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    "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": 224
        },
        {
            "id": 14892,
            "url": "https://svs.gsfc.nasa.gov/14892/",
            "result_type": "Produced Video",
            "release_date": "2025-08-29T16:00:00-04:00",
            "title": "Solar Wind Animations",
            "description": "The Sun releases a constant stream of charged particles, called the solar wind. The solar wind originates  in the outermost layer of the Sun’s atmosphere, the corona, when plasma is heated to a point that the Sun’s gravity can’t hold it down. When this plasma escapes – often reaching speeds of over one million miles per hour – it drags  the Sun’s magnetic out across the solar system. When the solar wind encounters Earth, it is deflected by our planet's magnetic shield, causing most of the solar wind's energetic particles to flow around and beyond us. However, some of these high-energy particles can sneak past Earth’s natural magnetic defenses and produce hazardous conditions for satellites and astronauts, as well as power grids and infrastructure on Earth.Learn more about the solar wind: https://science.nasa.gov/sun/what-is-the-solar-wind/ || ",
            "hits": 965
        },
        {
            "id": 14876,
            "url": "https://svs.gsfc.nasa.gov/14876/",
            "result_type": "Produced Video",
            "release_date": "2025-07-25T15:00:00-04:00",
            "title": "NASA’s TRACERS Mission Launches to Study Earth’s Magnetic Shield",
            "description": "NASA’s newest mission, TRACERS, soon will begin studying how Earth’s magnetic shield protects our planet from the effects of space weather. Short for Tandem Reconnection and Cusp Electrodynamics Reconnaissance Satellites, the twin TRACERS spacecraft lifted off at 11:13 a.m. PDT (2:13 p.m. EDT) Wednesday, July 23, 2025, aboard a SpaceX Falcon 9 rocket from Space Launch Complex 4 East at Vandenberg Space Force Base in California.Learn more about the mission: https://science.nasa.gov/mission/tracers/ || ",
            "hits": 129
        },
        {
            "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": 192
        },
        {
            "id": 14862,
            "url": "https://svs.gsfc.nasa.gov/14862/",
            "result_type": "Produced Video",
            "release_date": "2025-07-14T11:00:00-04:00",
            "title": "NASA’s TRACERS Studies Magnetic Explosions Above Earth",
            "description": "NASA's TRACERS mission, or the Tandem Reconnection and Cusp Electrodynamics Reconnaissance Satellites, will fly in low Earth orbit through the polar cusps, funnel-shaped holes in the magnetic field, to study magnetic reconnection and its effects in Earth's atmosphere. Magnetic reconnection is a mysterious process that happens when the solar wind, made of electrically charged particles and magnetic fields from the Sun, collides with Earth's magnetic shield, causing magnetic field lines to violently snap and explosively fling away particles at high speeds. This process has huge impacts on Earth, from causing breathtaking auroras to disrupting communications and power grids on Earth. TRACERS is launching no earlier than summer 2025 aboard a SpaceX Falcon 9 rocket from Space Launch Complex 4 East at Vandenberg Space Force Base in California.Find out more about the TRACERS mission and how it will help us better understand the ways space weather affects us on Earth: https://science.nasa.gov/mission/tracers/ || ",
            "hits": 378
        },
        {
            "id": 20404,
            "url": "https://svs.gsfc.nasa.gov/20404/",
            "result_type": "Animation",
            "release_date": "2025-06-02T12:00:00-04:00",
            "title": "TRACERS Science Animations",
            "description": "The TRACERS, or the Tandem Reconnection and Cusp Electrodynamics Reconnaissance Satellites, mission will help scientists understand an explosive process called magnetic reconnection and its effects in Earth’s atmosphere. Magnetic reconnection occurs when magnetic fields and particles from the Sun interact with Earth’s magnetic field. By understanding this process, scientists will be able to better understand and prepare for impacts of solar activity on Earth, such as auroras and disruptions to telecommunications.Learn more about the mission:  https://science.nasa.gov/mission/tracers/ || ",
            "hits": 149
        },
        {
            "id": 14829,
            "url": "https://svs.gsfc.nasa.gov/14829/",
            "result_type": "Produced Video",
            "release_date": "2025-04-25T10:00:00-04:00",
            "title": "TRACERS Thermal Vacuum Testing at Millennium Space Systems",
            "description": "NASA’s Tandem Reconnection and Cusp Electrodynamics Reconnaissance Satellites, or TRACERS, is embarking on its integration and testing campaign, during which all of the instruments and components will be added to the spacecraft structure, tested to ensure they will survive the harsh environments of launch and space, and made ready to execute its mission. The TRACERS mission will help scientists understand an explosive process called magnetic reconnection and its effects in Earth’s atmosphere. Magnetic reconnection occurs when magnetic fields and particles from the Sun interact with Earth’s magnetic field. By understanding this process, scientists will be able to better understand and prepare for impacts of solar activity on Earth, such as auroras and disruptions to telecommunications.Below are clips of Millennium Space Systems’ team members conducting Thermal Vacuum (TVAC) testing at the Boeing Space Systems Laboratory in El Segundo, California.Learn more about the mission: https://science.nasa.gov/mission/tracers/ || ",
            "hits": 146
        },
        {
            "id": 14827,
            "url": "https://svs.gsfc.nasa.gov/14827/",
            "result_type": "Produced Video",
            "release_date": "2025-04-24T15:00:00-04:00",
            "title": "TRACERS Instrument Development & Testing at the University of Iowa",
            "description": "NASA’s Tandem Reconnection and Cusp Electrodynamics Reconnaissance Satellites, or TRACERS, is embarking on its integration and testing campaign, during which all of the instruments and components will be added to the spacecraft structure, tested to ensure they will survive the harsh environments of launch and space, and made ready to execute its mission. The TRACERS mission will help scientists understand an explosive process called magnetic reconnection and its effects in Earth’s atmosphere. Magnetic reconnection occurs when magnetic fields and particles from the Sun interact with Earth’s magnetic field. By understanding this process, scientists will be able to better understand and prepare for impacts of solar activity on Earth, such as auroras and disruptions to telecommunications.Below are clips of TRACERS’ instrument design, build, and testing at the University of Iowa in Iowa City, Iowa.Learn more about the mission: https://science.nasa.gov/mission/tracers/ || ",
            "hits": 50
        },
        {
            "id": 14828,
            "url": "https://svs.gsfc.nasa.gov/14828/",
            "result_type": "Produced Video",
            "release_date": "2025-04-24T15:00:00-04:00",
            "title": "TRACERS Testing & Integration at Millennium Space Systems",
            "description": "NASA’s Tandem Reconnection and Cusp Electrodynamics Reconnaissance Satellites, or TRACERS, is embarking on its integration and testing campaign, during which all of the instruments and components will be added to the spacecraft structure, tested to ensure they will survive the harsh environments of launch and space, and made ready to execute its mission. The TRACERS mission will help scientists understand an explosive process called magnetic reconnection and its effects in Earth’s atmosphere. Magnetic reconnection occurs when magnetic fields and particles from the Sun interact with Earth’s magnetic field. By understanding this process, scientists will be able to better understand and prepare for impacts of solar activity on Earth, such as auroras and disruptions to telecommunications.Below are clips of TRACERS’ testing and integration at the Millennium Space Systems Small Satellite Factory in El Segundo, California. Learn more about the mission: https://science.nasa.gov/mission/tracers/ || ",
            "hits": 71
        },
        {
            "id": 14805,
            "url": "https://svs.gsfc.nasa.gov/14805/",
            "result_type": "Animation",
            "release_date": "2025-03-24T12:00:00-04:00",
            "title": "TRACERS Spacecraft Beauty Passes",
            "description": "The TRACERS, or the Tandem Reconnection and Cusp Electrodynamics Reconnaissance Satellites, mission will help scientists understand an explosive process called magnetic reconnection and its effects in Earth’s atmosphere. Magnetic reconnection occurs when magnetic fields and particles from the Sun interact with Earth’s magnetic field. By understanding this process, scientists will be able to better understand and prepare for impacts of solar activity on Earth, such as auroras and disruptions to telecommunications.Learn more about the mission: https://science.nasa.gov/mission/tracers/ || ",
            "hits": 66
        },
        {
            "id": 14628,
            "url": "https://svs.gsfc.nasa.gov/14628/",
            "result_type": "Produced Video",
            "release_date": "2024-08-28T11:30:00-04:00",
            "title": "Discovering Earth’s Third Global Energy Field",
            "description": "High above the Earth’s North and South Poles, a steady stream of particles escapes from our atmosphere into space. Scientists call this mysterious outflow the “polar wind,” and for almost 60 years, spacecraft have been flying through it as scientists have theorized about its cause. The leading theory was that a planet-wide electric field was drawing those particles up into space. But this so-called ambipolar electric field, if it exists, is so weak that all attempts to measure it have failed – until now.In 2022, scientists traveled to Svalbard, a small archipelago in Norway, to launch a rocket in an attempt to measure Earth’s ambipolar electric field for the first time. This was NASA’s Endurance rocketship mission, and this is its story.To learn more, visit: https://science.nasa.gov/science-research/heliophysics/nasa-discovers-long-sought-global-electric-field-on-earth/ || ",
            "hits": 329
        },
        {
            "id": 5240,
            "url": "https://svs.gsfc.nasa.gov/5240/",
            "result_type": "Visualization",
            "release_date": "2024-04-22T00:00:00-04:00",
            "title": "Radio Signal Reflection & Refraction on a Simple Ionosphere Model",
            "description": "A simple animated plotting of radio wave refraction and reflection on a simplified ionosphere model, landscape format. || polar.propagation.basic.sample.1920x1080.png (1920x1080) [178.8 KB] || polar.propagation.basic.sample.1920x1080.1590_print.jpg (1024x576) [69.8 KB] || polar.propagation.basic.sample.1920x1080.1590_searchweb.png (320x180) [20.5 KB] || polar.propagation.basic.sample.1920x1080.1590_thm.png (80x40) [3.2 KB] || polar.propagation.basic.sample.1920x1080_p30.mp4 (1920x1080) [456.4 KB] || polar.propagation.basic.sample.1920x1080 (1920x1080) [0 Item(s)] || ",
            "hits": 198
        },
        {
            "id": 14299,
            "url": "https://svs.gsfc.nasa.gov/14299/",
            "result_type": "Produced Video",
            "release_date": "2023-03-10T10:00:00-05:00",
            "title": "What is Plasma?",
            "description": "Plasma makes up 99.9% of the visible universe, but what is it? This video discusses what plasma is, where it lives, and how NASA studies it. || ",
            "hits": 799
        },
        {
            "id": 4987,
            "url": "https://svs.gsfc.nasa.gov/4987/",
            "result_type": "Visualization",
            "release_date": "2022-04-28T11:00:00-04:00",
            "title": "Fast Magnetic Reconnection and the Hall Effect",
            "description": "Magnetic reconnection is one of the most complex processes known for converting energy from magnetic fields to particle motion.  It takes place in solar flares and regions of planetary (and stellar) magnetospheres.  Having been studied since the 1950s, many details of the process are still undergoing study.One of the key components in magnetic reconnection is the collision of two magnetic field regions with opposite-directed field lines, imbedded in a plasma.  The field and plasma combination forms an X-shaped configuration at their closest, and most intense point.These visualizations are plotted from a reconnection model generated by VPIC (Vector Particle-In-Cell) code.  Quantities are plotted in 'dimensionless' coordinates, that are normalized to the ion inertial length (di). || ",
            "hits": 141
        },
        {
            "id": 13687,
            "url": "https://svs.gsfc.nasa.gov/13687/",
            "result_type": "Produced Video",
            "release_date": "2020-08-14T10:00:00-04:00",
            "title": "NASA Spacecraft Uncover Mystery Behind Auroral Beads",
            "description": "A special type of aurora, draped east-west across the night sky like a glowing pearl necklace, is helping scientists better understand the science of auroras and their powerful drivers out in space. Known as auroral beads, these lights often show up just before large auroral displays, which are caused by electrical storms in space called substorms. Until now, scientists weren’t sure if auroral beads are somehow connected to other auroral displays as a phenomenon in space that precedes substorms, or if they are caused by disturbances closer to Earth’s atmosphere.But powerful new computer models, combined with observations from NASA’s Time History of Events and Macroscale Interactions during Substorms – THEMIS – mission, have provided the first direct evidence of the events in space that lead to the appearance of these beads, and demonstrated the important role they play in our local space environment. || ",
            "hits": 87
        },
        {
            "id": 13282,
            "url": "https://svs.gsfc.nasa.gov/13282/",
            "result_type": "Produced Video",
            "release_date": "2019-12-04T13:00:00-05:00",
            "title": "5 New Discoveries from NASA's Parker Solar Probe",
            "description": "Music Credit: Smooth as Glass by The Freeharmonic OrchestraWatch this video on the NASA Goddard YouTube channel.Complete transcript available. || parkerscience.thumb.jpg (1920x1080) [731.2 KB] || parkerscience.thumb_thm.png (80x40) [6.8 KB] || parkerscience.thumb_searchweb.png (320x180) [87.7 KB] || 13282_ParkerFirstScience_Twitter1080.mp4 (1920x1080) [53.4 MB] || 13282_ParkerFirstScience.YouTube1080.webm (1920x1080) [26.9 MB] || 13282_ParkerFirstScience.mp4 (1920x1080) [246.1 MB] || 13282_ParkerFirstScience_Mobile1080.mp4 (1920x1080) [194.5 MB] || 13282_ParkerFirstScience.YouTube1080.mp4 (1920x1080) [387.1 MB] || 13282_ParkerFirstScience_Twitter1080.en_US.srt [4.5 KB] || 13282_ParkerFirstScience_Twitter1080.en_US.vtt [4.5 KB] || 13282_ParkerFirstScienceMASTER.APR1080.mov (1920x1080) [3.2 GB] || ",
            "hits": 147
        },
        {
            "id": 13275,
            "url": "https://svs.gsfc.nasa.gov/13275/",
            "result_type": "Produced Video",
            "release_date": "2019-08-07T11:30:00-04:00",
            "title": "How NASA Will Protect Astronauts From Space Radiation",
            "description": "Today, the Apollo-era flares serve as a reminder of the threat of radiation exposure for technology and astronauts in space. Understanding and predicting solar eruptions is crucial for safe space exploration. Almost 50 years since those 1972 storms, the data, technology and resources available to NASA have improved, enabling advancements towards space weather forecasts and astronaut protection — key to NASA’s Artemis program to return astronauts to the Moon.",
            "hits": 724
        },
        {
            "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": 439
        },
        {
            "id": 4560,
            "url": "https://svs.gsfc.nasa.gov/4560/",
            "result_type": "Visualization",
            "release_date": "2017-03-31T09:00:00-04:00",
            "title": "Alfvén Waves - Basic",
            "description": "Alfven waves represented by undulation in the magnetic field vector. || AlfvenWaveBasic_staticXwide_inertial.HD1080i.0300_print.jpg (1024x576) [158.5 KB] || AlfvenWaveBasic_staticXwide_inertial.HD1080i.0300_thm.png (80x40) [4.6 KB] || AlfvenWaveBasic_staticXwide_inertial.HD1080i.0300_web.png (320x180) [71.9 KB] || WavesOnly (1920x1080) [128.0 KB] || AlfvenWaveBasic_staticXwide.HD1080i_p30.mp4 (1920x1080) [34.0 MB] || AlfvenWaveBasic_staticXwide.HD1080i_p30.webm (1920x1080) [4.9 MB] || ",
            "hits": 316
        },
        {
            "id": 4561,
            "url": "https://svs.gsfc.nasa.gov/4561/",
            "result_type": "Visualization",
            "release_date": "2017-03-31T09:00:00-04:00",
            "title": "Alfvén Waves - Kinetic",
            "description": "Kinetic Alfven waves represented by undulation in the magnetic field vector. || AlfvenWaveKinetic_staticXwide_inertial.HD1080i.0300_print.jpg (1024x576) [155.7 KB] || WavesOnly (1920x1080) [128.0 KB] || AlfvenWaveKinetic_staticXwide.HD1080i_p30.mp4 (1920x1080) [37.9 MB] || AlfvenWaveKinetic_staticXwide.HD1080i_p30.webm (1920x1080) [4.9 MB] || ",
            "hits": 105
        },
        {
            "id": 12512,
            "url": "https://svs.gsfc.nasa.gov/12512/",
            "result_type": "Produced Video",
            "release_date": "2017-03-31T09:00:00-04:00",
            "title": "Observations Reshape Basic Plasma Wave Physics",
            "description": "Music credit: Coolheaded by Jeff CardoniComplete transcript available. || 12512_Observations_Reshape_Basic_Plasma_Wave_Physics_V5_prores.00282_print.jpg (1024x576) [26.7 KB] || 12512_Observations_Reshape_Basic_Plasma_Wave_Physics_V5_prores.00282_searchweb.png (320x180) [16.4 KB] || 12512_Observations_Reshape_Basic_Plasma_Wave_Physics_V5_prores.00282_thm.png (80x40) [2.5 KB] || 12512_Observations_Reshape_Basic_Plasma_Wave_Physics_V5.webm (960x540) [31.9 MB] || 12512_Observations_Reshape_Basic_Plasma_Wave_Physics_V5_appletv.m4v (1280x720) [46.8 MB] || 12512_Observations_Reshape_Basic_Plasma_Wave_Physics_V5_large.mp4 (1920x1080) [83.0 MB] || 12512_Observations_Reshape_Basic_Plasma_Wave_Physics_V5_prores.mov (1280x720) [1.0 GB] || 12512_Observations_Reshape_Basic_Plasma_Wave_Physics_V5_youtube_hq.mov (1920x1080) [141.1 MB] || 12512_Observations_Reshape_Basic_Plasma_Wave_Physics_V5_appletv_subtitles.m4v (1280x720) [46.9 MB] || 12512_Observations_Reshape_Basic_Plasma_Wave_Physics_V3.en_US.srt [1.6 KB] || 12512_Observations_Reshape_Basic_Plasma_Wave_Physics_V3.en_US.vtt [1.6 KB] || 12512_Observations_Reshape_Basic_Plasma_Wave_Physics_V5_ipod_sm.mp4 (320x240) [15.0 MB] || ",
            "hits": 60
        },
        {
            "id": 4513,
            "url": "https://svs.gsfc.nasa.gov/4513/",
            "result_type": "Visualization",
            "release_date": "2016-11-14T13:00:00-05:00",
            "title": "Shock Drift Acceleration (SDA)",
            "description": "This visualization of particle acceleration across a shock is a simplied representation of shock drift acceleration (SDA) showing the motion of electrons (yellow) and protons (blue).  It is presented with the same color table designations as other critters in our Plasma Zoo. || SDAShock_tour_inertial.HD1080i.1000_print.jpg (1024x576) [124.6 KB] || SDAShock_tour_inertial.HD1080i.1000_searchweb.png (320x180) [83.0 KB] || SDAShock_tour_inertial.HD1080i.1000_thm.png (80x40) [5.3 KB] || StandardVersion (1920x1080) [0 Item(s)] || SDAShock_tour_standard.HD1080i_p30.mp4 (1920x1080) [72.8 MB] || SDAShock_tour_standard.HD1080i_p30.webm (1920x1080) [7.1 MB] || StandardVersion (3840x2160) [0 Item(s)] || SDAShock_tour_standard.UHD3840_2160p30.mp4 (3840x2160) [232.9 MB] || SDAShock_tour_standard.HD1080i_p30.mp4.hwshow [200 bytes] || ",
            "hits": 108
        },
        {
            "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": 136
        },
        {
            "id": 10204,
            "url": "https://svs.gsfc.nasa.gov/10204/",
            "result_type": "Produced Video",
            "release_date": "2015-02-18T11:30:00-05:00",
            "title": "MMS Mission Overview",
            "description": "Watch this video on the NASAexplorer YouTube channel.For complete transcript, click here. || missionoverview_print.jpg (1024x576) [146.3 KB] || missionoverview.jpg (1280x720) [125.0 KB] || missionoverview_thm.png (80x40) [16.6 KB] || missionoverview_web.png (320x180) [72.7 KB] || missionoverview_searchweb.png (320x180) [72.7 KB] || missionoverview_web.jpg (320x180) [28.5 KB] || G2014-103_MMS_Mission_OverviewMASTER_appletv.webm (960x540) [31.6 MB] || G2014-103_MMS_Mission_OverviewMASTER_appletv_subtitles.m4v (960x540) [117.8 MB] || G2014-103_MMS_Mission_OverviewMASTER_youtube_hq.mov (1280x720) [183.1 MB] || G2014-103_MMS_Mission_OverviewMASTER_appletv.m4v (960x540) [117.9 MB] || G2014-103_MMS_Mission_OverviewMASTER_1280x720.wmv (1280x720) [136.2 MB] || G2014-103_MMS_Mission_OverviewMASTER_ipod_lg.m4v (640x360) [47.2 MB] || G2014-103_MMS_Mission_OverviewMASTER.en_US.vtt [5.6 KB] || G2014-103_MMS_Mission_OverviewMASTER.en_US.srt [5.6 KB] || G2014-103_MMS_Mission_OverviewMASTER_nasaportal.mov (640x360) [109.7 MB] || G2014-103_MMS_Mission_OverviewMASTER_ipod_sm.mp4 (320x240) [25.0 MB] || G2014-103_MMS_Mission_OverviewMASTER_prores.mov (1280x720) [4.3 GB] || ",
            "hits": 145
        },
        {
            "id": 4088,
            "url": "https://svs.gsfc.nasa.gov/4088/",
            "result_type": "Visualization",
            "release_date": "2013-09-26T14:00:00-04:00",
            "title": "Reconnection Fronts - What the Models Say...",
            "description": "Mathematical models of Earth's magnetosphere have become increasingly more complex and accurate. They have sufficient detail to illustrate many small-scale phenomena.In this simulation run of the Geospace General Circulation Model (GGCM) we see new details that have been observed by in situ satellites. As the solar wind is deflected around Earth's magnetosphere (the 'bubble' of plasma surrounding Earth held by Earth's magnetic field), plasma flows within the bubble can change. In the graphics below, physical variables such as magnetic field and electric currents are plotted. With these variables, we overlay the net flow of the plasma (arrows), subjected to selection criteria to separate flows of plasma away from Earth and towards Earth. Green arrows are low-speed flows (below about 150 kilometers/second), while red arrows correspond to high-speed plasmal flows (about 300 kilometers/second and higher). || ",
            "hits": 59
        },
        {
            "id": 11309,
            "url": "https://svs.gsfc.nasa.gov/11309/",
            "result_type": "Produced Video",
            "release_date": "2013-09-26T14:00:00-04:00",
            "title": "Several NASA Spacecraft Track Energy Through Space",
            "description": "Taking advantage of an unprecedented alignment of eight satellites through the vast magnetic environment that surrounds Earth in space, including NASA's ARTEMIS and THEMIS, scientists now have comprehensive details of the energy's journey through a process that forms the aurora, called a substorm. Their results showed that small events unfolding over the course of a millisecond can result in energy flows that last up to half an hour and cover an area 10 times larger than Earth.Trying to understand how gigantic explosions on the sun can create space weather effects involves tracking energy from the original event all the way to Earth. It's not unlike keeping tabs on a character in a play with many costume changes, because the energy changes form frequently along its journey: magnetic energy causes eruptions that lead to kinetic energy as particles hurtle away, or thermal energy as the particles heat up. Near Earth, the energy can change through all these various forms once again.Most of the large and small features of substorms take place largely in the portion of Earth's magnetic environment called the magnetotail. Earth sits inside a large magnetic bubble called the magnetosphere. As Earth orbits around the sun, the solar wind from the sun streams past the bubble, stretching it outward into a teardrop. The magnetotail is the long point of the teardrop trailing out to more than 1 million miles on the night side of Earth. The moon orbits Earth much closer, some 240,000 miles away, crossing in and out of the magnetotail. || ",
            "hits": 87
        },
        {
            "id": 11301,
            "url": "https://svs.gsfc.nasa.gov/11301/",
            "result_type": "Produced Video",
            "release_date": "2013-07-10T12:30:00-04:00",
            "title": "IBEX Provides First View Of the Solar System’s Tail",
            "description": "This page contains resources from the July 10, 2013 media briefing.To watch the media briefing on YouTube, click here.To view the web short on YouTube about this story, click here.NASA’s Interstellar Boundary Explorer, or IBEX, recently mapped the boundaries of the solar system’s tail, called the heliotail. By combining observations from the first three years of IBEX imagery, scientists have mapped out a tail that shows a combination of fast and slow moving particles. The entire structure twisted, because it experiences the pushing and pulling of magnetic fields outside the solar system. || ",
            "hits": 89
        },
        {
            "id": 11168,
            "url": "https://svs.gsfc.nasa.gov/11168/",
            "result_type": "Produced Video",
            "release_date": "2013-02-20T10:00:00-05:00",
            "title": "SDO Sees Fiery Looping Rain on the Sun",
            "description": "Eruptive events on the sun can be wildly different. Some come just with a solar flare, some with an additional ejection of solar material called a coronal mass ejection (CME), and some with complex moving structures in association with changes in magnetic field lines that loop up into the sun's atmosphere, the corona. On July 19, 2012, an eruption occurred on the sun that produced all three. A moderately powerful solar flare exploded on the sun's lower right hand limb, sending out light and radiation. Next came a CME, which shot off to the right out into space. And then, the sun treated viewers to one of its dazzling magnetic displays — a phenomenon known as coronal rain. Over the course of the next day, hot plasma in the corona cooled and condensed along strong magnetic fields in the region. Magnetic fields, themselves, are invisible, but the charged plasma is forced to move along the lines, showing up brightly in the extreme ultraviolet wavelength of 304 angstroms, which highlights material at a temperature of about 50,000 Kelvin. This plasma acts as a tracer, helping scientists watch the dance of magnetic fields on the sun, outlining the fields as it slowly falls back to the solar surface. The footage in this video was collected by the Solar Dynamics Observatory's AIA instrument. SDO collected one frame every 12 seconds, and the movie plays at 30 frames per second, so each second in this video corresponds to 6 minutes of real time. The video covers 12:30 a.m. EDT to 10:00 p.m. EDT on July 19, 2012.Watch this video on YouTube. || ",
            "hits": 178
        },
        {
            "id": 3945,
            "url": "https://svs.gsfc.nasa.gov/3945/",
            "result_type": "Visualization",
            "release_date": "2012-04-20T00:00:00-04:00",
            "title": "Plasma 'Dance' on the Sun!",
            "description": "Full resolution 4Kx4K SDO images || SDO_2011-09-25_171_Wispy.00900.jpg (4096x4096) [2.2 MB] || SDO_2011-09-25_171_Wispy.00900_web.png (320x320) [100.9 KB] || SDO_2011-09-25_171_Wispy.00900_thm.png (80x40) [6.1 KB] || SDO_2011-09-25_171_Wispy.00900_searchweb.png (320x180) [96.0 KB] || SDO_2011-09-25_171_Wispy_1Kx1K.mp4 (1024x1024) [27.4 MB] || SDO_2011-09-25_171_Wispy_1Kx1K.mov (1024x1024) [27.4 MB] || SDO_2011-09-25_171_Wispy_2Kx2K.webmhd.webm (960x540) [8.1 MB] || SDO_2011-09-25_171_Wispy_2Kx2K.mp4 (2048x2048) [207.3 MB] || 4096x4096_1x1_30p (4096x4096) [0 Item(s)] || SDO_2011-09-25_171_Wispy.mp4 (4096x4096) [651.1 KB] || SDO_2011-09-25_171_Wispy_iPod.m4v (480x480) [11.3 MB] || ",
            "hits": 70
        },
        {
            "id": 10745,
            "url": "https://svs.gsfc.nasa.gov/10745/",
            "result_type": "Produced Video",
            "release_date": "2011-06-07T09:00:00-04:00",
            "title": "SDO Catches Surf Waves on the Sun",
            "description": "Scientists have spotted the iconic surfer's wave rolling through the atmosphere of the sun. This makes for more than just a nice photo-op: the waves hold clues as to how energy moves through that atmosphere, known as the corona. Since scientists know how these kinds of waves — initiated by a Kelvin-Helmholtz instability if you're being technical — disperse energy in the water, they can use this information to better understand the corona. This in turn, may help solve an enduring mystery of why the corona is thousands of times hotter than originally expected.Kelvin-Helmholtz instabilities occur when two fluids of different densities or different speeds flow by each other. In the case of ocean waves, that's the dense water and the lighter air. As they flow past each other, slight ripples can be quickly amplified into the giant waves loved by surfers. In the case of the solar atmosphere, which is made of a very hot and electrically charged gas called plasma, the two flows come from an expanse of plasma erupting off the sun's surface as it passes by plasma that is not erupting. The difference in flow speeds and densities across this boundary sparks the instability that builds into the waves. In order to confirm this description, the team developed a computer model to see what takes place in the region. Their model showed that these conditions could indeed lead to giant surfing waves rolling through the corona. Seeing the big waves suggests they can cascade down to smaller forms of turbulence too. Scientists believe that the friction created by turbulence — the simple rolling of material over and around itself — could help add heating energy to the corona. The analogy is the way froth at the top of a surfing wave provides friction that will heat up the wave. || ",
            "hits": 34
        },
        {
            "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": 43
        },
        {
            "id": 97,
            "url": "https://svs.gsfc.nasa.gov/97/",
            "result_type": "Visualization",
            "release_date": "1996-02-08T12:00:00-05:00",
            "title": "Images of Earth and Space: The Role of Visualization in NASA Science",
            "description": "This compilation video contains visualizations of Earth and Space Sciences resulting from supercomputer models. The excerpted visualizations include: Ocean Planet, El Niño, Ozone 1991, Clouds, Changes in Glacier Bay, Alaska, Biosphere, Lunar Topography from the Clementine Mission, Musculoskeletal Modeling Dynamic Simulations, Simulations of the Breakup and Dynamical Evolution of Comet Shoemaker-Levy 9, Convective Penetration in Stellar Interiors, Topological Features of a Compressible Plasma Vortex Sheet: A Model for the Outer Heliospheric Solar Wind, R-Aquarii Jet, The Evolution of Distorted Black Holes, Rayleigh-Taylor Instability in a Supernova, Galaxy Harassment, N-Body Simulation of the Cold Dark Matter Cosmology. || ",
            "hits": 214
        },
        {
            "id": 8,
            "url": "https://svs.gsfc.nasa.gov/8/",
            "result_type": "Visualization",
            "release_date": "1993-12-17T12:00:00-05:00",
            "title": "Topological Features of a Compressible Plasma Vortex Sheet: 6 Cases",
            "description": "The Voyager and Pioneer Spacecraft have detected large-scale quasi-periodic plasma fluctuations in the outer heliosphere beyond 20 AU. A plasma vortex sheet model can explain these fluctuations and the observed correlations between various physical variables. The large scale outer heliosphere is modeled by solving the 3-D compressible magnetohydrodynamic equations involving three interacting shear layers.Computations were done on a Cray computer at the NASA Center for Computational Sciences.Six cases are animated: Weak magnetic field and strong magnetic field, each at three values of tau, the vortex street characteristic time. Contours of density are shown as dark transparent 'tubes'. Critical points of the velocity field are represented by 'Glyphs'. Vortex cores are shown in orange and blue. || ",
            "hits": 83
        },
        {
            "id": 9,
            "url": "https://svs.gsfc.nasa.gov/9/",
            "result_type": "Visualization",
            "release_date": "1993-12-17T12:00:00-05:00",
            "title": "Topological Features of a Compressible Plasma Vortex Sheet - a Model of the Outer Heliospheric Wind",
            "description": "The Voyager and Pioneer Spacecraft have detected large-scale quasi-periodic plasma fluctuations in the outer heliosphere beyond 20 AU. A plasma vortex sheet model can explain these fluctuations and the observed correlations between various physical variables. The large scale outer heliosphere is modeled by solving the 3-D compressible magnetohydrodynamic equations involving three interacting shear layers. Computations were done on a Cray computer at the NASA Center for Computational Sciences. Six cases are animated: Weak magnetic field and strong magnetic field, each at three values of tau, the vortex street characteristic time. Contours of densityare shown as dark transparent 'tubes'. Critical points of the velocity field are represented by 'Glyphs'. Vortex cores are shown in orange and blue. || ",
            "hits": 62
        }
    ]
}