{
    "count": 13,
    "next": null,
    "previous": null,
    "results": [
        {
            "id": 5375,
            "url": "https://svs.gsfc.nasa.gov/5375/",
            "result_type": "Visualization",
            "release_date": "2025-08-07T14:00:00-04:00",
            "title": "Carrington Class Coronal Mass Ejection - ENLIL Simulation of A Series of CMEs",
            "description": "A series of visualizations of the simulation of a series of CMEs between July 2012 and August 2012, including a carrington class coronal mass ejection that hit STEREO-A.",
            "hits": 310
        },
        {
            "id": 4861,
            "url": "https://svs.gsfc.nasa.gov/4861/",
            "result_type": "Visualization",
            "release_date": "2021-03-17T00:00:00-04:00",
            "title": "Three years of SAGE III/ISS Stratospheric Aerosol Data",
            "description": "About three years of stratospheric aerosol data from SAGE III visualizing a zonal mean and measurements of various high aerosol events across the globe || sage3_final_full_60fps.7300_print.jpg (1024x576) [98.9 KB] || sage3_final_full_60fps.7300_searchweb.png (320x180) [57.4 KB] || sage3_final_full_60fps.7300_thm.png (80x40) [4.4 KB] || sage3_final_full_1080p59.94.webm (1920x1080) [25.5 MB] || orig (3840x2160) [1.0 MB] || sage3_final_full_1080p59.94.mp4 (1920x1080) [234.0 MB] || sage3_final_full_2160p59.94.mp4 (3840x2160) [1.0 GB] || ",
            "hits": 25
        },
        {
            "id": 4699,
            "url": "https://svs.gsfc.nasa.gov/4699/",
            "result_type": "Visualization",
            "release_date": "2018-11-30T14:00:00-05:00",
            "title": "The CME Heard 'Round the Solar System",
            "description": "As the CMEs and SIRs move through the solar system, we include graphs of particle fluxes measured at Earth, Mars, and STEREO-A. || SEPsAtMars.topfixed.UHDframes.clockSlate_HAE.UHD3840.01000_print.jpg (1024x576) [100.6 KB] || SEPsAtMars.topfixed.UHDframes.clockSlate_HAE.UHD3840.01000_thm.png (80x40) [6.5 KB] || SEPsAtMars.topfixed.UHDframes.clockSlate_HAE.UHD3840.01000_searchweb.png (320x180) [87.5 KB] || SEPsAtMars.topfixed_HAE.HD1080i_p30.mp4 (1920x1080) [19.4 MB] || 1920x1080_16x9_30p (1920x1080) [0 Item(s)] || SEPsAtMars.topfixed_HAE.HD1080i_p30.webm (1920x1080) [3.0 MB] || SEPsAtMars.topfixed_HAE_2160p30.mp4 (3840x2160) [61.6 MB] || 3840x2160_16x9_30p (3840x2160) [0 Item(s)] || ",
            "hits": 84
        },
        {
            "id": 4188,
            "url": "https://svs.gsfc.nasa.gov/4188/",
            "result_type": "Visualization",
            "release_date": "2014-09-25T10:00:00-04:00",
            "title": "Comparative Magnetospheres: A Noteworthy Coronal Mass Ejection",
            "description": "In an effort to understand and predict the impact of space weather events on Earth, the Community-Coordinated Modeling Center (CCMC) at NASA Goddard Space Flight Center, routinely runs computer models of the many historical events.  These model runs are then compared to actual data to determine ways to improve the model, and therefore forecasts of the impacts of future space weather events.In mid-December of 2006, the Sun erupted with a bright flare and coronal mass ejection (CME) that launched particles Earthward.  While not the brightest or largest event observed, its impact on Earth was substantial, requiring some effort to protect satellites (ESA: Reacting to a solar flare).The visualization presented here is a CCMC run of a BATS-R-US model simulating the impact of this event on Earth.  Here, lines are used to represent the 'flow direction' of magnetic field of the solar wind impacting Earth, as well as the effects on Earth's geomagnetic field. A 'cut-plane' through the data illustrates the changes in the particle density in the solar wind and magnetosphere.  The color of the data represents a logarithmic scaling of density, with red as the highest (1000 particles per cubic centimeter) down to blue (0.01 particles per cubic centimeter).  In this simulation, each frame of the movie corresponds to two minutes of real time.In the movie, we see vertical field lines of magnetic field carried by the solar wind, coming in from the left.  As this field, and the plasma carrying it, strike Earth's magnetic field, they bend and reconnect, around the Earth.  Some field lines actually reconnect to the polar regions of the Earth, providing a ready flow-path for particles to reach the ionosphere and generate aurora.   This interaction between the solar wind and the plasma trapped in Earth's magnetosphere also creates a density enhancement between Earth and the solar wind helping to shield Earth from some of the effects.   A lower density wake forms behind Earth (the blue region).  There is a circular 'hole' around the Earth which is a gap in the model. || ",
            "hits": 164
        },
        {
            "id": 4167,
            "url": "https://svs.gsfc.nasa.gov/4167/",
            "result_type": "Visualization",
            "release_date": "2014-07-23T00:00:00-04:00",
            "title": "The Big CME that Missed Earth",
            "description": "July of 2012 witnessed the eruption of a very large and fast solar coronal mass ejection (CME) (see NASA STEREO Observes One of the Fastest CMEs On Record and Carrington-class CME Narrowly Misses Earth ).  While not directed at Earth, it was sufficiently large that it could have seriously disrupted the global electrical infrastructure.  The event did impact STEREO-A of NASA's heliophysics fleet which provided a host of measurements (see Sentinels of the Heliosphere).One of the conditions which contributed to the high speed of this event is that two smaller CMEs were launched a little earlier, and these events cleared out much of the solar wind material, leaving little to slow the outflow of the July 23 event (UTC).In the visualizations below, generated from the Enlil space weather model, green represents particle density, usually protons and other ions.  In green, we see the Parker spiral moving out from the sun generated by the sun's current sheet (Wikipedia).  Red represents particles at high temperatures and shows the CME is hotter than the usual solar wind flow.  Large changes in density are represented in blue.  These three colors sometimes combine to tell us more about the characteristics of the event (noted in the 3-color Venn diagram below).However, if this CME had struck Earth's magnetosphere, which has a much stronger magnetic field, the changing magnetic field would induce much larger voltages in systems with long electrical conductors, such as power lines that run over long distances.  These significantly higher voltages can damage power transformers. || ",
            "hits": 131
        },
        {
            "id": 3740,
            "url": "https://svs.gsfc.nasa.gov/3740/",
            "result_type": "Visualization",
            "release_date": "2010-07-08T00:00:00-04:00",
            "title": "Space Weather Event: The View from L1",
            "description": "We start from a position 'behind' the Earth, looking towards the Sun. From this position we see the orbit of the Moon as well as three of the heliospheric 'sentinels' (see \"Sentinels of the Heliosphere\"), ACE, SOHO, and Wind patrolling along 'halo orbits' (Wikipedia) around the Sun-Earth Lagrange Point, L1.The CME (orange isosurface) erupts, heading towards the Earth. The density enhancement of the CME is visible in slice of data in the Earth's orbit plane which provides a better sense of when the CME actually reaches the Earth.As the particle density enhancement from the CME strikes the Earth, we see the Earth's magnetosphere respond, with the outer, high density surface (red), 'blown away'. This surface location corresponds roughly to the location of the bow shock. The bow shock has not been eliminated, only some of its particles have been depleted, to be carried off in the CME and solar wind. As the densest material of the CME passes (orange surface), plasma from the CME continues to flow by the Earth, stretching the magnetosphere into a long, thin structure behind the Earth.The magnetosphere slowly recovers from the 'impact', and regions that can confine higher particle densities reform - the red surfaces return. But not for long as the rarefaction behind the CME reaches the Earth. This lower density region provides fewer particles to repopulate the magnetosphere and make it easier for particles confined in the magnetosphere to 'leak' out into the solar wind.For the BATS-R-US model, the isosurface colors are: red=20 AMUs per cubic centimeter, yellow=10.0 AMUs per cubic centimeter, light blue=1.0 AMUs per cubic centimeter, and blue=0.1 AMUs per cubic centimeter. An AMU corresponds to about the mass of a hydrogen atom, the dominant component of the solar wind.This visualization is part of a series of visualizations on space weather modeling. || ",
            "hits": 22
        },
        {
            "id": 3741,
            "url": "https://svs.gsfc.nasa.gov/3741/",
            "result_type": "Visualization",
            "release_date": "2010-07-08T00:00:00-04:00",
            "title": "Space Weather Event: The View from Above",
            "description": "We open with a view from high above the ecliptic plane, at the space between the Sun (left) and the Earth (within the small rectangular box on the right). In the plane of the Earth's orbit, we show a 'slice' of the Enlil model showing the particle density profile of the solar wind (white to yellow for decreasing particle density). The spiral 'rotating water sprinkler' pattern in the density is the Parker spiral (Wikipedia). The CME (orange surface) erupts in the direction of the Earth. The orange surface represents a boundary of common pressure differences, which better identifies sharp transitions in pressure common in shocks fronts. The CME clears out particles in the region behind it, called a rarefaction (Wikipedia), visible in the particle density.This visualization is part of a series of visualizations on space weather modeling. || ",
            "hits": 21
        },
        {
            "id": 3742,
            "url": "https://svs.gsfc.nasa.gov/3742/",
            "result_type": "Visualization",
            "release_date": "2010-07-08T00:00:00-04:00",
            "title": "Space Weather Event: A View from the Orbit Plane",
            "description": "We start with a view of the space between the Sun (left) and the Earth (within the small rectangular box on the right), slightly above the ecliptic plane. In the plane of the Earth's orbit, we show a 'slice' of the particle density profile of the solar wind (white to yellow for decreasing particle density). Perpendicular to this, we have another 'slice' of particle density from the Enlil model. The Enlil model extends to 60 degrees above and below the solar equator, and beyond 20 solar radii from the Sun. This gap creates the 'hourglass' empty region around the Sun.The CME (orange surface) erupts in the direction of the Earth. The orange surface represents a boundary of common pressure differences, which better identifies sharp transitions in pressure common in shocks fronts. The CME clears out particles in the region behind it, called a rarefaction (Wikipedia), visible in the particle density.This visualization is part of a series of visualizations on space weather modeling. || ",
            "hits": 32
        },
        {
            "id": 3743,
            "url": "https://svs.gsfc.nasa.gov/3743/",
            "result_type": "Visualization",
            "release_date": "2010-07-08T00:00:00-04:00",
            "title": "Space Weather Event: Close-up on the Earth Environment",
            "description": "We open with a view from high above the ecliptic plane, at the space between the Sun (left) and the Earth (within the small rectangular box on the right). In the plane of the Earth's orbit, we show a 'slice' of the Enlil model showing the particle density profile of the solar wind (white to yellow for decreasing particle density). The spiral 'rotating water sprinkler' pattern in the density is the Parker spiral (Wikipedia). We zoom down to the Earth as the CME (orange surface) erupts in the direction of the Earth and move into a position above the Earth's orbital plane with the Earth (geospace) environment in view.As the particle density enhancement from the CME strikes the Earth, we see the Earth's magnetosphere respond, with the outer, high density surface (red) 'blown away'. This surface location corresponds roughly to the location of the bow shock. The bow shock has not been eliminated, only some of its particles have been depleted, to be carried off in the CME and solar wind. As the densest material of the CME passes (orange surface), plasma from the CME continues to flow by the Earth, stretching the magnetosphere into a long, thin structure behind the Earth.The magnetosphere slowly recovers from the 'impact', and regions that can confine higher particle densities reform - the red surfaces return. But not for long as the rarefaction (Wikipedia) behind the CME reaches the Earth. This lower density region provides fewer particles to repopulate the magnetosphere and makes it easier for particles confined in the magnetosphere to 'leak' out into the solar wind.For the BATS-R-US model, the isosurface colors are: red=20 AMUs per cubic centimeter, yellow=10.0 AMUs per cubic centimeter, light blue=1.0 AMUs per cubic centimeter, and blue=0.1 AMUs per cubic centimeter. An AMU corresponds to about the mass of a hydrogen atom, the dominant component of the solar wind.This visualization is part of a series of visualizations on space weather modeling. || ",
            "hits": 32
        },
        {
            "id": 3739,
            "url": "https://svs.gsfc.nasa.gov/3739/",
            "result_type": "Visualization",
            "release_date": "2010-07-06T00:00:00-04:00",
            "title": "Space Weather Event: Incoming View",
            "description": "We open with a view from high above the ecliptic plane, at the space between the Sun (left) and the Earth (within the small rectangular box on the right). In the plane of the Earth's orbit, we show a 'slice' of the Enlil model showing the particle density profile of the solar wind (white to yellow for decreasing particle density). The spiral 'rotating water sprinkler' pattern in the density is the Parker spiral (Wikipedia). The nested grid pattern centered on the Earth, provides a sense of scale to the scene. The smallest grid square in the opening view is 1,000 Earth radii on each side. The scale changes by a factor of ten for each step larger or smaller in size.We zoom down to the Earth as the CME (orange surface) erupts in the direction of the Earth, then move into a position behind the Earth with the Sun visible in the distance.As the particle density enhancement from the CME strikes the Earth, we see the Earth's magnetosphere respond, with the outer, high density surface (red) 'blown away'. This surface location corresponds roughly to the location of the bow shock. The bow shock has not been eliminated, only some of its particles have been depleted, to be carried off in the CME and solar wind. As the densest material of the CME passes (orange surface), plasma from the CME continues to flow by the Earth, stretching the magnetosphere into a long, thin structure behind the Earth.The magnetosphere slowly recovers from the 'impact', and regions that can confine higher particle densities reform - the red surfaces return. But not for long as the rarefaction (Wikipedia) behind the CME reaches the Earth. This lower density region provides fewer particles to repopulate the magnetosphere and makes it easier for particles confined in the magnetosphere to 'leak' out into the solar wind.For the BATS-R-US model, the isosurface colors correpond to densities of: red=20 AMUs per cubic centimeter, yellow=10.0 AMUs per cubic centimeter, light blue=1.0 AMUs per cubic centimeter, and blue=0.1 AMUs per cubic centimeter. An AMU corresponds to about the mass of a hydrogen atom, so the value roughly corresponds to the number of atoms per cubic centimeter.This visualization is part of a series of visualizations on space weather modeling. || ",
            "hits": 31
        },
        {
            "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": 39
        },
        {
            "id": 2391,
            "url": "https://svs.gsfc.nasa.gov/2391/",
            "result_type": "Visualization",
            "release_date": "2002-03-01T12:00:00-05:00",
            "title": "Magnetosphere II: The Solar Wind Strikes Back!",
            "description": "A view of a computer-generated model of the Earth's magnetosphere.  Semi-transparent surfaces represent particle density (red is high, blue is low), the silvery tube represent magnetic field lines and the yellow ribbons represent the paths of charged solar wind particles.  In this particular model, the solar wind has an ambient density of 8.35 particles/cm^3.  The isosurfaces are then red (> 17 particles/cm^3), yellow (> 12 particles/cm^3), green (> 8.6 particles/cm^3) and blue (< 1.0 particle/cm^3). || ",
            "hits": 48
        },
        {
            "id": 2387,
            "url": "https://svs.gsfc.nasa.gov/2387/",
            "result_type": "Visualization",
            "release_date": "2002-02-28T12:00:00-05:00",
            "title": "The Magnetosphere: Earth Raises its Shields",
            "description": "A view of a computer-generated model of the Earth's magnetosphere. Semi-transparent surfaces represent particle density (red is high, blue is low) and silvery tubes represent the magnetic field lines. In this particular model, the solar wind has an ambient density of 8.35 particles/cm^3. The isosurfaces are then red (> 17 particles/cm^3), yellow (> 12 particles/cm^3), green (> 8.6 particles/cm^3) and blue (< 1.0 particle/cm^3). || ",
            "hits": 56
        }
    ]
}