{
    "count": 7,
    "next": null,
    "previous": null,
    "results": [
        {
            "id": 5617,
            "url": "https://svs.gsfc.nasa.gov/5617/",
            "result_type": "Visualization",
            "release_date": "2026-02-26T10:30:00-05:00",
            "title": "ESCAPADE Visits the Distant Magnetotail",
            "description": "Launched on Nov. 13, 2025, NASA’s ESCAPADE (Escape and Plasma Acceleration and Dynamics Explorers) 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.",
            "hits": 413
        },
        {
            "id": 4188,
            "url": "https://svs.gsfc.nasa.gov/4188/",
            "result_type": "Visualization",
            "release_date": "2014-09-25T10:00:00-04:00",
            "title": "Comparative Magnetospheres: A Noteworthy Coronal Mass Ejection",
            "description": "In an effort to understand and predict the impact of space weather events on Earth, the Community-Coordinated Modeling Center (CCMC) at NASA Goddard Space Flight Center, routinely runs computer models of the many historical events.  These model runs are then compared to actual data to determine ways to improve the model, and therefore forecasts of the impacts of future space weather events.In mid-December of 2006, the Sun erupted with a bright flare and coronal mass ejection (CME) that launched particles Earthward.  While not the brightest or largest event observed, its impact on Earth was substantial, requiring some effort to protect satellites (ESA: Reacting to a solar flare).The visualization presented here is a CCMC run of a BATS-R-US model simulating the impact of this event on Earth.  Here, lines are used to represent the 'flow direction' of magnetic field of the solar wind impacting Earth, as well as the effects on Earth's geomagnetic field. A 'cut-plane' through the data illustrates the changes in the particle density in the solar wind and magnetosphere.  The color of the data represents a logarithmic scaling of density, with red as the highest (1000 particles per cubic centimeter) down to blue (0.01 particles per cubic centimeter).  In this simulation, each frame of the movie corresponds to two minutes of real time.In the movie, we see vertical field lines of magnetic field carried by the solar wind, coming in from the left.  As this field, and the plasma carrying it, strike Earth's magnetic field, they bend and reconnect, around the Earth.  Some field lines actually reconnect to the polar regions of the Earth, providing a ready flow-path for particles to reach the ionosphere and generate aurora.   This interaction between the solar wind and the plasma trapped in Earth's magnetosphere also creates a density enhancement between Earth and the solar wind helping to shield Earth from some of the effects.   A lower density wake forms behind Earth (the blue region).  There is a circular 'hole' around the Earth which is a gap in the model. || ",
            "hits": 156
        },
        {
            "id": 4189,
            "url": "https://svs.gsfc.nasa.gov/4189/",
            "result_type": "Visualization",
            "release_date": "2014-09-25T10:00:00-04:00",
            "title": "Comparative Magnetospheres: A Carrington-Class CME",
            "description": "In an effort to understand and predict the impact of space weather events on Earth, the Community-Coordinated Modeling Center (CCMC) at NASA Goddard Space Flight Center, routinely runs computer models of the many historical events. These model runs are then compared to actual data to determine ways to improve the model, and therefore forecasts of the impacts of future space weather events.But sometimes we don't have an actual event where we have lots of data for comparison.  Extreme space weather events are one example where we must test models with a rather limited set of data.This is a model run used to examine the consequences if a large coronal mass ejection (CME) such as The Carrington-Class CME of 2012 had actual hit Earth.  Such model runs allow us to estimate consequences of a large event hitting Earth so we can better protect power grids and satellites.Some of the conclusions from this model run are (documented in the paper linked below):The magnetopause is compressed to the point it is moved inside the orbits of our geosynchronous satellites.Large field-aligned currents are created on the night-side of Earth, generating large ionospheric potentials.At high latitudes, geo-electric fields of 26 volts per kilometer can be generated.For comparison, the geo-electric field of the March 1989 storm which generated an extensive power outage in Canada (Wikipedia) had a value of only about 6 volts per kilometer; and the 2003 Halloween solar storms (see Halloween Solar Storms 2003) generated a field of about 12 volts per kilometer. || ",
            "hits": 103
        },
        {
            "id": 4088,
            "url": "https://svs.gsfc.nasa.gov/4088/",
            "result_type": "Visualization",
            "release_date": "2013-09-26T14:00:00-04:00",
            "title": "Reconnection Fronts - What the Models Say...",
            "description": "Mathematical models of Earth's magnetosphere have become increasingly more complex and accurate. They have sufficient detail to illustrate many small-scale phenomena.In this simulation run of the Geospace General Circulation Model (GGCM) we see new details that have been observed by in situ satellites. As the solar wind is deflected around Earth's magnetosphere (the 'bubble' of plasma surrounding Earth held by Earth's magnetic field), plasma flows within the bubble can change. In the graphics below, physical variables such as magnetic field and electric currents are plotted. With these variables, we overlay the net flow of the plasma (arrows), subjected to selection criteria to separate flows of plasma away from Earth and towards Earth. Green arrows are low-speed flows (below about 150 kilometers/second), while red arrows correspond to high-speed plasmal flows (about 300 kilometers/second and higher). || ",
            "hits": 49
        },
        {
            "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": 64
        },
        {
            "id": 3392,
            "url": "https://svs.gsfc.nasa.gov/3392/",
            "result_type": "Visualization",
            "release_date": "2006-12-14T00:00:00-05:00",
            "title": "THEMIS Orbits: Nightside Science Configuration",
            "description": "In the latter phase of the mission, the five THEMIS spacecraft will travel on five co-aligned elliptical orbits with their apogee on the nightside of the Earth. From there, they will sample the particle and electromagnetic wave environment along the magnetotail. The dates in this visualization are based on an ephemeris assuming a launch date of January 20, 2007. The five satellites are represented by colors: red=P1, green=P2, cyan=P3, blue=P4, magenta=P5 || ",
            "hits": 27
        },
        {
            "id": 3356,
            "url": "https://svs.gsfc.nasa.gov/3356/",
            "result_type": "Visualization",
            "release_date": "2006-05-22T00:00:00-04:00",
            "title": "THEMIS Mission and Substorm Simulation",
            "description": "This visualization combines simulations of the THEMIS (Time History of Events and Macroscale Interactions during Substorms) mission orbits with a GGCM (Geospace General Circulation Model) simulation.  It illustrates how the five THEMIS satellites will work together to detect substorm events in the magnetosphere.  One goal of the THEMIS mission is to test how these substorm events are related to the formation of the aurora.This mission consists of five identical spacecraft (usually designated P1, P2, P3, P4 and P5) with orbits aligned so they reach their apogee along the same line from the Earth.  This alignment remains fixed in space so as the Earth moves around the Sun, the constellation of spacecraft will extend on the nightside of the Earth in winter to sample the Earth's magnetosphere, and on the dayside of the Earth in summer to sample the incoming solar wind.  This way they can better map the geospace environment.Probes P1 and P2 are called the 'outer probes' and P3, 4, and 5 are the 'inner probes'.  P3 and P4 share the same orbit.  The outer probes will detect the onset of the substorm, while the inner probes will monitor the Earthward plasma flows from the event.For more information on the GGCM model, visit the Community Coordinated Modeling Center and OpenGGCM. || ",
            "hits": 45
        }
    ]
}