{ "count": 127, "next": "https://svs.gsfc.nasa.gov/api/search/?keywords=Magnetic+Fields&limit=100&offset=100", "previous": null, "results": [ { "id": 14949, "url": "https://svs.gsfc.nasa.gov/14949/", "result_type": "Produced Video", "release_date": "2026-01-09T09:00:00-05:00", "title": "NASA Monitors Space Weather 24/7", "description": "Our Sun creates conditions in space, called space weather, that can affect our technologies both in space and on Earth — from GPS satellites to airplanes to power grids. NASA’s Space Weather Program monitors space weather 24 hours a day, 7 days a week. This important work helps decision makers not only protect people and equipment but maintain the services our modern-day society relies on every day. NASA’s space weather monitoring is also critical for safeguarding astronauts as they journey to the Moon and onward to Mars. || ", "hits": 265 }, { "id": 14666, "url": "https://svs.gsfc.nasa.gov/14666/", "result_type": "Produced Video", "release_date": "2025-11-13T12:00:00-05:00", "title": "ESCAPADE Launch Phase and Deployment Animations", "description": "The Escape and Plasma Acceleration and Dynamics Explorers, or ESCAPADE, will use two identical spacecraft to investigate how the solar wind interacts with Mars’ magnetic environment and how this interaction drives the planet’s atmospheric escape. The first multi-spacecraft orbital science mission to the Red Planet, ESCAPADE’s twin orbiters will take simultaneous observations from different locations around Mars to reveal the planet’s real-time response to space weather and how the Martian magnetosphere changes over time.The ESCAPADE mission will be carried into orbit on the second launch of Blue Origin’s New Glenn rocket. New Glenn is a single-configuration, heavy-lift orbital launch vehicle capable of routinely carrying both spacecraft and people to low Earth orbits, geostationary transfer orbits, cislunar orbits (between Earth and the Moon), and beyond via Earth-departure orbits like the one required for ESCAPADE. The vehicle is named after John Glenn, the first American astronaut to orbit Earth.The ESCAPADE mission is managed by the Space Sciences Laboratory at the University of California, Berkeley, with key partners Rocket Lab, NASA's Goddard Space Flight Center, Embry-Riddle Aeronautical University, Advanced Space LLC, and Blue Origin. || ", "hits": 134 }, { "id": 14915, "url": "https://svs.gsfc.nasa.gov/14915/", "result_type": "Produced Video", "release_date": "2025-11-13T00:00:00-05:00", "title": "ESCAPADE Trajectory Animations", "description": "The Escape and Plasma Acceleration and Dynamics Explorers, or ESCAPADE, mission will use two identical spacecraft to investigate how the solar wind interacts with Mars’ magnetic environment and how this interaction drives the planet’s atmospheric escape. The first multi-spacecraft orbital science mission to the Red Planet, ESCAPADE’s twin orbiters will take simultaneous observations from different locations around Mars to reveal the planet’s real-time response to space weather and how the Martian magnetosphere changes over time.The ESCAPADE mission is being carried into orbit on the second launch of Blue Origin’s New Glenn rocket (NG-2) and is scheduled to launch in November 2025 from Cape Canaveral, Florida. New Glenn is a single-configuration, heavy-lift orbital launch vehicle capable of routinely carrying both spacecraft and people to low Earth orbits, geostationary transfer orbits, cislunar orbits (between Earth and the Moon), and beyond via Earth-departure orbits like the one required for ESCAPADE. The vehicle is named after John Glenn, the first American astronaut to orbit Earth.The ESCAPADE mission is managed by the Space Sciences Laboratory at the University of California, Berkeley, with key partners Rocket Lab, NASA's Goddard Space Flight Center, Embry-Riddle Aeronautical University, Advanced Space LLC, and Blue Origin.Below are animations demonstrating the different phases of the mission's trajectory from traveling from Earth to Mars to implementing its science orbits around the Red Planet. || ", "hits": 590 }, { "id": 14918, "url": "https://svs.gsfc.nasa.gov/14918/", "result_type": "Produced Video", "release_date": "2025-11-11T00:00:00-05:00", "title": "ESCAPADE Prepares for Flight (2025)", "description": "The Escape and Plasma Acceleration and Dynamics Explorers, or ESCAPADE, will use two identical spacecraft to investigate how the solar wind interacts with Mars’ magnetic environment and how this interaction drives the planet’s atmospheric escape. The first multi-spacecraft orbital science mission to the Red Planet, ESCAPADE’s twin orbiters will take simultaneous observations from different locations around Mars to reveal the planet’s real-time response to space weather and how the Martian magnetosphere changes over time.The ESCAPADE mission is being carried into orbit on the second launch of Blue Origin’s New Glenn rocket (NG-2) and is scheduled to launch in November 2025 from Cape Canaveral, Florida. New Glenn is a single-configuration, heavy-lift orbital launch vehicle capable of routinely carrying both spacecraft and people to low Earth orbits, geostationary transfer orbits, cislunar orbits (between Earth and the Moon), and beyond via Earth-departure orbits like the one required for ESCAPADE. The vehicle is named after John Glenn, the first American astronaut to orbit Earth.The ESCAPADE mission is managed by the Space Sciences Laboratory at the University of California, Berkeley, with key partners Rocket Lab, NASA's Goddard Space Flight Center, Embry-Riddle Aeronautical University, Advanced Space LLC, and Blue Origin. || ", "hits": 345 }, { "id": 14898, "url": "https://svs.gsfc.nasa.gov/14898/", "result_type": "Produced Video", "release_date": "2025-09-15T15:00:00-04:00", "title": "Our Home In Space Series", "description": "The heliosphere, the massive bubble created by our Sun, is like our “house” in space. It shelters us from harsh weather outside and regulates the environment inside. Without our heliosphere, Earth may never have developed life at all. But there’s a lot we still don’t know about our cosmic home. How big is it, and what is it shaped like? How does it compare to the “houses” created by other stars? A new NASA mission will soon unlock answers to these questions and more. Launching as early as Sept. 23, NASA’s Interstellar Mapping and Acceleration Probe will help us construct the “blueprints” or our home in space. This three-part series explores how we learn about our heliosphere, how it protects us, and how it advances the search for life elsewhere in the Universe. || ", "hits": 348 }, { "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": 1175 }, { "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": 138 }, { "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": 126 }, { "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": 294 }, { "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": 128 }, { "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": 105 }, { "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": 78 }, { "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": 85 }, { "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": 91 }, { "id": 14739, "url": "https://svs.gsfc.nasa.gov/14739/", "result_type": "Produced Video", "release_date": "2025-01-03T12:00:00-05:00", "title": "From the Moon, NASA’s LEXI Will Reveal Earth’s Magnetic Shield", "description": "NASA’s next mission to the Moon will carry an instrument called LEXI (the Lunar Environment Heliospheric X-ray Imager), which will provide the first-ever global view of the magnetic environment that shields Earth from solar radiation.From the surface of the Moon, LEXI will capture wide-field images of Earth's magnetic environment, or magnetosphere, in low-energy (or \"soft\") X-rays. LEXI will study changes in the magnetosphere and help us learn more about how it interacts with a stream of particles from the Sun called the solar wind, which can pose hazards for Artemis astronauts traveling to the Moon.Learn more about LEXI and its CLPS (Commercial Lunar Payload Services) flight to the Moon from Hyunju Connor, LEXI co-investigator at NASA’s Goddard Space Flight Center.More on LEXI: https://science.nasa.gov/science-research/heliophysics/nasas-lexi-will-provide-x-ray-vision-of-earths-magnetosphere/ || ", "hits": 112 }, { "id": 14664, "url": "https://svs.gsfc.nasa.gov/14664/", "result_type": "Produced Video", "release_date": "2024-08-23T16:00:00-04:00", "title": "ESCAPADE Mission Trailer", "description": "The Escape and Plasma Acceleration and Dynamics Explorers, or ESCAPADE, will use two identical spacecraft to investigate how the solar wind interacts with Mars’ magnetic environment and how this interaction drives the planet’s atmospheric escape.The first coordinated multi-spacecraft orbital science mission to the Red Planet, ESCAPADE’s twin orbiters will take simultaneous observations from different locations around Mars to reveal the planet’s real-time response to space weather and how the Martian magnetosphere changes over time.ESCAPADE will analyze how Mars’ magnetic field guides particle flows around the planet, how energy and momentum are transported from the solar wind through the magnetosphere, and what processes control the flow of energy and matter into and out of the Martian atmosphere. The data returned from the ESCAPADE spacecraft will provide new insight into the evolution of Mars’ climate, contributing to the body of research investigating how Mars began losing its atmosphere and water system.The ESCAPADE mission is managed by the Space Sciences Laboratory at the University of California, Berkeley, with key partners Rocket Lab, NASA's Goddard Space Flight Center, Embry-Riddle Aeronautical University, Advanced Space LLC, and Blue Origin. || ", "hits": 108 }, { "id": 14667, "url": "https://svs.gsfc.nasa.gov/14667/", "result_type": "Produced Video", "release_date": "2024-08-22T14:00:00-04:00", "title": "ESCAPADE Instrument Build and Testing", "description": "The Escape and Plasma Acceleration and Dynamics Explorers, or ESCAPADE, will use two identical spacecraft to investigate how the solar wind interacts with Mars’ magnetic environment and how this interaction drives the planet’s atmospheric escape.The first multi-spacecraft orbital science mission to the Red Planet, ESCAPADE’s twin orbiters will take simultaneous observations from different locations around Mars to reveal the planet’s real-time response to space weather and how the Martian magnetosphere changes over time.ESCAPADE will analyze how Mars’ magnetic field guides particle flows around the planet, how energy and momentum are transported from the solar wind through the magnetosphere, and what processes control the flow of energy and matter into and out of the Martian atmosphere. The data returned from the ESCAPADE spacecraft will provide new insight into the evolution of Mars’ climate, contributing to the body of research investigating how Mars began losing its atmosphere and water system.The ESCAPADE mission is managed by the Space Sciences Laboratory at the University of California, Berkeley, with key partners Rocket Lab, NASA's Goddard Space Flight Center, Embry-Riddle Aeronautical University, Advanced Space LLC, and Blue Origin. || ", "hits": 150 }, { "id": 14665, "url": "https://svs.gsfc.nasa.gov/14665/", "result_type": "Produced Video", "release_date": "2024-08-21T09:00:00-04:00", "title": "ESCAPADE Spacecraft Development Images", "description": "The Escape and Plasma Acceleration and Dynamics Explorers, or ESCAPADE, will use two identical spacecraft to investigate how the solar wind interacts with Mars’ magnetic environment and how this interaction drives the planet’s atmospheric escape.The first coordinated multi-spacecraft orbital science mission to the Red Planet, ESCAPADE’s twin orbiters will take simultaneous observations from different locations around Mars to reveal the planet’s real-time response to space weather and how the Martian magnetosphere changes over time. The data returned from the ESCAPADE spacecraft will provide new insight into the evolution of Mars’ climate, contributing to the body of research investigating how Mars began losing its atmosphere and water system.The ESCAPADE mission is managed by the Space Sciences Laboratory at the University of California, Berkeley, with key partners Rocket Lab, NASA's Goddard Space Flight Center, Embry-Riddle Aeronautical University, Advanced Space LLC, and Blue Origin.The spacecraft were designed, built, integrated, and tested at Rocket Lab’s Spacecraft Production Complex and headquarters in Long Beach, California. Based on Rocket Lab’s Explorer spacecraft, a configurable, high delta-V interplanetary platform, the duo features Rocket Lab-built components and subsystems, including solar panels, star trackers, propellant tanks, reaction wheels, reaction control systems, radios, and more. || ", "hits": 89 }, { "id": 14641, "url": "https://svs.gsfc.nasa.gov/14641/", "result_type": "Infographic", "release_date": "2024-07-30T15:00:00-04:00", "title": "ESCAPADE Mission Posters", "description": "The Escape and Plasma Acceleration and Dynamics Explorers, or ESCAPADE, will use two identical spacecraft to investigate how the solar wind interacts with Mars’ magnetic environment and how this interaction drives the planet’s atmospheric escape.The first coordinated multi-spacecraft orbital science mission to the Red Planet, ESCAPADE’s twin orbiters will take simultaneous observations from different locations around Mars to reveal the planet’s real-time response to space weather and how the Martian magnetosphere changes over time.ESCAPADE will analyze how Mars’ magnetic field guides particle flows around the planet, how energy and momentum are transported from the solar wind through the magnetosphere, and what processes control the flow of energy and matter into and out of the Martian atmosphere. The data returned from the ESCAPADE spacecraft will provide new insight into the evolution of Mars’ climate, contributing to the body of research investigating how Mars began losing its atmosphere and water system.The ESCAPADE mission is managed by the Space Sciences Laboratory at the University of California, Berkeley, with key partners Rocket Lab, NASA's Goddard Space Flight Center, Embry-Riddle Aeronautical University, Advanced Space LLC, and Blue Origin. || ", "hits": 84 }, { "id": 14642, "url": "https://svs.gsfc.nasa.gov/14642/", "result_type": "Infographic", "release_date": "2024-07-30T15:00:00-04:00", "title": "ESCAPADE Spacecraft Specifications", "description": "The Escape and Plasma Acceleration and Dynamics Explorers (ESCAPADE) mission, led by Rob Lillis at the University of California, Berkeley, Space Sciences Laboratory (UCBSSL), is a twin-spacecraft science mission that will orbit two spacecraft around Mars to understand the structure, composition, variability, and dynamics of Mars' unique hybrid magnetosphere. The mission will leverage its unique dual viewpoint on the Mars environment to explore how the solar wind strips atmosphere away from Mars to better understand how its climate has changed over time. ESCAPADE is being developed under NASA’s Small Innovative Missions for Planetary Exploration (SIMPLEx) program in the Science Mission Directorate (SMD). The mission is led by UCBSSL with spacecraft design provided by Rocket Lab.The spacecraft were designed, built, integrated, and tested at Rocket Lab’s Spacecraft Production Complex and headquarters in Long Beach, California. Based on Rocket Lab’s Explorer spacecraft, a configurable, high delta-V interplanetary platform, the duo features Rocket Lab-built components and subsystems, including solar panels, star trackers, propellant tanks, reaction wheels, reaction control systems, radios, and more. || ", "hits": 229 }, { "id": 14635, "url": "https://svs.gsfc.nasa.gov/14635/", "result_type": "Produced Video", "release_date": "2024-07-22T12:00:00-04:00", "title": "ESCAPADE Mission Spacecraft Beauty Passes", "description": "NASA’s Escape and Plasma Acceleration and Dynamics Explorers (ESCAPADE) mission will study the interaction between the solar wind and Martian atmosphere. Two identical spacecraft will orbit around the Red Planet to understand the structure, composition, variability, and dynamics of Mars’ unique hybrid magnetosphere, including its real-time response to space weather.The mission will leverage its unique dual viewpoint on the Mars environment to explore how the solar wind strips atmosphere away from Mars to better understand how its climate has changed over time — so much that Mars no longer supports liquid water on its surface. The pair will be the first coordinated multi-spacecraft orbital science mission to Mars.ESCAPADE is part of the NASA Small Innovative Missions for Planetary Exploration (SIMPLEx) program. The mission is managed by the University of California Berkeley’s Space Sciences Laboratory, with key partners Rocket Lab, NASA Goddard Space Flight Center, Embry-Riddle Aeronautical University, Advanced Space LLC, and Blue Origin. || ", "hits": 128 }, { "id": 14542, "url": "https://svs.gsfc.nasa.gov/14542/", "result_type": "Produced Video", "release_date": "2024-03-05T10:00:00-05:00", "title": "Electrojet Zeeman Imaging Explorer (EZIE)", "description": "Slated to launch in 2025, NASA’s Electrojet Zeeman Imaging Explorer (EZIE) will be the first mission to image the magnetic fingerprint of the auroral electrojets — intense electric currents flowing high above Earth’s poles that are central to the electrical circuit coupling the planet’s magnetosphere to its atmosphere.Led by the Johns Hopkins Applied Physics Laboratory (APL), EZIE will use a trio of small satellites to characterize and record the electrojets’ structure over space and time. It will fill gaps in our understanding of this space weather phenomenon and provide findings that scientists can apply to other magnetized planets, both within and outside our solar system. || ", "hits": 176 }, { "id": 14204, "url": "https://svs.gsfc.nasa.gov/14204/", "result_type": "Produced Video", "release_date": "2022-08-31T09:00:00-04:00", "title": "Mars Patchy Proton Aurora", "description": "NASA’s MAVEN (Mars Atmosphere and Volatile Evolution) mission and the United Arab Emirates’ Emirates Mars Mission (EMM) have released joint observations of dynamic proton aurora events at Mars. Remote auroral observations by EMM paired with in-situ plasma observations made by MAVEN open new avenues for understanding the Martian atmosphere. This collaboration was made possible by recent data-sharing between the two missions and highlights the value of multi-point observations in space.Learn more about this discovery by MAVEN and EMM. || ", "hits": 89 }, { "id": 14148, "url": "https://svs.gsfc.nasa.gov/14148/", "result_type": "Produced Video", "release_date": "2022-05-05T12:45:00-04:00", "title": "Magnetic Flip Drives Flare-Up of Monster Black Hole", "description": "Explore the unusual eruption of 1ES 1927+654, a galaxy located 236 million light-years away in the constellation Draco. A sudden reversal of the magnetic field around its million-solar-mass black hole may have triggered the outburst.Credit: NASA’s Goddard Space Flight Center Music: \"Water Dance\" and \"Alternate Worlds\" from Universal Production MusicWatch this video on the NASA Goddard YouTube channel.Complete transcript available. || ChangingLookAGN_Still1.jpg (1920x1080) [822.9 KB] || ChangingLookAGN_Still1_searchweb.png (320x180) [79.5 KB] || ChangingLookAGN_Still1_thm.png (80x40) [6.2 KB] || 14148_ChangingLook_AGN_1080.webm (1920x1080) [24.8 MB] || 14148_ChangingLook_AGN_Sub100MB.mp4 (1920x1080) [91.5 MB] || 14148_ChangingLook_AGN_1080.mp4 (1920x1080) [246.5 MB] || 14148_ChangingLook_AGN_Best_1080.mp4 (1920x1080) [534.7 MB] || 14148_ChangingLook_AGN_SRT_Captions.en_US.srt [4.2 KB] || 14148_ChangingLook_AGN_SRT_Captions.en_US.vtt [4.3 KB] || 14148_ChangingLook_AGN_ProRes_1920x1080_2997.mov (1920x1080) [3.2 GB] || ", "hits": 105 }, { "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": 146 }, { "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": 1120 }, { "id": 4730, "url": "https://svs.gsfc.nasa.gov/4730/", "result_type": "Visualization", "release_date": "2020-05-25T11:00:00-04:00", "title": "MAVEN – Mars Electric Current Systems", "description": "The current systems formed around Mars as a result of a solar wind driven convective electric field(Note: These frame sets were converted to the sRGB color space on 6/16/2020)This video is also available on our YouTube channel. || ideal_currents_1080.00600_print.jpg (1024x576) [71.1 KB] || ideal_currents_1080.00600_searchweb.png (320x180) [21.7 KB] || ideal_currents_1080.00600_thm.png (80x40) [2.0 KB] || ideal_currents_1080p30.mp4 (1920x1080) [74.0 MB] || ideal_currents_1080.webm (1920x1080) [9.9 MB] || ideal_curr (1920x1080) [0 Item(s)] || ideal_curr (3840x2160) [0 Item(s)] || captions_silent.25991.en_US.srt [43 bytes] || ideal_currents_4k_2160p30.mp4 (3840x2160) [170.1 MB] || idealized_currents_prores.mov (1920x1080) [2.9 GB] || Mars_idealized_currents_4k_prores.mov (3840x2160) [3.5 GB] || ideal_currents_1080p30.mp4.hwshow || ", "hits": 74 }, { "id": 13625, "url": "https://svs.gsfc.nasa.gov/13625/", "result_type": "Produced Video", "release_date": "2020-05-25T11:00:00-04:00", "title": "First Map of Mars Electric Currents", "description": "MAVEN data have enabled the first map of the electric current systems (blue and red arrows) that shape the induced magnetic field surrounding Mars.Credit: NASA/Goddard/MAVEN/CU Boulder/SVSUniversal Production Music: “A Lucid Dream” and “Shimmer Oscillations” by James Joshua OttoWatch this video on the NASA Goddard YouTube channel.Complete transcript available. || MarsElectricCurrentsPreview6_print.jpg (1024x576) [305.8 KB] || MarsElectricCurrentsPreview6.jpg (1920x1080) [853.6 KB] || MarsElectricCurrentsPreview6_searchweb.png (320x180) [50.6 KB] || MarsElectricCurrentsPreview6_thm.png (80x40) [5.3 KB] || 13625_Mars_Electric_Currents_Twitter.mp4 (1280x720) [63.8 MB] || 13625_Mars_Electric_Currents_Facebook.mp4 (1920x1080) [359.1 MB] || 13625_Mars_Electric_Currents_YouTube.webm (3840x2160) [91.7 MB] || 13625_Mars_Electric_Currents_Captions.en_US.srt [7.2 KB] || 13625_Mars_Electric_Currents_Captions.en_US.vtt [6.8 KB] || 13625_Mars_Electric_Currents_YouTube.mp4 (3840x2160) [2.8 GB] || 13625_Mars_Electric_Currents_MASTER.mov (3840x2160) [14.2 GB] || 13625_Mars_Electric_Currents_Facebook.mp4.hwshow [134 bytes] || ", "hits": 85 }, { "id": 4824, "url": "https://svs.gsfc.nasa.gov/4824/", "result_type": "Visualization", "release_date": "2020-05-25T00:00:00-04:00", "title": "MAVEN Observes Solar Particle Velocities and the Induced Magnetic Field", "description": "MAVEN orbits Mars and measures solar particle velocities and variations in the solar wind’s magnetic field. || maven_vels_magField.03000_print.jpg (1024x576) [92.5 KB] || maven_vels_magField.03000_searchweb.png (320x180) [63.5 KB] || maven_vels_magField.03000_thm.png (80x40) [4.2 KB] || maven_vels_magField_1080p30.mp4 (1920x1080) [83.1 MB] || 1920x1080_16x9_30p 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"release_date": "2020-02-10T00:00:00-05:00", "title": "Solar Orbiter: Preguntas más frecuentes", "description": "Música: Carrier of Life, de Joe BennieAnimación de naves espaciales: ESA / ATG MedialabMira este vídeo en el canal de YouTube de la NASA en español..La transcripción completa || SolO.Es.00250_print.jpg (1024x576) [68.8 KB] || SolO.Es.00250_searchweb.png (320x180) [76.7 KB] || SolO.Es.00250_thm.png (80x40) [5.8 KB] || SolO.Es.mov (1920x1080) [6.8 GB] || SolO.Es_questions.mp4 (1920x1080) [258.4 MB] || SolO.Es.webm (1920x1080) [30.7 MB] || ", "hits": 25 }, { "id": 13509, "url": "https://svs.gsfc.nasa.gov/13509/", "result_type": "Produced Video", "release_date": "2020-02-04T11:00:00-05:00", "title": "Solar Orbiter Trailer - Videos in English and Spanish", "description": "Music: Find Her by Yuri SazonoffAnimation by ESA/ATG MedialabWatch this video on the NASA Goddard YouTube channel.Complete transcript available. || SolO_Trailer.00_00_48_09.Still001.jpg (1920x1080) [760.6 KB] || SolO_Trailer.00_00_48_09.Still001_searchweb.png (180x320) [123.9 KB] || SolO_Trailer.00_00_48_09.Still001_thm.png (80x40) [8.2 KB] || SolO_Trailer_EnglishV2.mov (1920x1080) [819.6 MB] || SolO_Trailer_EnglishV2.mp4 (1920x1080) [88.9 MB] || SolO_Trailer_EnglishV2.webm (1920x1080) [10.0 MB] || SolO_Trailer_EnglishV2Transcripts.en_US.srt [237 bytes] || SolO_Trailer_EnglishV2Transcripts.en_US.vtt [249 bytes] || ", "hits": 52 }, { "id": 20306, "url": "https://svs.gsfc.nasa.gov/20306/", "result_type": "Animation", "release_date": "2020-01-27T14:00:00-05:00", "title": "Solar Orbiter - NASA Animations", "description": "Solar Orbiter is an international cooperative mission between the European Space Agency and NASA that addresses a central question of heliophysics: How does the Sun create and control the constantly changing space environment throughout the solar system? The Sun creates what’s known as the heliosphere — a giant bubble of charged particles and magnetic fields blown outward by the Sun that stretches more than twice the distance to Pluto at its nearest edge, enveloping every planet in our solar system and shaping the space around us. To understand it, Solar Orbiter will travel as close as 26 million miles from the Sun, inside the orbit of Mercury. There, it will measure the magnetic fields, waves, energetic particles and plasma escaping the Sun while they are in their pristine state, before being modified and mixed in their long journey from the Sun. || ", "hits": 96 }, { "id": 13514, "url": "https://svs.gsfc.nasa.gov/13514/", "result_type": "Produced Video", "release_date": "2019-12-20T17:00:00-05:00", "title": "The Cusp Aurora", "description": "A conceptual animation showing electrons traveling down Earth's magnetic field lines, colliding into oxygen atoms in Earth's atmosphere and causing oxygen molecules to escape and release red light causing the cusp aurora. || YOUTUBE_1080_13514_Cusp_Aurora_from_ground_youtube_1080.00888_print.jpg (1024x576) [70.9 KB] || YOUTUBE_1080_13514_Cusp_Aurora_from_ground_youtube_1080.00888_searchweb.png (320x180) [64.8 KB] || YOUTUBE_1080_13514_Cusp_Aurora_from_ground_youtube_1080.00888_web.png (320x180) [64.8 KB] || YOUTUBE_1080_13514_Cusp_Aurora_from_ground_youtube_1080.00888_thm.png (80x40) [4.4 KB] || FACEBOOK_720_13514_Cusp_Aurora_from_ground_facebook_720.mp4 (1280x720) [49.5 MB] || TWITTER_720_13514_Cusp_Aurora_from_ground_twitter_720.mp4 (1280x720) [8.0 MB] || YOUTUBE_1080_13514_Cusp_Aurora_from_ground_youtube_1080.webm (1920x1080) [4.9 MB] || YOUTUBE_1080_13514_Cusp_Aurora_from_ground_youtube_1080.mp4 (1920x1080) [64.2 MB] || PRORES_B-ROLL_13514_Cusp_Aurora_from_ground_prores_b-roll.mov (1280x720) [346.4 MB] || YOUTUBE_4K_13514_Cusp_Aurora_from_ground_youtube_4k.mp4 (3840x2160) [285.2 MB] || 13514_Cusp_Aurora_from_ground_Prores.mov (3840x2160) [3.9 GB] || ", "hits": 72 }, { "id": 13422, "url": "https://svs.gsfc.nasa.gov/13422/", "result_type": "Produced Video", "release_date": "2019-12-17T10:00:00-05:00", "title": "A New Kind of Explosion on the Sun", "description": "Complete transcript available.Watch this video on the NASA Goddard YouTube channel.Music Credit: Light Hearted Angst by Dewey Dellay || ReconnThumb.jpg (1920x1080) [156.1 KB] || ReconnThumb_searchweb.png (320x180) [100.6 KB] || ReconnThumb_thm.png (80x40) [7.3 KB] || ForcedReconnV2_Twitter.mp4 (1920x1080) [29.6 MB] || ForcedReconnV2.webm (1920x1080) [14.8 MB] || ForcedReconnV2.mp4 (1920x1080) [134.9 MB] || ForcedReconnV2_FB.mp4 (1920x1080) [155.5 MB] || ForcedReconnV2_YouTube.mp4 (1920x1080) [207.3 MB] || ForcedReconnV2.en_US.srt [2.6 KB] || ForcedReconnV2.en_US.vtt [2.6 KB] || ForcedReconnV2.mov (1920x1080) [1.7 GB] || ", "hits": 79 }, { "id": 12589, "url": "https://svs.gsfc.nasa.gov/12589/", "result_type": "Produced Video", "release_date": "2019-06-10T10:00:00-04:00", "title": "Getting SET - The Mission to Protect Satellites from Radiation", "description": "SET is the latest addition to NASA’s fleet of heliophysics observatories. NASA heliophysics missions study a vast interconnected system from the Sun to the space surrounding Earth and other planets, and to the farthest limits of the Sun’s constantly flowing stream of solar wind. SET’s observations provide key information on the Sun’s effects on our spacecraft, enabling further exploration of space. Watch this video on the NASA Goddard YouTube channel.Complete transcript available.Music credits: Night Moves by Max Cameron Concors, Wavelengths by Max Cameron Concors, and Alpha Helix by David Travis Edwards, Robert Anthony Navarro, Matthew St Laurent, and Christian Telford. End tag music credits: Radiant Energy by Chris Constantinou, Paul Frazer || SETThumb.jpg (1920x1080) [191.0 KB] || SETThumb_searchweb.png (320x180) [79.4 KB] || SETThumb_thm.png (80x40) [6.2 KB] || 12589_SET.V3.webm (1920x1080) [31.1 MB] || captions.en_US.srt [4.4 KB] || captions.en_US.vtt [4.2 KB] || 12589_SET.en_US.srt [4.2 KB] || 12589_SET.en_US.vtt [4.2 KB] || 12589_SET.V3.mov (1920x1080) [5.5 GB] || 12589_SET.V3.mp4 (1920x1080) [206.9 MB] || 12589_SET.V3FB1080.mp4 (1920x1080) [241.6 MB] || ", "hits": 54 }, { "id": 4620, "url": "https://svs.gsfc.nasa.gov/4620/", "result_type": "Visualization", "release_date": "2019-02-27T15:30:00-05:00", "title": "Magnetic Bubbles on the Moon...", "description": "View of 'deluxe' model with camera in fixed position. Fades from schematic view showing underground dipole field sources (blue and yellow arrows), induced electric field (red arrows) and magnetic field (gold curves) to a view with Reiner Gamma region of moon. Solar protons (blue) rain down on lunar surface with enhanced accumulation near dipoles. || SolarWindRain.dipole.Efield_fixed_inertial.HD1080i.1000_print.jpg (1024x576) [163.4 KB] || SolarWindRain.dipole.Efield_fixed_inertial.HD1080i.1000_searchweb.png (320x180) [101.6 KB] || SolarWindRain.dipole.Efield_fixed_inertial.HD1080i.1000_thm.png (80x40) [6.9 KB] || VizEDFixedCamera (1920x1080) [0 Item(s)] || SolarWindRain.dipole.Efield_fixed.HD1080i_p30.webm (1920x1080) [7.5 MB] || SolarWindRain.dipole.Efield_fixed.HD1080i_p30.mp4 (1920x1080) [97.0 MB] || VizEDFixedCamera (3840x2160) [0 Item(s)] || SolarWindRain.dipole.Efield_fixed_2160p30.mp4 (3840x2160) [270.4 MB] || SolarWindRain.dipole.Efield_fixed.HD1080i_p30.mp4.hwshow [211 bytes] || ", "hits": 53 }, { "id": 13150, "url": "https://svs.gsfc.nasa.gov/13150/", "result_type": "Produced Video", "release_date": "2019-02-27T15:30:00-05:00", "title": "Magnetic Bubbles on the Moon Reveal Evidence of \"Sunburn\"", "description": "Research using data from NASA's ARTEMIS mission suggests that lunar swirls, like the Reiner Gamma lunar swirl imaged here by NASA's Lunar Reconnaissance Orbiter, could be the result of solar wind interactions with the Moon's isolated pockets of magnetic field. Watch this video on the NASA Goddard YouTube channel.Complete transcript available.Music credit: Genetic Spices by Jean Christophe Lemay || swirls.jpg (1920x1080) [514.5 KB] || swirls_searchweb.png (320x180) [90.4 KB] || swirls_thm.png (80x40) [6.3 KB] || 12589_MoonBubbles_GSFC.ENDTAG.mp4 (1920x1080) [140.8 MB] || 12589_MoonBubbles_GSFC.ENDTAG.mov (1920x1080) [1.9 GB] || 12589_MoonBubbles_GSFC.ENDTAG_FB.mp4 (1920x1080) [166.4 MB] || 12589_MoonBubbles_GSFC.ENDTAG_YouTube.mp4 (1920x1080) [222.2 MB] || 12589_MoonBubbles_GSFC.ENDTAG.webm (1920x1080) [15.0 MB] || 12589_MoonBubbles_GSFC.en_US.srt [2.8 KB] || 12589_MoonBubbles_GSFC.en_US.vtt [2.8 KB] || ", "hits": 75 }, { "id": 4637, "url": "https://svs.gsfc.nasa.gov/4637/", "result_type": "Visualization", "release_date": "2018-10-10T11:00:00-04:00", "title": "Pulsars and their Magnetic Field - Vacuum solution", "description": "This movie presents a basic tour around the vacuum magnetic field solution. This version is generated with some simple reference objects for more general use. || BasicPulsarDipole_tour_inertial.HD1080i.01001_print.jpg (1024x576) [51.0 KB] || tour-glyph (1920x1080) [0 Item(s)] || BasicPulsarDipole_tour_glyph.HD1080i_p30.mp4 (1920x1080) [29.3 MB] || BasicPulsarDipole_tour_glyph.HD1080i_p30.webm (1920x1080) [4.3 MB] || tour-glyph (3840x2160) [0 Item(s)] || BasicPulsarDipole_tour_glyph_2160p30.mp4 (3840x2160) [67.0 MB] || BasicPulsarDipole_tour_glyph.HD1080i_p30.mp4.hwshow [206 bytes] || ", "hits": 96 }, { "id": 4638, "url": "https://svs.gsfc.nasa.gov/4638/", "result_type": "Visualization", "release_date": "2018-10-10T11:00:00-04:00", "title": "Pulsar Current Sheets - Magnetic Field Solution", "description": "This movie presents a basic tour around the simulation magnetic field. This version is generated with some simple reference objects for more general use. || PulsarParticles_grid_tour_inertial.HD1080i.01001_print.jpg (1024x576) [49.5 KB] || tour-glyph (1920x1080) [0 Item(s)] || PulsarParticles_grid_tour_inertial.HD1080i_p30.mp4 (1920x1080) [22.6 MB] || PulsarParticles_grid_tour_inertial.HD1080i_p30.webm (1920x1080) [4.3 MB] || tour-glyph (3840x2160) [0 Item(s)] || PulsarParticles_grid_tour_2160p30.mp4 (3840x2160) [66.2 MB] || PulsarParticles_grid_tour_inertial.HD1080i_p30.mp4.hwshow [212 bytes] || ", "hits": 47 }, { "id": 4644, "url": "https://svs.gsfc.nasa.gov/4644/", "result_type": "Visualization", "release_date": "2018-10-10T11:00:00-04:00", "title": "Pulsar Current Sheets - Bulk Particle Trajectories", "description": "This movie presents a basic tour around the simulation magnetic field including motion of the bulk particles. This version is generated with some simple reference objects for more general use. || PulsarParticles_grid_bulk_tour_inertial.HD1080i.01001_print.jpg (1024x576) [112.0 KB] || tour-glyph (1920x1080) [0 Item(s)] || PulsarParticles_grid_bulk_tour.HD1080i_p30.mp4 (1920x1080) [67.7 MB] || PulsarParticles_grid_bulk_tour.HD1080i_p30.webm (1920x1080) [5.3 MB] || tour-glyph (3840x2160) [0 Item(s)] || PulsarParticles_grid_bulk_tour_2160p30.mp4 (3840x2160) [129.1 MB] || PulsarParticles_grid_bulk_tour.HD1080i_p30.mp4.hwshow [208 bytes] || ", "hits": 56 }, { "id": 4645, "url": "https://svs.gsfc.nasa.gov/4645/", "result_type": "Visualization", "release_date": "2018-10-10T11:00:00-04:00", "title": "Pulsar Current Sheets - Electron flows", "description": "This movie presents a basic tour around the simulation magnetic field including motion of the high-energy electrons. This version is generated with some simple reference objects for more general use. || PulsarParticles_grid_electrons_tour_inertial.HD1080i.01001_print.jpg (1024x576) [100.3 KB] || tour-glyph (1920x1080) [0 Item(s)] || PulsarParticles_grid_electrons_tour.HD1080i_p30.mp4 (1920x1080) [78.4 MB] || PulsarParticles_grid_electrons_tour.HD1080i_p30.webm (1920x1080) [5.4 MB] || tour-glyph (3840x2160) [0 Item(s)] || PulsarParticles_grid_electrons_tour_2160p30.mp4 (3840x2160) [187.4 MB] || PulsarParticles_grid_electrons_tour.HD1080i_p30.mp4.hwshow [213 bytes] || ", "hits": 39 }, { "id": 4646, "url": "https://svs.gsfc.nasa.gov/4646/", "result_type": "Visualization", "release_date": "2018-10-10T11:00:00-04:00", "title": "Pulsar Current Sheets - Positron Flows", "description": "This movie presents a basic tour around the simulation magnetic field including motion of the high-energy positrons. This version is generated with some simple reference objects for more general use. || PulsarParticles_grid_positrons_tour_inertial.HD1080i.01001_print.jpg (1024x576) [114.9 KB] || tour-glyph (1920x1080) [0 Item(s)] || PulsarParticles_grid_positrons_tour.HD1080i_p30.mp4 (1920x1080) [82.8 MB] || PulsarParticles_grid_positrons_tour.HD1080i_p30.webm (1920x1080) [7.9 MB] || tour-glyph (3840x2160) [0 Item(s)] || PulsarParticles_grid_positrons_tour_2160p30.mp4 (3840x2160) [198.5 MB] || PulsarParticles_grid_positrons_tour.HD1080i_p30.mp4.hwshow [213 bytes] || ", "hits": 126 }, { "id": 4647, "url": "https://svs.gsfc.nasa.gov/4647/", "result_type": "Visualization", "release_date": "2018-10-10T11:00:00-04:00", "title": "Pulsar Current Sheets - Electron & Positron Flows", "description": "This movie presents a basic tour around the simulation magnetic field including motion of the high-energy electrons and positrons. This version is generated with some simple reference objects for more general use. || PulsarParticles_grid_positrons_electrons_tour_inertial.HD1080i.01001_print.jpg (1024x576) [142.4 KB] || tour-glyph (1920x1080) [0 Item(s)] || PulsarParticles_grid_positrons_electrons_tour.HD1080i_p30.webm (1920x1080) [8.7 MB] || PulsarParticles_grid_positrons_electrons_tour.HD1080i_p30.mp4 (1920x1080) [121.5 MB] || tour-glyph (3840x2160) [0 Item(s)] || PulsarParticles_grid_positrons_electrons_tour_2160p30.mp4 (3840x2160) [302.5 MB] || PulsarParticles_grid_positrons_electrons_tour.HD1080i_p30.mp4.hwshow [223 bytes] || ", "hits": 46 }, { "id": 4648, "url": "https://svs.gsfc.nasa.gov/4648/", "result_type": "Visualization", "release_date": "2018-10-10T11:00:00-04:00", "title": "Pulsar Current Sheets - All Particle Flows", "description": "This movie presents a basic tour around the simulation magnetic field including motion of the the bulk particles and high-energy electrons and positrons. This version is generated with some simple reference objects for more general use. || PulsarParticles_grid_bulk_positrons_electrons_tour_inertial.HD1080i.01001_print.jpg (1024x576) [172.3 KB] || tour-glyph (1920x1080) [0 Item(s)] || PulsarParticles_grid_bulk_positrons_electrons_tour.HD1080i_p30.webm (1920x1080) [9.4 MB] || PulsarParticles_grid_bulk_positrons_electrons_tour.HD1080i_p30.mp4 (1920x1080) [148.0 MB] || tour-glyph (3840x2160) [0 Item(s)] || PulsarParticles_grid_bulk_positrons_electrons_tour_2160p30.mp4 (3840x2160) [375.4 MB] || PulsarParticles_grid_bulk_positrons_electrons_tour.HD1080i_p30.mp4.hwshow [228 bytes] || ", "hits": 98 }, { "id": 13076, "url": "https://svs.gsfc.nasa.gov/13076/", "result_type": "Produced Video", "release_date": "2018-09-24T16:00:00-04:00", "title": "Grand Challenge-Cusp Graphics", "description": "GraphicNorth of Norway over the Norwegian and Greenland Seas, a magnetic bubble, known as the cusp, surrounds Earth and dips inward, allowing space particles to funnel in toward the planet.Credit: Andøya Space Center/Trond Abrahamsen || asc-earth-magnetosphere-to-scale_print.jpg (1024x619) [138.1 KB] || asc-earth-magnetosphere-to-scale.jpeg (5352x3240) [13.0 MB] || asc-earth-magnetosphere-to-scale_searchweb.png (320x180) [67.0 KB] || asc-earth-magnetosphere-to-scale_web.png (320x193) [71.7 KB] || asc-earth-magnetosphere-to-scale_thm.png (80x40) [4.3 KB] || ", "hits": 36 }, { "id": 4649, "url": "https://svs.gsfc.nasa.gov/4649/", "result_type": "Visualization", "release_date": "2018-05-29T10:00:00-04:00", "title": "Plasma Zoo: Gyroresonant Scattering", "description": "In a background magnetic field, represented by the cyan arrows, two electrons are propagating to the right, executing identical gyromotion. 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Watch this video on the NASA.gov Video YouTube channel. || JupiterMagneticTourSmall.mp4 (1920x1080) [71.9 MB] || JupiterMagneticTourPreview.jpg (3840x2160) [1.2 MB] || JupiterMagneticTourPreview_searchweb.png (320x180) [57.0 KB] || JupiterMagneticTourPreview_thm.png (80x40) [3.5 KB] || JupiterMagneticTourProRes.webm (960x540) [28.4 MB] || JupiterMagneticTour1080.mp4 (1920x1080) [193.9 MB] || Foreground_Jupiter_Frames (3840x2160) [0 Item(s)] || Background_Star_Frames (3840x2160) [0 Item(s)] || JupiterMagneticTour4k.mp4 (3840x2160) [492.1 MB] || JupiterMagneticTourProRes.mov (3840x2160) [4.1 GB] || ", "hits": 274 }, { "id": 4228, "url": "https://svs.gsfc.nasa.gov/4228/", "result_type": "Visualization", "release_date": "2017-08-11T10:00:00-04:00", "title": "The Little Flux Rope that Couldn't", "description": "HD1080 version of full disk SDO imagery in the 131 Angstrom filter. || Sept2014_FluxRope_stand.HD1080i.00400_print.jpg (1024x576) [50.9 KB] || Sept2014_FluxRope_stand.HD1080i.00400_searchweb.png (320x180) [29.8 KB] || Sept2014_FluxRope_stand.HD1080i.00400_thm.png (80x40) [2.6 KB] || 1920x1080_16x9_30p (1920x1080) [0 Item(s)] || Sept2014_FluxRope.HD1080i_p30.mp4 (1920x1080) [15.8 MB] || Sept2014_FluxRope.HD1080i_p30.webm (1920x1080) [3.3 MB] || Sept2014_FluxRope.HD1080i_p30.mp4.hwshow [195 bytes] || ", "hits": 29 }, { "id": 4568, "url": "https://svs.gsfc.nasa.gov/4568/", "result_type": "Visualization", "release_date": "2017-05-18T10:00:00-04:00", "title": "Exploring Reconnection - Guide Field Off", "description": "This visualization shows an oblique view of the reconnection region. Magnetic field direction is represented by the cyan lines. The color trail represents an electron moving in the field. Color of the particle trail represents a dimensionless speed of the particle, with blue for slow and red for fast. || GuideFieldOff_oblique_inertial.HD1080i.0300_print.jpg (1024x576) [118.2 KB] || GuideFieldOff_oblique_inertial.HD1080i.0300_searchweb.png (320x180) [70.8 KB] || GuideFieldOff_oblique_inertial.HD1080i.0300_thm.png (80x40) [4.4 KB] || GuideFieldOff_oblique (1920x1080) [0 Item(s)] || GuideFieldOff_oblique_inertial.HD1080i_p30.mp4 (1920x1080) [6.3 MB] || GuideFieldOff_oblique_inertial.HD1080i_p30.webm (1920x1080) [776.5 KB] || GuideFieldOff_oblique_inertial.HD1080i_p30.mp4.hwshow [208 bytes] || ", "hits": 59 }, { "id": 4569, "url": "https://svs.gsfc.nasa.gov/4569/", "result_type": "Visualization", "release_date": "2017-05-18T10:00:00-04:00", "title": "Exploring Reconnection - Guide Field On", "description": "This visualization shows an oblique view of the reconnection region. Magnetic field direction is represented by the cyan lines. The color trail represents an electron moving in the field. Color of the particle trail represents a dimensionless speed of the particle, with blue for slow and red for fast. || GuideFieldOn_oblique_inertial.HD1080i.0300_print.jpg (1024x576) [129.7 KB] || GuideFieldOn_oblique_inertial.HD1080i.0300_searchweb.png (320x180) [76.2 KB] || GuideFieldOn_oblique_inertial.HD1080i.0300_thm.png (80x40) [4.6 KB] || GuideFieldOn_oblique (1920x1080) [0 Item(s)] || GuideFieldOn_oblique.HD1080i_p30.mp4 (1920x1080) [6.5 MB] || GuideFieldOn_oblique.HD1080i_p30.webm (1920x1080) [761.3 KB] || GuideFieldOn_oblique.HD1080i_p30.mp4.hwshow [198 bytes] || ", "hits": 113 }, { "id": 12588, "url": "https://svs.gsfc.nasa.gov/12588/", "result_type": "Produced Video", "release_date": "2017-04-26T13:00:00-04:00", "title": "A Solar Eruption in 5 Steps", "description": "Music credit: Prism Mystery by Donn WilkersonComplete transcript available.Watch this video on the NASA Goddard YouTube channel. || filament.thumb.jpg (1920x1080) [239.3 KB] || filament.thumb_print.jpg (1024x576) [176.5 KB] || filament.thumb_searchweb.png (320x180) [106.4 KB] || filament.thumb_web.png (320x180) [106.4 KB] || filament.thumb_thm.png (80x40) [7.0 KB] || 12588_Mechanisms_for_Solar_EruptionsV4.mov (1920x1080) [3.2 GB] || 12588_Mechanisms_for_Solar_EruptionsV4.webm (1920x1080) [10.2 MB] || 12588MechanismsforSolarEruptionsV4_VX-281901_appletv.m4v (1280x720) [63.8 MB] || 12588MechanismsforSolarEruptionsV4_VX-281901_large.mp4 (1920x1080) [114.5 MB] || 12588MechanismsforSolarEruptionsV4_VX-281901_youtube_hq.mov (1920x1080) [244.4 MB] || 12588MechanismsforSolarEruptionsV4_VX-281901_appletv_subtitles.m4v (1280x720) [63.8 MB] || 12588_Mechanisms_for_Solar_EruptionsV4.en_US.srt [1.2 KB] || 12588_Mechanisms_for_Solar_EruptionsV4.en_US.vtt [1.2 KB] || 12588MechanismsforSolarEruptionsV4_VX-281901_ipod_sm.mp4 (320x240) [17.5 MB] || ", "hits": 32 }, { "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": 271 }, { "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": 327 }, { "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": 109 }, { "id": 12296, "url": "https://svs.gsfc.nasa.gov/12296/", "result_type": "Produced Video", "release_date": "2016-06-29T09:00:00-04:00", "title": "Exploring Jupiter's Magnetic Field", "description": "NASA is sending the Juno spacecraft to peer beneath the cloudy surface of Jupiter. Juno's twin magnetometers, built at Goddard Space Flight Center, will give scientists their first look at the dynamo that drives Jupiter's vast magnetic field. Watch this video on the NASA Goddard YouTube channel.Complete transcript available. || JupiterMagnetometerPreview.jpg (1920x1080) [591.9 KB] || JupiterMagnetometerPreview_searchweb.png (320x180) [118.7 KB] || JupiterMagnetometerPreview_thm.png (80x40) [8.0 KB] || 12296_Juno_Magnetometer_appletv.m4v (1280x720) [159.8 MB] || WEBM_12296_Juno_Magnetometer_APR.webm (960x540) [124.4 MB] || 12296_Juno_Magnetometer_appletv_subtitles.m4v (1280x720) [159.9 MB] || LARGE_MP4_12296_Juno_Magnetometer_APR_large.mp4 (1920x1080) [311.4 MB] || 12296_Juno_Magnetometer_APR_Output.en_US.srt [6.2 KB] || 12296_Juno_Magnetometer_APR_Output.en_US.vtt [6.2 KB] || 12296_Juno_Magnetometer_ipod_sm.mp4 (320x240) [53.1 MB] || 12296_Juno_Magnetometer_APR.mov (1920x1080) [4.1 GB] || ", "hits": 183 }, { "id": 4469, "url": "https://svs.gsfc.nasa.gov/4469/", "result_type": "Visualization", "release_date": "2016-06-16T15:00:00-04:00", "title": "Dynamic Earth-A New Beginning", "description": "The visualization 'Excerpt from \"Dynamic Earth\"' has been one of the most popular visualizations that the Scientific Visualization Studio has ever created. It's often used in presentations and Hyperwall shows to illustrate the connections between the Earth and the Sun, as well as the power of computer simulation in understanding those connections.There is one part of this visualization, however, that has always seemed a little clumsy to us. The opening shot is a pullback from the limb of the sun, where the sun is represented by a movie of 304 Angstrom images from the Solar Dynamics Observatory (SDO). It is difficult to pull back from the limb of a flat sun image and make the sun look spherical, and the problem was made more difficult because the original sun images were in a spherical dome show format. As a result, the pullback from the sun showed some odd reprojection artifacts.The best solution to this issue was to replace the existing pullout with a new one, one which pulled directly out from the center of the solar disk. For the new beginning, we chose a series of SDO images in the 171 Angstrom channel that show a visible coronal mass ejection (CME) in the lower right corner of the solar disk. Although this is not the specific CME that is seen affecting Venus and Earth later in this visualization, its presence links the SDO animation thematically to the later solar storm. The SDO images were also brightened considerably and tinted yellow to match the common perception of the Sun as a bright yellow object (even though it is actually white).Please go to the original version of this visualization to see the complete credits and additional details. || ", "hits": 62 }, { "id": 11853, "url": "https://svs.gsfc.nasa.gov/11853/", "result_type": "Produced Video", "release_date": "2016-05-23T11:00:00-04:00", "title": "The Faint Young Star Paradox: Solar Storms May Have Been Key to Life on Earth", "description": "Energy from our young sun – 4 billion years ago -- aided in creating molecules in Earth's atmosphere that allowed it to warm up enough to incubate life. Complete transcript available.Watch this video on the NASA Goddard YouTube channel. || faintyoung.jpg (1280x720) [105.6 KB] || faintyoung_searchweb.png (320x180) [81.4 KB] || faintyoung_thm.png (80x40) [15.3 KB] || WEBM_G2015-036_FaintYoungStarParadox_V2.webm (960x540) [39.6 MB] || G2015-036_FaintYoungStarParadox_V2.mov (1920x1080) [1.4 GB] || APPLE_TV_G2015-036_FaintYoungStarParadox_V2_appletv.m4v (1280x720) [54.0 MB] || YOUTUBE_HQ_G2015-036_FaintYoungStarParadox_V2_youtube_hq.mov (1920x1080) [318.5 MB] || NASA_TV_G2015-036_FaintYoungStarParadox_V2.mpeg (1280x720) [346.1 MB] || PRORES_B-ROLL_G2015-036_FaintYoungStarParadox_V2_prores.mov (1280x720) [719.8 MB] || APPLE_TV_G2015-036_FaintYoungStarParadox_V2_appletv_subtitles.m4v (1280x720) [54.0 MB] || G2015-036FaintYoungStarParadox_V2.en_US.srt [1.8 KB] || G2015-036FaintYoungStarParadox_V2.en_US.vtt [1.8 KB] || NASA_PODCAST_G2015-036_FaintYoungStarParadox_V2_ipod_sm.mp4 (320x240) [18.8 MB] || G2015-036_FaintYoungStarParadox_V2_lowres.mp4 (480x272) [14.8 MB] || ", "hits": 93 }, { "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": 66 }, { "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": 158 }, { "id": 4312, "url": "https://svs.gsfc.nasa.gov/4312/", "result_type": "Visualization", "release_date": "2015-06-01T16:00:00-04:00", "title": "Measuring Mercury's Magnetism", "description": "Three orbits of MESSENGER at different altitudes show small magnetic field signals from rocks magnetized early in Mercury's history. The signals are strongest at the lowest altitude. || mercury_magnetometry_print.jpg (1024x576) [134.6 KB] || mercury_magnetometry_searchweb.png (320x180) [66.9 KB] || mercury_magnetometry_thm.png (80x40) [4.8 KB] || mercury_magnetometry.tif (2800x3600) [5.4 MB] || ", "hits": 106 }, { "id": 11798, "url": "https://svs.gsfc.nasa.gov/11798/", "result_type": "Produced Video", "release_date": "2015-03-12T00:00:00-04:00", "title": "MMS Pre-launch Live Shots", "description": "MMS Roll Ins || MMS_Roll_Ins.frame741.png (1280x720) [655.3 KB] || MMS_Roll_Ins.frame741_searchweb.png (320x180) [55.2 KB] || MMS_Roll_Ins.mov (1280x720) [2.1 GB] || MMS_Roll_Ins.webmhd.webm (1280x720) [36.6 MB] || ", "hits": 46 }, { "id": 11801, "url": "https://svs.gsfc.nasa.gov/11801/", "result_type": "Produced Video", "release_date": "2015-03-11T09:45:00-04:00", "title": "Goddard's Speedy MMS Instruments Will Measure Mysterious Physics", "description": "MMS Fast Plasma InvestigationHost Katrina Jackson talks with Craig Pollock and Ulrik Gliese about Goddard's contribution to the Magnetospheric Multiscale mission - the Fast Plasma Investigation suite of instruments. These instruments will study a little-understood physics phenomenon known as magnetic reconnection, which is common throughout the universe and affects space weather in Earth's magnetosphere. Watch the video on NASA Explorer. For complete transcript, click here. || MMS_FPI_thumbnail_print.jpg (1024x577) [129.0 KB] || MMS_FPI_thumbnail.png (1407x793) [1.3 MB] || MMS_FPI_thumbnail_thm.png (80x40) [9.9 KB] || MMS_FPI_thumbnail_web.png (320x180) [100.1 KB] || MMS_FPI_thumbnail_searchweb.png (320x180) [100.1 KB] || G2015-003_MMS_FPI_MASTER_youtube_hq.mov (1280x720) [299.8 MB] || G2015-003_MMS_FPI_MASTER_appletv_subtitles.m4v (960x540) [105.8 MB] || G2015-003_MMS_FPI_MASTER_appletv.m4v (960x540) [105.9 MB] || G2015-003_MMS_FPI_MASTER_prores.mov (1280x720) [3.7 GB] || G2015-003_MMS_FPI_MASTER_1280x720.wmv (1280x720) [122.7 MB] || G2015-003_MMS_FPI_MASTER_720x480.webm (720x480) [28.1 MB] || G2015-003_MMS_FPI_MASTER_ipod_lg.m4v (640x360) [41.8 MB] || G2015-003_MMS_FPI_MASTER_720x480.wmv (720x480) [114.2 MB] || MMS_FPI_captions.en_US.srt [5.3 KB] || MMS_FPI_captions.en_US.vtt [5.3 KB] || G2015-003_MMS_FPI_MASTER_nasaportal.mov (640x360) [103.0 MB] || G2015-003_MMS_FPI_MASTER_ipod_sm.mp4 (320x240) [22.6 MB] || ", "hits": 42 }, { "id": 11794, "url": "https://svs.gsfc.nasa.gov/11794/", "result_type": "Produced Video", "release_date": "2015-03-10T12:30:00-04:00", "title": "MMS L-2 Prelaunch News Conference", "description": "On March 12 from Cape Canaveral Florida, NASA is scheduled to launch the Magnetospheric Multiscale, or MMS, mission, which will provide unprecedented detail on a phenomenon called magnetic reconnection. The process of reconnection involves the explosive release of energy when the magnetic fields around Earth connect and disconnect. These fields help protect Earth from harmful effects of solar storms and cosmic rays. Magnetic reconnection also occurs throughout the universe and can accelerate particles up to nearly the speed of light.By studying reconnection in this local, natural laboratory, MMS helps us understand reconnection elsewhere as well, such as in the atmosphere of the Sun and other stars, in the vicinity of black holes and neutron stars, and at the boundary between our solar system's heliosphere and interstellar space.MMS consists of four identical observatories that will provide the first three-dimensional view of magnetic reconnection. The four MMS observatories will fly through reconnection regions in a tight formation in well under a second, so key sensors on each spacecraft are designed to measure the space environment at rates faster than any previous mission.For additional visuals regarding the MMS mission and science, please see our MMS Pre-launch Gallery.Briefing participants include:Geoffrey Yoder, deputy associate administratorNASA Science Mission Directorate, WashingtonOmar Baez, NASA launch managerKennedy Space Center, FloridaVernon Thorp, program manager, NASA MissionsUnited Launch Alliance, Centennial, ColoradoCraig Tooley, NASA MMS project manager,Goddard Space Flight Center, Greenbelt, MarylandJim Burch, principal investigatorSouthwest Research Institute, San Antonio, TexasClay Flinn, launch weather officer, 45th Weather SquadronCape Canaveral Air Force Station, Florida || ", "hits": 13 }, { "id": 11799, "url": "https://svs.gsfc.nasa.gov/11799/", "result_type": "Produced Video", "release_date": 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GyromotionPlane.HD1080.mov (1920x1080) [117.5 MB] || ", "hits": 54 }, { "id": 4262, "url": "https://svs.gsfc.nasa.gov/4262/", "result_type": "Visualization", "release_date": "2015-02-02T00:00:00-05:00", "title": "Plasma Zoo: Gyromotion in Three Dimensions", "description": "Visualization from two camera positions of simple 3-dimensional gyro-motion of charged particles in a magnetic field. || GyromotionZ_inertial.HD1080i.0600_print.jpg (1024x576) [120.9 KB] || GyromotionZ_inertial.HD1080i.0600_searchweb.png (320x180) [78.1 KB] || GyromotionZ_inertial.HD1080i.0600_thm.png (80x40) [5.4 KB] || GyromotionZ_inertial.HD1080i.0600_web.png (320x180) [78.1 KB] || 1920x1080_16x9_30p (1920x1080) [0 Item(s)] || GyromotionZ.HD1080.webm (1920x1080) [3.6 MB] || GyromotionZ_inertial_1080.mp4 (1920x1080) [22.1 MB] || GyromotionZ.HD1080.mov (1920x1080) [118.8 MB] || ", "hits": 96 }, { "id": 4263, "url": "https://svs.gsfc.nasa.gov/4263/", "result_type": "Visualization", "release_date": "2015-02-02T00:00:00-05:00", "title": "Plasma Zoo: Particle Drift in a Magnetic Gradient", "description": "Visualization from two camera positions of simple gyro-motion of charged particles in a changing magnetic field. || BGradient_inertial.HD1080i.0600_print.jpg (1024x576) [124.3 KB] || BGradient_inertial.HD1080i.0600_searchweb.png (320x180) [81.3 KB] || BGradient_inertial.HD1080i.0600_thm.png (80x40) [5.6 KB] || BGradient_inertial.HD1080i.0600_web.png (320x180) [81.3 KB] || 1920x1080_16x9_30p (1920x1080) [0 Item(s)] || BGradient.HD1080.webm (1920x1080) [3.7 MB] || BGradient_inertial_1080.mp4 (1920x1080) [22.2 MB] || BGradient.HD1080.mov (1920x1080) [121.1 MB] || ", "hits": 107 }, { "id": 4264, "url": "https://svs.gsfc.nasa.gov/4264/", "result_type": "Visualization", "release_date": "2015-02-02T00:00:00-05:00", "title": "Plasma Zoo: Field-Aligned Current (Birkeland Current)", "description": "Visualization from two camera positions of gyro-motion of charged particles in parallel electric and magnetic fields. || EBParallel_inertial.HD1080i.0600_print.jpg (1024x576) [123.4 KB] || EBParallel_inertial.HD1080i.0600_searchweb.png (320x180) [80.8 KB] || EBParallel_inertial.HD1080i.0600_web.png (320x180) [80.8 KB] || EBParallel_inertial.HD1080i.0600_thm.png (80x40) [5.6 KB] || EBParallel.cam1 (1920x1080) [0 Item(s)] || EBParallel.cam1.HD1080.webm (1920x1080) [3.6 MB] || EBParallel_cam1_HD1080.mp4 (1920x1080) [22.3 MB] || EBParallel.cam1.HD1080.mov (1920x1080) [120.0 MB] || ", "hits": 168 }, { "id": 4265, "url": "https://svs.gsfc.nasa.gov/4265/", "result_type": "Visualization", "release_date": "2015-02-02T00:00:00-05:00", "title": "Plasma Zoo: E-cross-B Drift", "description": "Visualization from two camera positions of gyro-motion of charged particles in perpendicular electric and magnetic fields. || EBvOrthogonal_inertial.HD1080i.0600_print.jpg (1024x576) [123.3 KB] || EBvOrthogonal_inertial.HD1080i.0600_searchweb.png (320x180) [79.0 KB] || EBvOrthogonal_inertial.HD1080i.0600_thm.png (80x40) [5.5 KB] || EBvOrthogonal_inertial.HD1080i.0600_web.png (320x180) [79.0 KB] || 1920x1080_16x9_30p (1920x1080) [0 Item(s)] || EBvOrthogonal.HD1080.webm (1920x1080) [3.6 MB] || EBvOrthogonal_inertial_1080.mp4 (1920x1080) [22.2 MB] || EBvOrthogonal.HD1080.mov (1920x1080) [120.0 MB] || ", "hits": 307 }, { "id": 11251, "url": "https://svs.gsfc.nasa.gov/11251/", "result_type": "Produced Video", "release_date": "2014-12-10T10:00:00-05:00", "title": "MMS Science Overview: The Mysteries of MMS", "description": "Scientists Michael Hesse and John Dorelli explain the science objectives of the MMS mission. || MMSSciOvThumb720.jpg (1280x720) [60.9 KB] || MMSSciOvThumb720_print.jpg (1024x576) [79.2 KB] || MMSSciOvThumb720_thm.png (80x40) [17.9 KB] || MMSSciOvThumb720_web.png (320x180) [67.2 KB] || MMSSciOvThumb720_searchweb.png (320x180) [67.2 KB] || MMSSciOvThumb720_web.jpg (320x180) [27.4 KB] || 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"hits": 94 }, { "id": 11440, "url": "https://svs.gsfc.nasa.gov/11440/", "result_type": "Produced Video", "release_date": "2014-09-11T09:30:00-04:00", "title": "Ionospheric Holes on Venus", "description": "The European Space Agency's Venus Express mission saw something it could not explain. It appeared that there were holes on the nightside of Venus' ionosphere. Researchers at NASA's Goddard Space Flight Center investigated these mysterious holes, and found evidence that the sun's magnetic field lines may be penetrating through the planet. || ", "hits": 54 }, { "id": 11526, "url": "https://svs.gsfc.nasa.gov/11526/", "result_type": "Produced Video", "release_date": "2014-05-15T01:30:00-04:00", "title": "MMS Mission Trailer", "description": "In March 2015, NASA will launch four identical spacecraft to study how magnetic fields around Earth connect and disconnect, explosively releasing energy – a process known as magnetic reconnection. The Magnetospheric Multiscale, or MMS, mission will provide the first three-dimensional views of this fundamental process that can accelerate particles to nearly the speed of light. MMS uses Earth’s protective magnetic space environment, the magnetosphere, as a natural laboratory to directly measure reconnection. Reconnection is a common processes in our universe; occurring in space near Earth, in the atmosphere of the sun and other stars, in the vicinity of black holes and neutron stars, and at virtually any boundary between space plasmas, including the boundary between our solar system's heliosphere and interstellar space. || ", "hits": 50 }, { "id": 11485, "url": "https://svs.gsfc.nasa.gov/11485/", "result_type": "Produced Video", "release_date": "2014-05-06T00:00:00-04:00", "title": "MMS Narrated Orbit", "description": "Scientist John Dorelli explains the MMS mission's orbit and why the four spacecraft fly in a tetrahedron formation. On its journey, MMS will observe a little-understood, but universal phenomenon called magnetic reconnection, responsible for dramatic re-shaping of the magnetic environment near Earth, often sending intense amounts of energy and fast-moving particles off in a new direction. Not only is this a fundamental physical process that occurs throughout the universe, it is also one of the drivers of space weather events at Earth. To truly understanding the process, requires four identical spacecraft to track how such reconnection events move across and through any given space in 3D. || ", "hits": 43 }, { "id": 11524, "url": "https://svs.gsfc.nasa.gov/11524/", "result_type": "Produced Video", "release_date": "2014-04-18T10:00:00-04:00", "title": "3 Days in 1 Minute: Stacking the MMS Spacecraft", "description": "The Magnetospheric Multiscale, or MMS, mission stacked all four of its spacecraft in preparation for vibration testing. This time lapse shows one image every thirty seconds over three days of work. First, the spacecraft are assembled into mini-stacks, or placed on top of each other in sets of two. To create a full stack, engineers lift one mini-stack on top of another.Vibration testing simulates the conditions that the MMS spacecraft will experience during launch.MMS will study how the sun and the Earth's magnetic fields connect and disconnect, an explosive process that can accelerate particles through space to nearly the speed of light. This process is called magnetic reconnection and can occur throughout all space. || ", "hits": 34 }, { "id": 20210, "url": "https://svs.gsfc.nasa.gov/20210/", "result_type": "Animation", "release_date": "2014-03-14T10:30:00-04:00", "title": "MMS Spacecraft Animation", "description": "The Magnetospheric Multiscale (MMS) mission is a Solar Terrestrial Probes mission comprising four identically instrumented spacecraft that will use Earth’s magnetosphere as a laboratory to study the microphysics of three fundamental plasma processes: magnetic reconnection, energetic particle acceleration, and turbulence. These processes occur in all astrophysical plasma systems but can be studied in situ only in our solar system and most efficiently only in Earth’s magnetosphere, where they control the dynamics of the geospace environment and play an important role in the processes known as “space weather.”Learn more about MMS at www.nasa.gov/mms || ", "hits": 54 }, { "id": 11429, "url": "https://svs.gsfc.nasa.gov/11429/", "result_type": "Produced Video", "release_date": "2013-12-05T17:00:00-05:00", "title": "Sun Magnetic Field Flip Live Shots and Media Resources", "description": "On Dec. 6, 2013, NASA scientists Alex Young and Holly Gilbert discussed how the sun's magnetic field is in the process of flipping. || ", "hits": 152 }, { "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": 95 }, { "id": 11199, "url": "https://svs.gsfc.nasa.gov/11199/", "result_type": "Produced Video", "release_date": "2013-07-15T10:00:00-04:00", "title": "X Marks the Spot: SDO Sees Reconnection", "description": "Two NASA spacecraft have provided the most comprehensive movie ever of a mysterious process at the heart of all explosions on the sun: magnetic reconnection. Magnetic reconnection happens when magnetic field lines come together, break apart, and then exchange partners, snapping into new positions and releasing a jolt of magnetic energy. This process lies at the heart of giant explosions on the sun such as solar flares and coronal mass ejections, which can fling radiation and particles across the solar system. Magnetic field lines, themselves, are invisible, but the sun's charged plasma particles course along their length. Space telescopes can see that material appearing as bright lines looping and arcing through the sun’s atmosphere, and so map out the presence of magnetic field lines. Looking at a series of images from the Solar Dynamics Observatory (SDO), scientists saw two bundles of field lines move toward each other, meet briefly to form what appeared to be an “X” and then shoot apart with one set of lines and its attendant particles leaping into space and one set falling back down onto the sun. To confirm what they were seeing, the scientists turned to a second NASA spacecraft, the Reuven Ramaty High Energy Solar Spectroscopic Imager (RHESSI). RHESSI collects spectrograms, a kind of data that can show where exceptionally hot material is present in any given event on the sun. RHESSI showed hot pockets of solar material forming above and below the reconnection point, an established signature of such an event. By combining the SDO and RHESSI data, the scientists were able to describe the process of what they were seeing, largely confirming previous models and theories, while revealing new, three-dimensional aspects of the process. || ", "hits": 79 }, { "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": 74 }, { "id": 11306, "url": "https://svs.gsfc.nasa.gov/11306/", "result_type": "Produced Video", "release_date": "2013-07-10T12:30:00-04:00", "title": "IBEX Maps Solar System's Tail", "description": "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.To view this video on YouTube, click here. || ", "hits": 69 }, { "id": 11224, "url": "https://svs.gsfc.nasa.gov/11224/", "result_type": "Produced Video", "release_date": "2013-03-26T13:00:00-04:00", "title": "MAVEN Magnetometer", "description": "When you navigate with a compass you can orient yourself thanks to Earth's global magnetic field. But on Mars, if you were to walk around with a compass it would haphazardly point from one anomaly to another, because the Red Planet does not possess a global magnetosphere. Scientists think that this lack of a protective magnetic field may have allowed the solar wind to strip away the Martian atmosphere over billions of years, and now NASA's MAVEN spacecraft will study this process in detail with its pair of ring core fluxgate magnetometers. || ", "hits": 96 }, { "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": 252 }, { "id": 11180, "url": "https://svs.gsfc.nasa.gov/11180/", "result_type": "Produced Video", "release_date": "2013-01-31T13:00:00-05:00", "title": "SDO Provides First Sightings of How
a CME Forms", "description": "On July 18, 2012, a fairly small explosion of light burst off the lower right limb of the sun. Such flares often come with an associated eruption of solar material, known as a coronal mass ejection or CME — but this one did not. Something interesting did happen, however. Magnetic field lines in this area of the sun's atmosphere, the corona, began to twist and kink, generating the hottest solar material — a charged gas called plasma — to trace out the newly-formed slinky shape. The plasma glowed brightly in extreme ultraviolet images from the Atmospheric Imaging Assembly (AIA) aboard NASA's Solar Dynamics Observatory (SDO) and scientists were able to watch for the first time the very formation of something they had long theorized was at the heart of many eruptive events on the sun: a flux rope. Eight hours later, on July 19, the same region flared again. This time the flux rope's connection to the sun was severed, and the magnetic fields escaped into space, dragging billions of tons of solar material along for the ride — a classic CME. More than just gorgeous to see, such direct observation offers one case study on how this crucial kernel at the heart of a CME forms. Such flux ropes have been seen in images of CMEs as they fly away from the sun, but it's never been known — indeed, has been strongly debated — whether the flux rope formed before or in conjunction with a CME's launch. This case shows a clear-cut example of the flux rope forming ahead of time.Watch this video on YouTube. || ", "hits": 68 }, { "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": 50 }, { "id": 11086, "url": "https://svs.gsfc.nasa.gov/11086/", "result_type": "Produced Video", "release_date": "2012-09-27T12:00:00-04:00", "title": "Simulations Uncover 'Flashy' Secrets of Merging Black Holes", "description": "According to Einstein, whenever massive objects interact, they produce gravitational waves — distortions in the very fabric of space and time — that ripple outward across the universe at the speed of light. While astronomers have found indirect evidence of these disturbances, the waves have so far eluded direct detection. Ground-based observatories designed to find them are on the verge of achieving greater sensitivities, and many scientists think that this discovery is just a few years away. Catching gravitational waves from some of the strongest sources — colliding black holes with millions of times the sun's mass — will take a little longer. These waves undulate so slowly that they won't be detectable by ground-based facilities. Instead, scientists will need much larger space-based instruments, such as the proposed Laser Interferometer Space Antenna, which was endorsed as a high-priority future project by the astronomical community. A team that includes astrophysicists at NASA's Goddard Space Flight Center in Greenbelt, Md., is looking forward to that day by using computational models to explore the mergers of supersized black holes. Their most recent work investigates what kind of \"flash\" might be seen by telescopes when astronomers ultimately find gravitational signals from such an event. To explore the problem, a team led by Bruno Giacomazzo at the University of Colorado, Boulder, and including Baker developed computer simulations that for the first time show what happens in the magnetized gas (also called a plasma) in the last stages of a black hole merger. In the turbulent environment near the merging black holes, the magnetic field intensifies as it becomes twisted and compressed. The team suggests that running the simulation for additional orbits would result in even greater amplification. The most interesting outcome of the magnetic simulation is the development of a funnel-like structure — a cleared-out zone that extends up out of the accretion disk near the merged black hole. The most important aspect of the study is the brightness of the merger's flash. The team finds that the magnetic model produces beamed emission that is some 10,000 times brighter than those seen in previous studies, which took the simplifying step of ignoring plasma effects in the merging disks. || ", "hits": 137 }, { "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": 109 }, { "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": 160 }, { "id": 10804, "url": "https://svs.gsfc.nasa.gov/10804/", "result_type": "Produced Video", "release_date": "2011-10-27T08:00:00-04:00", "title": "The Solar Cycle", "description": "The number of sunspots increases and decreases over time in a regular, approximately 11-year cycle, called the sunspot cycle. The exact length of the cycle can vary. It has been as short as eight years and as long as fourteen, but the number of sunspots always increases over time, and then returns to low again. More sunspots mean increased solar activity, when great blooms of radiation known as solar flares or bursts of solar material known as coronal mass ejections (CMEs) shoot off the sun's surface. The highest number of sun spots in any given cycle is designated \"solar maximum,\" while the lowest number is designated \"solar minimum.\" Each cycle, varies dramatically in intensity, with some solar maxima being so low as to be almost indistinguishable from the preceding minimum. Sunspots are a magnetic phenomenon and the entire sun is magnetized with a north and a south magnetic pole just like a bar magnet. The comparison to a simple bar magnet ends there, however, as the sun's interior is constantly on the move. By tracking sound waves that course through the center of the sun, an area of research known as helioseismology, scientists can gain an understanding of what's deep inside the sun. They have found that the magnetic material inside the sun is constantly stretching, twisting, and crossing as it bubbles up to the surface. The exact pattern of movements is not conclusively mapped out, but over time they eventually lead to the poles reversing completely. The sunspot cycle happens because of this poles flip — north becomes south and south becomes north—approximately every 11 years. Some 11 years later, the poles reverse again back to where they started, making the full solar cycle actually a 22-year phenomenon. The sun behaves similarly over the course of each 11-year cycle no matter which pole is on top, however, so this shorter cycle tends to receive more attention. || ", "hits": 570 }, { "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": 39 }, { "id": 10740, "url": "https://svs.gsfc.nasa.gov/10740/", "result_type": "Produced Video", "release_date": "2011-04-07T09:00:00-04:00", "title": "When Neutron Stars Collide", "description": "Armed with state-of-the-art supercomputer models, scientists have shown that colliding neutron stars can produce the energetic jet required for a gamma-ray burst. Earlier simulations demonstrated that mergers could make black holes. Others had shown that the high-speed particle jets needed to make a gamma-ray burst would continue if placed in the swirling wreckage of a recent merger. Now, the simulations reveal the middle step of the process—how the merging stars' magnetic field organizes itself into outwardly directed components capable of forming a jet. The Damiana supercomputer at Germany's Max Planck Institute for Gravitational Physics needed six weeks to reveal the details of a process that unfolds in just 35 thousandths of a second—less than the blink of an eye.For the researchers' website, with more video and stills of their simulations, go here. || ", "hits": 372 }, { "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": 370 }, { "id": 3794, "url": "https://svs.gsfc.nasa.gov/3794/", "result_type": "Visualization", "release_date": "2010-11-09T00:00:00-05:00", "title": "STEREO in Stereo: April 8, 2007", "description": "Full Disk View: Image sequences taken April 8-9, 2007 by the EUVI telescopes on the two STEREO spacecraft (STEREO-B, left eye; STEREO-A, right eye). At this time the spacecraft were about 3.7 degrees apart. These images show the Sun in extreme ultraviolet light at a wavelength of 171 angstroms, highlighting parts of the Sun's atmosphere (the corona) at about one million degrees C. Note the bright active regions near the Sun's equator and the dark \"coronal holes\" at the north and south poles. These are features of the Sun's magnetic field. Coronal holes are areas where the magnetic field opens out to allow material to flow out into the solar system, while active regions are made up of strong, closed fields which bottle up hot plasma (ionized gas) close to the surface. This image was taken near the minimum in solar activity, so there are few active regions.Closeup View: Image sequences taken April 8-9, 2007 by the EUVI telescopes in the SECCHI imaging suites on the two STEREO spacecraft (STEREO-B, left eye; STEREO-A, right eye). At this time the spacecraft were about 3.7 degrees apart. Here we see a close up of solar magnetic active regions, flickering as they rotate out of sight around the sun. These are areas where the Sun's strong magnetic field bottles up million degree C plasma (ionized gas) low in the corona (the Sun's outer atmosphere). These images are taken at a wavelength of 171 angstroms (0.00000171 cm) in the extreme ultraviolet.Note for Large Displays: These movies are produced using images from STEREO where the angle between the spacecraft is getting larger than the optimum angle for stereo separation. While they work well on small displays, large-screens and projection systems can introduce significant distortions in the stereo effect which the audience may find uncomfortable. When doing large-screen projection, you may need to adjust the left-right image alignment for optimum viewing. However, this does not guarantee a distortion-free result. || ", "hits": 155 }, { "id": 3697, "url": "https://svs.gsfc.nasa.gov/3697/", "result_type": "Visualization", "release_date": "2010-04-21T14:15:00-04:00", "title": "SDO/HMI Magnetogram Full Disk View - March 29, 2010", "description": "This early sequence of images from the HMI imager is processed to reveal the magnetic field structure (magnetogram). White locations represent a positive magnetic field value (north polarity) while black represents a negative magnetic field value (south polarity). Grey is zero magnetic field.The black and white region slightly above the center corresponds to a visible sunspot. Weaker magnetic regions are visible around the disk. || ", "hits": 56 }, { "id": 3713, "url": "https://svs.gsfc.nasa.gov/3713/", "result_type": "Visualization", "release_date": "2010-04-21T14:15:00-04:00", "title": "SDO/HMI Magnetogram Full Disk View - April 7, 2010", "description": "This early sequence of images from the HMI imager is processed to reveal the magnetic field structure (magnetogram). White locations represent a positive magnetic field value (north polarity) while black represents a negative magnetic field value (south polarity). Gray is zero magnetic field.Notice that the surface magnetic fields reveal much more structure than the white-light images in SDO/HMI Continuum Full Disk View - April 7, 2010. || ", "hits": 38 }, { "id": 10584, "url": "https://svs.gsfc.nasa.gov/10584/", "result_type": "Produced Video", "release_date": "2010-03-22T00:00:00-04:00", "title": "Heliophysics Program Overview", "description": "This short program overview for NASA's heliophysics division explains how NASA studies the sun—and more importantly—how it affects our daily lives. || ", "hits": 136 }, { "id": 3605, "url": "https://svs.gsfc.nasa.gov/3605/", "result_type": "Visualization", "release_date": "2009-07-06T00:00:00-04:00", "title": "Magnetospheric Multiscale Mission (MMS) Dayside Orbit Animation for the Preliminary Design Review (PDR)", "description": "This visualization uses simulated ephemerides to show the proposed orbits of the Magnetospheric Multiscale Mission (MMS) during the \"dayside magnetosheath/magnetopause\" orbit phase. The movie initially shows the general orientation of the orbit with respect to the Earth, Moon, and Sun. It then zooms in to \"ride\" along with the spacecraft. We then zoom in even closer to show that there are actually four spacecraft flying in a tetrahedral formation. Finally, we see how the 4 spacecraft skim the magnetosheath such that, occasionally, some of the spacecraft are inside (e.g., MMS #1) and some are outside (e.g., MMS #2, #3, and #4) of the magnetosheath boundary.This visualization was created in support of the MMS Preliminary Design Review (PDR) which was held May 4 - 7, 2009. || ", "hits": 31 } ] }