determine ways to improve the model, and therefore forecasts of the impacts of future space weather events.In mid-December of 2006, the Sun erupted with a bright flare and coronal mass ejection (CME) that launched particles Earthward. While not the brightest or largest event observed, its impact on Earth was substantial, requiring some effort to protect satellites (ESA: Reacting to a solar flare).The visualization presented here is a CCMC run of a BATS-R-US model simulating the impact of this event on Earth. Here, lines are used to represent the 'flow direction' of magnetic field of the solar wind impacting Earth, as well as the effects on Earth's geomagnetic field. A 'cut-plane' through the data illustrates the changes in the particle density in the solar wind and magnetosphere. The color of the data represents a logarithmic scaling of density, with red as the highest (1000 particles per cubic centimeter) down to blue (0.01 particles per cubic centimeter). In this simulation, each frame of the movie corresponds to two minutes of real time.In the movie, we see vertical field lines of magnetic field carried by the solar wind, coming in from the left. As this field, and the plasma carrying it, strike Earth's magnetic field, they bend and reconnect, around the Earth. Some field lines actually reconnect to the polar regions of the Earth, providing a ready flow-path for particles to reach the ionosphere and generate aurora. This interaction between the solar wind and the plasma trapped in Earth's magnetosphere also creates a density enhancement between Earth and the solar wind helping to shield Earth from some of the effects. A lower density wake forms behind Earth (the blue region). There is a circular 'hole' around the Earth which is a gap in the model. || ", "hits": 164 }, { "id": 30481, "url": "https://svs.gsfc.nasa.gov/30481/", "result_type": "Infographic", "release_date": "2013-12-02T10:00:00-05:00", "title": "Heliophysics and Space Weather", "description": "The sun and its atmosphere consist of several zones, or layers, from the inner core to the outer corona. Beyond the corona is the solar wind, which is an outward expansion of coronal plasma that extends well beyond the orbit of Pluto. This entire region of space influenced by the sun is called the heliosphere. Controlled by the Earth’s magnetic field, the magnetosphere acts as a shield protecting the planet from solar wind. The shape of the Earth's magnetosphere is the direct result of being impacted by solar wind, compressed on its sunward side and elongated on the night-side, the magnetotail. The shock wave where the solar wind encounters Earth's magnetosphere is called the bow shock, which slows and diverts the solar wind. Solar activity lead to solar eruptions, which includes such phenomena as sunspots, flares, prominences, and coronal mass ejections that influence space weather, or near-Earth environmental conditions. Modern society depends heavily on a variety of technologies that are susceptible to space weather. CMEs for example can cause geomagnetic storms that can disrupt satellite communications and navigational equipment, and even cause blackouts. || ", "hits": 284 }, { "id": 4080, "url": "https://svs.gsfc.nasa.gov/4080/", "result_type": "Visualization", "release_date": "2013-09-26T14:00:00-04:00", "title": "Reconnection Fronts - When Satellites Align...", "description": "In July of 2012, a fleet of spacecraft studying Earth's magnetosphere were in an ideal alignment to detect a particle flow predicted in magnetospheric models. The grey mesh shell structure represents the approximate location of the magnetopause.In this visualization, THEMIS, ARTEMIS (in orbit around the Moon), and Geotail, as well as the particle detectors on the GOES-13 and GOES-15 satellites achieved a good alignment around 09:45 on July 3, 2012 to detect one of the particle flows predicted by magnetospheric models. || ", "hits": 65 }, { "id": 4006, "url": "https://svs.gsfc.nasa.gov/4006/", "result_type": "Visualization", "release_date": "2012-10-31T00:00:00-04:00", "title": "The Radiation Belts as seen by SAMPEX", "description": "This is a simulation of the Earth's radiation belts constructed from SAMPEX data around the time of the 2003 Halloween solar storms. In this visualization, we present the belts in cross-section to provide a better view of their interior structure.The Earth's magnetosphere is a very large magnetic structure around the Earth, and gets stretched into a large, teardrop-shaped configuration through its interaction with the solar wind. A number of the magnetic field lines, while they may originate on the Earth, do not connect back to the Earth, but connect into the magnetic field carried by the solar wind. However, near the Earth, the magnetic dipole component of the field is stronger than the solar wind field, and this allows all the magnetic field lines to connect back to the Earth, forming (approximately) the classic magnetic dipole configuration (Wikipedia). In this region, lower energy electrons and ions, many from the Earth's ionosphere, can become trapped by the magnetic field to form the radiation belts.The radiation belt model is constructed from particle flux information from the SAMPEX mission, with the flux mapped to constant L-shells of the Earth's dipole magnetic field (Wikipedia). The model is anchored to the Earth's geomagnetic field axis, which is not perfectly aligned with the Earth's rotation axis. This creates a small wobble of the radiation belts with time, which can be seen in this visualization.The data driving the radiation belt structure is from the 2003 Halloween solar storms, a series of strong solar eruptions that began in late October 2003 and continued into the first week of November. During this time, the particle content of the belts change rapidly due to the variation in the energetic particle flux from the Sun buffeting the Earth's magnetosphere.This dataset was also used to generate radiation belts for the RBSP prelaunch visualizations. || ", "hits": 102 }, { "id": 3551, "url": "https://svs.gsfc.nasa.gov/3551/", "result_type": "Visualization", "release_date": "2012-09-01T00:00:00-04:00", "title": "The Coronal Mass Ejection strikes the Earth!", "description": "This visualization is the sequel to animation ID 3867.The CME we saw before continues to expand from the Sun, and its outer boundary is approaching the Earth. Will the Earth be pummeled like its sister planet, Venus?Not this time, for the Earth has a fairly strong geomagnetic field.The geomagnetic field helps deflect the incoming blast of solar particles around the Earth, dramatically reducing the impact of the event.It is important to note that the flowing material of the CME are actually ions and electrons far too small to see. This visualization tries to represent the motions of these tiny particle in a form large enough for us to see.Technical DetailsThis is the dome show component where the CME strikes the Earth.The domemaster format was created by rendering 7 separate camera tiles. The tiles were then stitched together to form final domemaster layers at 4096x4096 resolution and 16 bits per channel with premultiplied alpha and no gamma correction. There are 2 domemaster layers that should be composited as follows:- Earth, Sun and particles- star field (no alpha channel)In addition to the final domemaster frames and movies, the individual camera tiles are included as well. Each domemaster layer has a set of camera tiles. There are 7 cameras numbered 00 through 06 that represent the itiles. Camera 00 is in the center of the domemaster, camera 01 is looking below camera 00, cameras 01 through 06 look around the outside of the dome master in counter-clockwise order. These frames are probably only useful if a better re-stitching algorithm is ever required to be run on the tiles. || ", "hits": 186 }, { "id": 3949, "url": "https://svs.gsfc.nasa.gov/3949/", "result_type": "Visualization", "release_date": "2012-05-08T00:00:00-04:00", "title": "Earth's Radiation Belts (side view)", "description": "This is a simulation of the Earth's radiation belts. In this version, we've kept the belts full structure. There is also a cross-section view of the belts in Earth's Radiation Belts (cross-section).The Earth's magnetosphere is a very large magnetic structure around the Earth, which gets stretched into a large, teardrop-shaped configuration through its interaction with the solar wind. A number of the magnetic field lines, which they may originate on the Earth, do not connect back to the Earth, but connect into the magnetic field carried by the solar wind. However, near the Earth, the dipole component of the field is stronger than the solar wind field, and this allows all the magnetic field lines to connect back to the Earth, forming (approximately) the classic magnetic dipole configuration. In this region, lower energy electrons and ions, many from the Earth's ionosphere, can become trapped by the magnetic field to form the radiation belts.The radiation belt model is constructed from particle flux information from the SAMPEX mission, with the flux mapped to constant L-shells of the Earth's dipole magnetic field. The model is anchored to the Earth's geomagnetic field axis, which is not perfectly aligned with the Earth's rotation axis. This creates a small wobble of the radiation belts with time, which can be seen in this visualization.The data driving the radiation belt structure is time-shifted from the 2003 Halloween solar storms, a series of strong solar eruptions that began in late October 2003 and continued into the first week of November. During this time, the particle content of the belts change rapidly due to the variation in the energetic particle flux from the Sun buffeting the Earth's magnetosphere. || ", "hits": 57 }, { "id": 3951, "url": "https://svs.gsfc.nasa.gov/3951/", "result_type": "Visualization", "release_date": "2012-05-08T00:00:00-04:00", "title": "The Van Allen Probes (formerly Radiation Belt Storm Probes - RBSP) Explore the Earth's Radiation Belts", "description": "The Radiation Belt Storm Probe (RBSP) is actually two satellites that will travel on a elliptical orbit around the Earth, ranging between 1.5 and 6 Earth radii. This range covers the inner region of the Earth's geomagnetic field. In this region, many of the magnetic field lines intersect the surface of the Earth in the north and south. This means that lower energy ions and electrons, some 'boiled off' the Earth's ionosphere by solar ultraviolet radiation, can be trapped along these field lines. The charged particles spend their time bouncing between the 'mirror points' in the Earth's magnetic field. This trapped population forms the radiation belts around the Earth. The radiation created by this charged particle population can be hazardous to satellites and astronauts so it is important to understand their characteristics. || ", "hits": 185 }, { "id": 3950, "url": "https://svs.gsfc.nasa.gov/3950/", "result_type": "Visualization", "release_date": "2012-05-01T00:00:00-04:00", "title": "Earth's Radiation Belts (cross-section)", "description": "This is a simulation of the Earth's radiation belts. In this version, we've 'sliced' the belts open to provide a better view of their structure in cross-section. The non-cross-section view of the belts is Earth's Radiation Belts (side view)The Earth's magnetosphere is a very large magnetic structure around the Earth, and gets stretched into a large, teardrop-shaped configuration through its interaction with the solar wind. A number of the magnetic field lines, while they may originate on the Earth, do not connect back to the Earth, but connect into the magnetic field carried by the solar wind. However, near the Earth, the dipole component of the field is stronger than the solar wind field, and this allows all the magnetic field lines to connect back to the Earth, forming (approximately) the classic magnetic dipole configuration. In this region, lower energy electrons and ions, many from the Earth's ionosphere, can become trapped by the magnetic field to form the radiation belts.The radiation belt model is constructed from particle flux information from the SAMPEX mission, with the flux mapped to constant L-shells of the Earth's dipole magnetic field. The model is anchored to the Earth's geomagnetic field axis, which is not perfectly aligned with the Earth's rotation axis. This creates a small wobble of the radiation belts with time, which can be seen in this visualization.The data driving the radiation belt structure is time-shifted from the 2003 Halloween solar storms, a series of strong solar eruptions that began in late October 2003 and continued into the first week of November. During this time, the particle content of the belts change rapidly due to the variation in the energetic particle flux from the Sun buffeting the Earth's magnetosphere. || ", "hits": 189 }, { "id": 10941, "url": "https://svs.gsfc.nasa.gov/10941/", "result_type": "Produced Video", "release_date": "2012-04-24T10:00:00-04:00", "title": "Space Weather FAQ Interviews", "description": "NASA scientists answer some frequently asked questions about the sun, space weather, and the effects on Earth. Each video is one or more scientists responding to the question above it. The videos are available as ProRes files for broadcast use and have had minor audio equalizing and color correction applied.The scientists interviewed are:Dr. Holly Gilbert, NASA HeliophysicistDr. Alex Young, NASA HeliophysicistDr. Phil Chamberlin, NASA Research Heliophysicist and SDO Deputy Project ScientistThere are also two short videos created with this interview content. They are available here.Additional responses to these questions are available upon specific request.For space weather-related footage, animations, and features, visit the Space Weather gallery. || ", "hits": 61 }, { "id": 10954, "url": "https://svs.gsfc.nasa.gov/10954/", "result_type": "Produced Video", "release_date": "2012-04-24T00:00:00-04:00", "title": "Rattling Earth's Force Field", "description": "A giant magnetic bubble surrounds Earth, shielding our planet from the sheer power of the sun. Invisible to the human eye, the bubble—called the magnetosphere—is fairly round on the side that faces the sun, and then forms long, spaghetti-like strands that trail behind Earth and move in concert with the constant stream of magnetized particles known as the solar wind. The magnetosphere protects Earth from the brunt of the sun's energetic outbursts. But some gigantic eruptions of solar material, called coronal mass ejections, can nonetheless compress the shape of the magnetosphere, creating a geomagnetic storm. During strong geomagnetic storms, the fluctuation of magnetism and electricity near Earth can interfere with communication and GPS satellites, induce electrical surges in power grids on the ground and light up the skies with auroras. Watch the visualization below to see the shape of the magnetosphere that surrounds and cradles Earth, protecting it from the sun's explosions. || ", "hits": 113 }, { "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": 145 }, { "id": 3822, "url": "https://svs.gsfc.nasa.gov/3822/", "result_type": "Visualization", "release_date": "2011-02-14T00:00:00-05:00", "title": "Stereoscopic Magnetic Field Lines", "description": "This stereoscopic visualization shows a simple model of the Earth's magnetic field. The magnetic field partially shields the Earth from harmful charged particles emanating from the sun. The field is stretched back away from Sun by solar particle and radiation pressures.The geomagnetic field is generated (and regenerated) as the conducting fluid of the Earth's mantle and core, driven by convection of heat from deeper in the interior, induces an electromotive force (EMF) with the existing magnetic field. This process is very similar to the way an electric generator generates a voltage. That voltage then drives an induced current in the conducting fluid, which also produces a magnetic field. This feedback mechanism helps maintain the field, continuously converting the thermal energy in the Earth into magnetic field energy.The magnetic field line data used in this visualization is from a simplified static model. More complex models deform the magnetic field over time as the Earth rotates and experiences solar pressures. Many of the field lines (particulary near the back, away from the Sun) should eventually connect (north and south poles), but the 3d model used in this visualization does not extend far enough to see this.The day/night terminator is aligned with the Sun and is therefore aligned with the magnetic field too. This visualization is based on a previous monoscopic visualizaton that included magnetic field line data. || ", "hits": 291 }, { "id": 10636, "url": "https://svs.gsfc.nasa.gov/10636/", "result_type": "Produced Video", "release_date": "2010-10-27T12:00:00-04:00", "title": "ARTEMIS Orbits Magnetic Moon", "description": "Launched in 2007, NASA's five THEMIS spacecraft have now successfully completed their 2 year mission to determine the cause of geomagnetic substorms. Because they are continuing to work perfectly, NASA is re-directing the outermost two spacecraft to special orbits at and around the Moon. This new mission, which is called ARTEMIS, uses some very complex maneuvers over two years (2009-2010) to get both spacecraft into position. As the Moon orbits the Earth, it passes in and out of the Earth's magnetic field and the million-mile per hour stream of particles emitted by the Sun known as the solar wind. While in these regions, the two ARTEMIS spacecraft will seek evidence for turbulence, particle acceleration, and magnetic reconnection, three fundamental phenomena that control the nature of the solar wind's interaction with the Earth's magnetosphere. Employing their full complement of instruments and unique two-point vantage points, the spacecraft will study the vacuum the Moon carves out in the solar wind, and the processes that eventually fill this lunar wake. Nearer the Moon, they will observe the effects of surface electric fields, ions sputtered off the lunar surface, and determine the internal structure of the Moon from transient variations in its magnetic field induced by external changes.Also available are the complete, unedited visualization and frames. || ", "hits": 644 }, { "id": 3740, "url": "https://svs.gsfc.nasa.gov/3740/", "result_type": "Visualization", "release_date": "2010-07-08T00:00:00-04:00", "title": "Space Weather Event: The View from L1", "description": "We start from a position 'behind' the Earth, looking towards the Sun. From this position we see the orbit of the Moon as well as three of the heliospheric 'sentinels' (see \"Sentinels of the Heliosphere\"), ACE, SOHO, and Wind patrolling along 'halo orbits' (Wikipedia) around the Sun-Earth Lagrange Point, L1.The CME (orange isosurface) erupts, heading towards the Earth. The density enhancement of the CME is visible in slice of data in the Earth's orbit plane which provides a better sense of when the CME actually reaches the Earth.As the particle density enhancement from the CME strikes the Earth, we see the Earth's magnetosphere respond, with the outer, high density surface (red), 'blown away'. This surface location corresponds roughly to the location of the bow shock. The bow shock has not been eliminated, only some of its particles have been depleted, to be carried off in the CME and solar wind. As the densest material of the CME passes (orange surface), plasma from the CME continues to flow by the Earth, stretching the magnetosphere into a long, thin structure behind the Earth.The magnetosphere slowly recovers from the 'impact', and regions that can confine higher particle densities reform - the red surfaces return. But not for long as the rarefaction behind the CME reaches the Earth. This lower density region provides fewer particles to repopulate the magnetosphere and make it easier for particles confined in the magnetosphere to 'leak' out into the solar wind.For the BATS-R-US model, the isosurface colors are: red=20 AMUs per cubic centimeter, yellow=10.0 AMUs per cubic centimeter, light blue=1.0 AMUs per cubic centimeter, and blue=0.1 AMUs per cubic centimeter. An AMU corresponds to about the mass of a hydrogen atom, the dominant component of the solar wind.This visualization is part of a series of visualizations on space weather modeling. || ", "hits": 40 }, { "id": 3743, "url": "https://svs.gsfc.nasa.gov/3743/", "result_type": "Visualization", "release_date": "2010-07-08T00:00:00-04:00", "title": "Space Weather Event: Close-up on the Earth Environment", "description": "We open with a view from high above the ecliptic plane, at the space between the Sun (left) and the Earth (within the small rectangular box on the right). In the plane of the Earth's orbit, we show a 'slice' of the Enlil model showing the particle density profile of the solar wind (white to yellow for decreasing particle density). The spiral 'rotating water sprinkler' pattern in the density is the Parker spiral (Wikipedia). We zoom down to the Earth as the CME (orange surface) erupts in the direction of the Earth and move into a position above the Earth's orbital plane with the Earth (geospace) environment in view.As the particle density enhancement from the CME strikes the Earth, we see the Earth's magnetosphere respond, with the outer, high density surface (red) 'blown away'. This surface location corresponds roughly to the location of the bow shock. The bow shock has not been eliminated, only some of its particles have been depleted, to be carried off in the CME and solar wind. As the densest material of the CME passes (orange surface), plasma from the CME continues to flow by the Earth, stretching the magnetosphere into a long, thin structure behind the Earth.The magnetosphere slowly recovers from the 'impact', and regions that can confine higher particle densities reform - the red surfaces return. But not for long as the rarefaction (Wikipedia) behind the CME reaches the Earth. This lower density region provides fewer particles to repopulate the magnetosphere and makes it easier for particles confined in the magnetosphere to 'leak' out into the solar wind.For the BATS-R-US model, the isosurface colors are: red=20 AMUs per cubic centimeter, yellow=10.0 AMUs per cubic centimeter, light blue=1.0 AMUs per cubic centimeter, and blue=0.1 AMUs per cubic centimeter. An AMU corresponds to about the mass of a hydrogen atom, the dominant component of the solar wind.This visualization is part of a series of visualizations on space weather modeling. || ", "hits": 58 }, { "id": 3739, "url": "https://svs.gsfc.nasa.gov/3739/", "result_type": "Visualization", "release_date": "2010-07-06T00:00:00-04:00", "title": "Space Weather Event: Incoming View", "description": "We open with a view from high above the ecliptic plane, at the space between the Sun (left) and the Earth (within the small rectangular box on the right). In the plane of the Earth's orbit, we show a 'slice' of the Enlil model showing the particle density profile of the solar wind (white to yellow for decreasing particle density). The spiral 'rotating water sprinkler' pattern in the density is the Parker spiral (Wikipedia). The nested grid pattern centered on the Earth, provides a sense of scale to the scene. The smallest grid square in the opening view is 1,000 Earth radii on each side. The scale changes by a factor of ten for each step larger or smaller in size.We zoom down to the Earth as the CME (orange surface) erupts in the direction of the Earth, then move into a position behind the Earth with the Sun visible in the distance.As the particle density enhancement from the CME strikes the Earth, we see the Earth's magnetosphere respond, with the outer, high density surface (red) 'blown away'. This surface location corresponds roughly to the location of the bow shock. The bow shock has not been eliminated, only some of its particles have been depleted, to be carried off in the CME and solar wind. As the densest material of the CME passes (orange surface), plasma from the CME continues to flow by the Earth, stretching the magnetosphere into a long, thin structure behind the Earth.The magnetosphere slowly recovers from the 'impact', and regions that can confine higher particle densities reform - the red surfaces return. But not for long as the rarefaction (Wikipedia) behind the CME reaches the Earth. This lower density region provides fewer particles to repopulate the magnetosphere and makes it easier for particles confined in the magnetosphere to 'leak' out into the solar wind.For the BATS-R-US model, the isosurface colors correpond to densities of: red=20 AMUs per cubic centimeter, yellow=10.0 AMUs per cubic centimeter, light blue=1.0 AMUs per cubic centimeter, and blue=0.1 AMUs per cubic centimeter. An AMU corresponds to about the mass of a hydrogen atom, so the value roughly corresponds to the number of atoms per cubic centimeter.This visualization is part of a series of visualizations on space weather modeling. || ", "hits": 39 }, { "id": 3595, "url": "https://svs.gsfc.nasa.gov/3595/", "result_type": "Visualization", "release_date": "2009-07-27T00:00:00-04:00", "title": "Sentinels of the Heliosphere", "description": "Heliophysics is a term to describe the study of the Sun, its atmosphere or the heliosphere, and the planets within it as a system. As a result, it encompasses the study of planetary atmospheres and their magnetic environment, or magnetospheres. These environments are important in the study of space weather.As a society dependent on technology, both in everyday life, and as part of our economic growth, space weather becomes increasingly important. Changes in space weather, either by solar events or geomagnetic events, can disrupt and even damage power grids and satellite communications. Space weather events can also generate x-rays and gamma-rays, as well as particle radiations, that can jeopardize the lives of astronauts living and working in space.This visualization tours the regions of near-Earth orbit; the Earth's magnetosphere, sometimes called geospace; the region between the Earth and the Sun; and finally out beyond Pluto, where Voyager 1 and 2 are exploring the boundary between the Sun and the rest of our Milky Way galaxy. Along the way, we see these regions patrolled by a fleet of satellites that make up NASA's Heliophysics Observatory Telescopes. Many of these spacecraft do not take images in the conventional sense but record fields, particle energies and fluxes in situ. Many of these missions are operated in conjunction with international partners, such as the European Space Agency (ESA) and the Japanese Space Agency (JAXA).The Earth and distances are to scale. Larger objects are used to represent the satellites and other planets for clarity.Here are the spacecraft featured in this movie:Near-Earth Fleet:Hinode: Observes the Sun in multiple wavelengths up to x-rays. SVS pageRHESSI : Observes the Sun in x-rays and gamma-rays. SVS pageTRACE: Observes the Sun in visible and ultraviolet wavelengths. SVS pageTIMED: Studies the upper layers (40-110 miles up) of the Earth's atmosphere.FAST: Measures particles and fields in regions where aurora form.CINDI: Measures interactions of neutral and charged particles in the ionosphere. AIM: Images and measures noctilucent clouds. SVS pageGeospace Fleet:Geotail: Conducts measurements of electrons and ions in the Earth's magnetotail. Cluster: This is a group of four satellites which fly in formation to measure how particles and fields in the magnetosphere vary in space and time. SVS pageTHEMIS: This is a fleet of five satellites to study how magnetospheric instabilities produce substorms. SVS pageL1 Fleet: The L1 point is a Lagrange Point, a point between the Earth and the Sun where the gravitational pull is approximately equal. Spacecraft can orbit this location for continuous coverage of the Sun.SOHO: Studies the Sun with cameras and a multitude of other instruments. SVS pageACE: Measures the composition and characteristics of the solar wind. Wind: Measures particle flows and fields in the solar wind. Heliospheric FleetSTEREO-A and B: These two satellites observe the Sun, with imagers and particle detectors, off the Earth-Sun line, providing a 3-D view of solar activity. SVS pageHeliopause FleetVoyager 1 and 2: These spacecraft conducted the original 'Planetary Grand Tour' of the solar system in the 1970s and 1980s. They have now travelled further than any human-built spacecraft and are still returning measurements of the interplanetary medium. SVS pageThis enhanced, narrated visualization was shown at the SIGGRAPH 2009 Computer Animation Festival in New Orleans, LA in August 2009; an eariler version created for AGU was called NASA's Heliophysics Observatories Study the Sun and Geospace. || ", "hits": 93 }, { "id": 3569, "url": "https://svs.gsfc.nasa.gov/3569/", "result_type": "Visualization", "release_date": "2008-12-16T00:00:00-05:00", "title": "THEMIS Dayside Science - Sampling the Bow Shock", "description": "In the early part of the mission, the five THEMIS satellites follow the same orbit single-file. The apogee of the orbit takes the spacecraft just beyond the bow shock of Earth's magnetosphere. This enables the closely spaced satellites to measure the thickness of the different regions that they encounter. || ", "hits": 29 }, { "id": 3570, "url": "https://svs.gsfc.nasa.gov/3570/", "result_type": "Visualization", "release_date": "2008-12-15T00:00:00-05:00", "title": "NASA's Heliophysics Observatories Study the Sun and Geospace", "description": "Heliophysics is a term to describe the study of the Sun, its atmosphere or the heliosphere, and the planets within it as a system. As a result, it encompasses the study of planetary atmospheres and their magnetic environment, or magnetospheres. These environments are important in the study of space weather.As a society dependent on technology, both in everyday life, and as part of our economic growth, space weather becomes increasingly important. Changes in space weather, either by solar events or geomagnetic events, can disrupt and even damage power grids and satellite communications. Space weather events can also generate x-rays and gamma-rays, as well as particle radiations, that can jeopardize the lives of astronauts living and working in space.This visualization tours the regions of near-Earth orbit; the Earth's magnetosphere, sometimes called geospace; the region between the Earth and the Sun; and finally out beyond Pluto, where Voyager 1 and 2 are exploring the boundary between the Sun and the rest of our Milky Way galaxy. Along the way, we see these regions patrolled by a fleet of satellites that make up NASA's Heliophysics Observatory Telescopes. Many of these spacecraft do not take images in the conventional sense but record fields, particle energies and fluxes in situ. Many of these missions are operated in conjunction with international partners, such as the European Space Agency (ESA) and the Japanese Space Agency (JAXA).The Earth and distances are to scale. Larger objects are used to represent the satellites and other planets for clarity.Here are the spacecraft featured in this movie:Near-Earth Fleet:Hinode: Observes the Sun in multiple wavelengths up to x-rays. SVS pageRHESSI : Observes the Sun in x-rays and gamma-rays. SVS pageTRACE: Observes the Sun in visible and ultraviolet wavelengths. SVS pageTIMED: Studies the upper layers (40-110 miles up) of the Earth's atmosphere.FAST: Measures particles and fields in regions where aurora form.CINDI: Measures interactions of neutral and charged particles in the ionosphere. AIM: Images and measures noctilucent clouds. SVS pageGeospace Fleet:Geotail: Conducts measurements of electrons and ions in the Earth's magnetotail. Cluster: This is a group of four satellites which fly in formation to measure how particles and fields in the magnetosphere vary in space and time. SVS pageTHEMIS: This is a fleet of five satellites to study how magnetospheric instabilities produce substorms. SVS pageL1 Fleet: The L1 point is a Lagrange Point between the Sun and the Earth. Spacecraft can orbit this location for continuous coverage of the Sun.SOHO: Studies the Sun with cameras and a multitude of other instruments. SVS pageACE: Measures the composition and characteristics of the solar wind. Wind: Measures particle flows and fields in the solar wind. Heliospheric FleetSTEREO-A and B: These two satellites observe the Sun, with imagers and particle detectors, off the Earth-Sun line, providing a 3-D view of solar activity. SVS pageHeliopause FleetVoyager 1 and 2: These spacecraft conducted the original 'Planetary Grand Tour' of the solar system in the 1970s and 1980s. They have now travelled further than any human-built spacecraft and are still returning measurements of the interplanetary medium. SVS pageA refined and narrated version of this visualization, Sentinels of the Heliosphere, is now available. || ", "hits": 148 }, { "id": 3478, "url": "https://svs.gsfc.nasa.gov/3478/", "result_type": "Visualization", "release_date": "2007-12-11T00:00:00-05:00", "title": "THEMIS Explores the Earth's Bow Shock", "description": "The solar wind's first contact with the Earth's magnetic field creates a region known as the bow shock, much like the bow wave of a boat moving through the water. This region can also create additional turbulence which generates bursts of explosion-like currents. In this visualization, the orbits of the THEMIS fleet are combined with a 2-D slice from a hybrid magnetosphere simulation which illustrates these turbulent regions in the bow shock. This hybrid magnetosphere simulation treats the slow-moving ions by particle-in-cell computational methods and the faster electrons as a massless fluid. These simulations more accurately represent the magnetospheric physics, enabling a view of turbulent non-linear processes not visible in the simpler magnetohydrodynamic models. In this simulation, the color table is somewhat unusual. In order of increasing density, the colors run from white through violet, blue, green to black. || ", "hits": 52 }, { "id": 3485, "url": "https://svs.gsfc.nasa.gov/3485/", "result_type": "Visualization", "release_date": "2007-12-10T00:00:00-05:00", "title": "THEMIS and the March 2007 Substorm", "description": "NASA's Time History of Events and Macroscale Interactions during Substorms (THEMIS) mission observed the dynamics of a rapidly developing substorm in March of 2007. This visualization combines the orbits of the THEMIS satellites with a magnetohydrodynamical simulation of the Earth's magnetosphere corresponding to this time. || ", "hits": 33 }, { "id": 3391, "url": "https://svs.gsfc.nasa.gov/3391/", "result_type": "Visualization", "release_date": "2006-12-14T00:00:00-05:00", "title": "THEMIS Orbits: Dayside Science Configuration", "description": "In the early part of the mission, the five THEMIS satellites will follow the same orbit single-file. The apogee of the orbit will take the spacecraft just beyond the bow shock of the Earth's magnetosphere. This will enable the satellites to collect data in this region over a short range of time so that the time history can be studied. The dates in this visualization are based on an ephemeris assuming a launch on January 20, 2007. The satellite colors are: red=P1, green=P2, cyan=P3, blue=P4, magenta=P5. || ", "hits": 30 }, { "id": 3392, "url": "https://svs.gsfc.nasa.gov/3392/", "result_type": "Visualization", "release_date": "2006-12-14T00:00:00-05:00", "title": "THEMIS Orbits: Nightside Science Configuration", "description": "In the latter phase of the mission, the five THEMIS spacecraft will travel on five co-aligned elliptical orbits with their apogee on the nightside of the Earth. From there, they will sample the particle and electromagnetic wave environment along the magnetotail. The dates in this visualization are based on an ephemeris assuming a launch date of January 20, 2007. The five satellites are represented by colors: red=P1, green=P2, cyan=P3, blue=P4, magenta=P5 || ", "hits": 47 }, { "id": 3394, "url": "https://svs.gsfc.nasa.gov/3394/", "result_type": "Visualization", "release_date": "2006-12-14T00:00:00-05:00", "title": "THEMIS Orbits: Transitions", "description": "Between the dayside and nightside phases of the mission, the five spacecraft will conduct orbit change maneuvers over a period of three months. During this visualization, the camera position is locked in GSE coordinates, keeping the Sun to the left. The orbital axis is actually fixed in space but appears to move due to the Earth's motion around the Sun. The dates in this visualization are based on an ephemeris assuming a launch on January 20, 2007. The satellites are represented by the colors: red=P1, green=P2, cyan=P3, blue=P4, magenta=P5. || ", "hits": 35 }, { "id": 3356, "url": "https://svs.gsfc.nasa.gov/3356/", "result_type": "Visualization", "release_date": "2006-05-22T00:00:00-04:00", "title": "THEMIS Mission and Substorm Simulation", "description": "This visualization combines simulations of the THEMIS (Time History of Events and Macroscale Interactions during Substorms) mission orbits with a GGCM (Geospace General Circulation Model) simulation. It illustrates how the five THEMIS satellites will work together to detect substorm events in the magnetosphere. One goal of the THEMIS mission is to test how these substorm events are related to the formation of the aurora.This mission consists of five identical spacecraft (usually designated P1, P2, P3, P4 and P5) with orbits aligned so they reach their apogee along the same line from the Earth. This alignment remains fixed in space so as the Earth moves around the Sun, the constellation of spacecraft will extend on the nightside of the Earth in winter to sample the Earth's magnetosphere, and on the dayside of the Earth in summer to sample the incoming solar wind. This way they can better map the geospace environment.Probes P1 and P2 are called the 'outer probes' and P3, 4, and 5 are the 'inner probes'. P3 and P4 share the same orbit. The outer probes will detect the onset of the substorm, while the inner probes will monitor the Earthward plasma flows from the event.For more information on the GGCM model, visit the Community Coordinated Modeling Center and OpenGGCM. || ", "hits": 48 }, { "id": 3311, "url": "https://svs.gsfc.nasa.gov/3311/", "result_type": "Visualization", "release_date": "2005-12-05T00:00:00-05:00", "title": "Zoom-in to plasmapause-induced TEC enhancement - April 2001", "description": "Space weather events which disturb the plasmapause (displayed here as a green surface enclosing the Earth) can propagate down to the Earth's ionosphere. There they enhance the ionosphere electron content which can disrupt radio signals from satellites.NOTE: This visualization shows the Earth's magnetic dipole field lines rotating rigidly with the Earth. Technically, this is inaccurate. Ions and electrons in the lower atmosphere can create currents which can make these lines 'drag' with Earth's rotation, but this will occur mostly near the Earth and not higher up. More details on this process can be found in the FAQ at the The Exploration of the Earth's Magnetosphere web site, Does the Earth's magnetic field rotate?. || ", "hits": 11 }, { "id": 3314, "url": "https://svs.gsfc.nasa.gov/3314/", "result_type": "Visualization", "release_date": "2005-12-05T00:00:00-05:00", "title": "Time-varying Plasmapause and Electron data - April 2001", "description": "This is another view of the plasmapause and electron content data for the April 11, 2001 time frame (similar to ID 3312). This point of view is shifted slightly to the sunlit side of the Earth to present a better view of the plume formation. || ", "hits": 13 }, { "id": 3316, "url": "https://svs.gsfc.nasa.gov/3316/", "result_type": "Visualization", "release_date": "2005-12-05T00:00:00-05:00", "title": "Zoom-in to Plasmapause-Induced TEC Enhancement - April 2001 (Version 2)", "description": "Space weather events which disturb the plasmapause (displayed here as a green surface enclosing the Earth) can propagate down to the Earth's ionosphere. There they enhance the ionosphere electron content which can disrupt radio signals from satellites. This movie is a variation on animation ID 3311 with slightly different camera motions. NOTE: This visualization shows the Earth's magnetic dipole field lines rotating rigidly with the Earth. Technically, this is inaccurate. Ions and electrons in the lower atmosphere can create currents which can make these lines 'drag' with Earth's rotation, but this will occur mostly near the Earth and not higher up. More details on this process can be found in the FAQ at the The Exploration of the Earth's Magnetosphere web site, Does the Earth's magnetic field rotate?. || ", "hits": 20 }, { "id": 3317, "url": "https://svs.gsfc.nasa.gov/3317/", "result_type": "Visualization", "release_date": "2005-12-05T00:00:00-05:00", "title": "Zoom-in to plasmapause-induced TEC enhancement - April 2001", "description": "Space weather events which disturb the plasmapause can propagate down to the Earth's ionosphere. There they enhance the ionosphere electron content which can disrupt radio signals from satellites. This is a re-timed version of ID 3311. This version is designed to play synchronously with ID 3310, ID 3312, and ID 3314.NOTE: This visualization shows the Earth's magnetic dipole field lines rotating rigidly with the Earth. Technically, this is inaccurate. Ions and electrons in the lower atmosphere can create currents which can make these lines 'drag' with Earth's rotation, but this will occur mostly near the Earth and not higher up. More details on this process can be found in the FAQ at the The Exploration of the Earth's Magnetosphere web site, Does the Earth's magnetic field rotate?. || ", "hits": 21 }, { "id": 20066, "url": "https://svs.gsfc.nasa.gov/20066/", "result_type": "Animation", "release_date": "2005-05-05T12:00:00-04:00", "title": "Cutaway View of the Earth's Radiation Belts", "description": "Energetic electrons and ions can get trapped in the Earth's geomagnetic field forming a toroidal region around the planet known as the radiation belts. || radbeltCutaway_640x480_pre.00077_print.jpg (1024x768) [76.3 KB] || radbeltCutaway_640x480_thm.png (80x40) [13.5 KB] || radbeltCutaway_640x480_pre.jpg (320x240) [5.3 KB] || radbeltCutaway_320x240_pre.jpg (320x240) [5.2 KB] || radbeltCutaway_320x240_pre_searchweb.jpg (320x180) [42.7 KB] || radbeltCutaway_NTSC.webmhd.webm (960x540) [1.0 MB] || 720x486_4x3_30 (720x486) [32.0 KB] || radbeltCutaway_640x480.mpg (640x480) [10.7 MB] || radbeltCutaway_NTSC.m2v (720x480) [17.2 MB] || a010068_seq.mpg (720x480) [9.2 MB] || a010068_H264_640x480.mp4 (640x480) [7.4 MB] || radbeltCutaway_320x240.mpg (320x240) [2.8 MB] || ", "hits": 93 }, { "id": 20056, "url": "https://svs.gsfc.nasa.gov/20056/", "result_type": "Animation", "release_date": "2005-03-30T12:00:00-05:00", "title": "Earth's Magnetic Field to Aurora", "description": "Join a ride with electrons along the Earth's magnetic field line to the formation site of the aurora. || ", "hits": 138 }, { "id": 20057, "url": "https://svs.gsfc.nasa.gov/20057/", "result_type": "Animation", "release_date": "2005-03-30T12:00:00-05:00", "title": "A CME Generates Reconnection in Earth's Magnetic Field", "description": "A burst of fast material from the Sun generates magnetic reconnection events in the Earth's magnetic field. This eventually sends high-speed electrons and protons into the Earth's upper atmosphere to form aurora. || ", "hits": 70 }, { "id": 3028, "url": "https://svs.gsfc.nasa.gov/3028/", "result_type": "Visualization", "release_date": "2005-01-12T12:00:00-05:00", "title": "A 3-Dimensional Model of the Magnetosphere (WMS)", "description": "The earth's magnetosphere protects the earth from high-energy charged particles coming from the sun. Some charged particles are deflected by the magnetosphere, while others become trapped and produce the aurora. This presentation shows a 3-dimensional model of the magnetosphere. The features that it highlights are flat ribbons representing the paths of charged particles deflected by the magnetosphere, triangular ribbons representing magnetic field lines, and colored surfaces representing constant values of magnetic force. The original model is in Open Inventor format, and is available here. || ", "hits": 116 }, { "id": 3048, "url": "https://svs.gsfc.nasa.gov/3048/", "result_type": "Visualization", "release_date": "2004-12-15T12:00:00-05:00", "title": "Earth's Radiation Belts Tremble Under Impact of Solar Storm", "description": "Under the wave of energetic particles from the Halloween 2003 solar storm events, the Earth's radiation belts underwent significant changes in structure. This visualization is constructed using daily-averaged particle flux data from the SAMPEX satellite installed in a simple dipole model for the Earth's magnetic field. The toroidal structure of the belts corresponds to regions with electron fluxes in excess of 100 electrons/s/cm^2/steradian with energies of 2-6 MeV. The color-scale on the cross section is violet for low flux and white for high flux. The translucent gray arcs represent the fields lines of the Earth's dipole field. The 3-dimensional structure was built from the SAMPEX measurement by propagating the particle flux values along field lines of a simple magnetic dipole.NOTE: This visualization shows the Earth's magnetic dipole field lines rotating rigidly with the Earth. Technically, this is inaccurate. Ions and electrons in the lower atmosphere can create currents which can make these lines 'drag' with Earth's rotation, but this will occur mostly near the Earth and not higher up. More details on this process can be found in the FAQ at the The Exploration of the Earth's Magnetosphere web site, Does the Earth's magnetic field rotate?. || ", "hits": 41 }, { "id": 3049, "url": "https://svs.gsfc.nasa.gov/3049/", "result_type": "Visualization", "release_date": "2004-12-15T12:00:00-05:00", "title": "Radiation Belts and Plasmapause Fluctuate Under Solar Storm", "description": "In this visualization, we see the interaction of the radiation belts (violet/white), the plasmapause (green surface) and magnetopause (gray surface).NOTE: This visualization shows the Earth's magnetic dipole field lines rotating rigidly with the Earth. Technically, this is inaccurate. Ions and electrons in the lower atmosphere can create currents which can make these lines 'drag' with Earth's rotation, but this will occur mostly near the Earth and not higher up. More details on this process can be found in the FAQ at the The Exploration of the Earth's Magnetosphere web site, Does the Earth's magnetic field rotate?. || ", "hits": 54 }, { "id": 3052, "url": "https://svs.gsfc.nasa.gov/3052/", "result_type": "Visualization", "release_date": "2004-12-15T12:00:00-05:00", "title": "Earth's Radiation Belts with Safe Zone Orbit", "description": "Spacecraft orbiting in the 'Safe Zone', between two and three Earth radii, can be subjected to high levels of harmful radiation as the radiation belts fluctuate in response to space weather events.NOTE: This visualization shows the Earth's magnetic dipole field lines rotating rigidly with the Earth. Technically, this is inaccurate. Ions and electrons in the lower atmosphere can create currents which can make these lines 'drag' with Earth's rotation, but this will occur mostly near the Earth and not higher up. More details on this process can be found in the FAQ at the The Exploration of the Earth's Magnetosphere web site, Does the Earth's magnetic field rotate?. || ", "hits": 76 }, { "id": 2676, "url": "https://svs.gsfc.nasa.gov/2676/", "result_type": "Visualization", "release_date": "2003-03-18T12:00:00-05:00", "title": "Tour of the Magnetosphere", "description": "Tour of the Earth's magnetosphere generated for 'Live from the Aurora'. This viz pulls out from the Earth and fades in components of the magnetosphere. || ", "hits": 156 }, { "id": 2391, "url": "https://svs.gsfc.nasa.gov/2391/", "result_type": "Visualization", "release_date": "2002-03-01T12:00:00-05:00", "title": "Magnetosphere II: The Solar Wind Strikes Back!", "description": "A view of a computer-generated model of the Earth's magnetosphere. Semi-transparent surfaces represent particle density (red is high, blue is low), the silvery tube represent magnetic field lines and the yellow ribbons represent the paths of charged solar wind particles. In this particular model, the solar wind has an ambient density of 8.35 particles/cm^3. The isosurfaces are then red (> 17 particles/cm^3), yellow (> 12 particles/cm^3), green (> 8.6 particles/cm^3) and blue (< 1.0 particle/cm^3). || ", "hits": 60 }, { "id": 2387, "url": "https://svs.gsfc.nasa.gov/2387/", "result_type": "Visualization", "release_date": "2002-02-28T12:00:00-05:00", "title": "The Magnetosphere: Earth Raises its Shields", "description": "A view of a computer-generated model of the Earth's magnetosphere. Semi-transparent surfaces represent particle density (red is high, blue is low) and silvery tubes represent the magnetic field lines. In this particular model, the solar wind has an ambient density of 8.35 particles/cm^3. The isosurfaces are then red (> 17 particles/cm^3), yellow (> 12 particles/cm^3), green (> 8.6 particles/cm^3) and blue (< 1.0 particle/cm^3). || ", "hits": 88 }, { "id": 88, "url": "https://svs.gsfc.nasa.gov/88/", "result_type": "Visualization", "release_date": "1995-12-07T12:00:00-05:00", "title": "Magnetic Cloud Event: October 18-20, 1995", "description": "This animation presents correlated measurements and model data for an impact of a magnetic cloud originating from the Sun on the Earths magnetosphere on October 18-20, 1995. || a000088.00095_web.png (720x480) [357.3 KB] || a000088_thm.png (80x40) [3.9 KB] || a000088_pre.jpg (320x238) [11.4 KB] || a000088_pre_searchweb.jpg (320x180) [49.4 KB] || a000088.webmhd.webm (960x540) [14.4 MB] || a000088.dv (720x480) [186.0 MB] || a000088.mp4 (640x480) [10.5 MB] || a000088.mpg (352x240) [7.8 MB] || ", "hits": 42 } ] }