{
    "count": 38,
    "next": null,
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    "results": [
        {
            "id": 109,
            "url": "http://svs.gsfc.nasa.gov/109/",
            "result_type": "Visualization",
            "release_date": "1996-10-16T12:00:00-04:00",
            "title": "Increasing Air Traffic Safety, Using Real Time Weather in the Cockpit",
            "description": "This video describes advances in remote sensing and information technology that can be used to provide real time weather to airline pilots during flight. || ",
            "hits": 68
        },
        {
            "id": 98,
            "url": "http://svs.gsfc.nasa.gov/98/",
            "result_type": "Visualization",
            "release_date": "1996-02-23T12:00:00-05:00",
            "title": "Glacier Bay, Alaska, from the Ground, Air and Space",
            "description": "This video contains a mix of live action video, stills, and computer animations of the Glacier Bay National Park in Glacier Bay, Alaska.Satellite mapping and imagery are used to show changes in the Glacier Bay area over a period of several years. Specific image processing techniques are discussed in relation to determining the evolution of glacier terminus points and in obtaining elevation data and how it is used to create fly-by visualizations of the area. || ",
            "hits": 52
        },
        {
            "id": 97,
            "url": "http://svs.gsfc.nasa.gov/97/",
            "result_type": "Visualization",
            "release_date": "1996-02-08T12:00:00-05:00",
            "title": "Images of Earth and Space: The Role of Visualization in NASA Science",
            "description": "This compilation video contains visualizations of Earth and Space Sciences resulting from supercomputer models. The excerpted visualizations include: Ocean Planet, El Niño, Ozone 1991, Clouds, Changes in Glacier Bay, Alaska, Biosphere, Lunar Topography from the Clementine Mission, Musculoskeletal Modeling Dynamic Simulations, Simulations of the Breakup and Dynamical Evolution of Comet Shoemaker-Levy 9, Convective Penetration in Stellar Interiors, Topological Features of a Compressible Plasma Vortex Sheet: A Model for the Outer Heliospheric Solar Wind, R-Aquarii Jet, The Evolution of Distorted Black Holes, Rayleigh-Taylor Instability in a Supernova, Galaxy Harassment, N-Body Simulation of the Cold Dark Matter Cosmology. || ",
            "hits": 101
        },
        {
            "id": 91,
            "url": "http://svs.gsfc.nasa.gov/91/",
            "result_type": "Visualization",
            "release_date": "1995-06-04T12:00:00-04:00",
            "title": "Motion in the R-Aquarii Jet 1991, 1992, 1993: Image Deconvolution of 1992 Data",
            "description": "Images from the Hubble Space Telescope's Faint Object Camera from 1991, 1992, and 1993 demonstrate motion in the R Aquarii emission jet. Since images from this period were still affected by the primary mirror flaw, the images were restored to the original design resolution using the maximum entropy method. || ",
            "hits": 20
        },
        {
            "id": 1388,
            "url": "http://svs.gsfc.nasa.gov/1388/",
            "result_type": "Visualization",
            "release_date": "1995-06-04T12:00:00-04:00",
            "title": "Motion in the R-Aquarii Jet 1991, 1992, 1993: 2-D Motion",
            "description": "Images from the Hubble Space Telescope's Faint Object Camera from 1991, 1992, and 1993 demonstrate motion in the R Aquarii emission jet. Since images from this period were still affected by the primary mirror flaw, the images were restored to the original design resolution using the maximum entropy method. || ",
            "hits": 13
        },
        {
            "id": 1389,
            "url": "http://svs.gsfc.nasa.gov/1389/",
            "result_type": "Visualization",
            "release_date": "1995-06-04T12:00:00-04:00",
            "title": "Motion in the R-Aquarii Jet 1991, 1992, 1993: 3-D Perspective",
            "description": "Images from the Hubble Space Telescope's Faint Object Camera from 1991, 1992, and 1993 demonstrate motion in the R Aquarii emission jet. Since images from this period were still affected by the primary mirror flaw, the images were restored to the original design resolution using the maximum entropy method. || ",
            "hits": 10
        },
        {
            "id": 89,
            "url": "http://svs.gsfc.nasa.gov/89/",
            "result_type": "Visualization",
            "release_date": "1995-01-01T12:00:00-05:00",
            "title": "SAMPEX - A Synoptic View of Earth's Electron Radiation Belts: North Pole Energetic Fluxes from HILT",
            "description": "The Solar Anomalous and Magnetospheric Particle Explorer, SAMPEX, measures fluxes of energetic particles from the sun, the Earth's magnetosphere, and cosmic ray sources over a broad range of energies. The four instruments aboard SAMPEX are the Low-Energy Ion Analyzer (LEICA), The Heavy Ion Large Telescope (HILT), The Mass Spectrometer Telescope (MAST), and the Proton-Electron Telescope (PET). || ",
            "hits": 42
        },
        {
            "id": 1385,
            "url": "http://svs.gsfc.nasa.gov/1385/",
            "result_type": "Visualization",
            "release_date": "1995-01-01T12:00:00-05:00",
            "title": "SAMPEX - A Synoptic View of Earth's Electron Radiation Belts: South Pole Energetic Fluxes from HILT",
            "description": "The Solar Anomalous and Magnetospheric Particle Explorer, SAMPEX, measures fluxes of energetic particles from the sun, the Earth's magnetosphere, and cosmic ray sources over a broad range of energies.  The four instruments aboard SAMPEX are the Low-Energy Ion Analyzer (LEICA), The Heavy Ion Large Telescope (HILT), The Mass Spectrometer Telescope (MAST), and the Proton-Electron Telescope (PET). || ",
            "hits": 12
        },
        {
            "id": 1386,
            "url": "http://svs.gsfc.nasa.gov/1386/",
            "result_type": "Visualization",
            "release_date": "1995-01-01T12:00:00-05:00",
            "title": "SAMPEX - A Synoptic View of Earth's Electron Radiation Belts: North Pole Energetic Fluxes from PET",
            "description": "The Solar Anomalous and Magnetospheric Particle Explorer, SAMPEX, measures fluxes of energetic particles from the sun, the Earth's magnetosphere, and cosmic ray sources over a broad range of energies.  The four instruments aboard SAMPEX are the Low-Energy Ion Analyzer (LEICA), The Heavy Ion Large Telescope (HILT), The Mass Spectrometer Telescope (MAST), and the Proton-Electron Telescope (PET). || ",
            "hits": 1912
        },
        {
            "id": 1387,
            "url": "http://svs.gsfc.nasa.gov/1387/",
            "result_type": "Visualization",
            "release_date": "1995-01-01T12:00:00-05:00",
            "title": "SAMPEX - A Synoptic View of Earth's Electron Radiation Belts: South Pole Energetic Fluxes from PET",
            "description": "The Solar Anomalous and Magnetospheric Particle Explorer, SAMPEX, measures fluxes of energetic particles from the sun, the Earth's magnetosphere, and cosmic ray sources over a broad range of energies.  The four instruments aboard SAMPEX are the Low-Energy Ion Analyzer (LEICA), The Heavy Ion Large Telescope (HILT), The Mass Spectrometer Telescope (MAST), and the Proton-Electron Telescope (PET). || ",
            "hits": 15
        },
        {
            "id": 18,
            "url": "http://svs.gsfc.nasa.gov/18/",
            "result_type": "Visualization",
            "release_date": "1994-10-19T12:00:00-04:00",
            "title": "SEDS-II: Before and After Deployment",
            "description": "An animation of the subsatellite dynamics of Small Expendable Deployer System Mission II || a000018.00005_web.png (720x480) [334.1 KB] || a000018_thm.png (80x40) [3.3 KB] || a000018_pre.jpg (320x238) [4.9 KB] || a000018_pre_searchweb.jpg (320x180) [28.5 KB] || a000018.webmhd.webm (960x540) [14.0 MB] || a000018.dv (720x480) [675.2 MB] || a000018.mp4 (640x480) [38.6 MB] || a000018.mpg (352x240) [26.4 MB] || ",
            "hits": 56
        },
        {
            "id": 19,
            "url": "http://svs.gsfc.nasa.gov/19/",
            "result_type": "Visualization",
            "release_date": "1994-10-19T12:00:00-04:00",
            "title": "SEDS-II: Slowest period of deployment",
            "description": "An animation of the subsatellite dynamics of Small Expendable Deployer System Mission II || a000019.00005_web.png (720x480) [327.8 KB] || a000019_thm.png (80x40) [2.9 KB] || a000019_pre.jpg (320x238) [4.6 KB] || a000019_pre_searchweb.jpg (320x180) [26.7 KB] || a000019.webmhd.webm (960x540) [7.0 MB] || a000019.dv (720x480) [346.3 MB] || a000019.mp4 (640x480) [19.8 MB] || a000019.mpg (352x240) [13.3 MB] || ",
            "hits": 53
        },
        {
            "id": 20,
            "url": "http://svs.gsfc.nasa.gov/20/",
            "result_type": "Visualization",
            "release_date": "1994-10-19T12:00:00-04:00",
            "title": "SEDS-II: End of Deployment",
            "description": "An animation of the subsatellite dynamics of Small Expendable Deployer System Mission II || a000020.00005_web.png (720x480) [328.5 KB] || a000020_thm.png (80x40) [2.9 KB] || a000020_pre.jpg (320x238) [4.6 KB] || a000020_pre_searchweb.jpg (320x180) [27.4 KB] || a000020.webmhd.webm (960x540) [20.6 MB] || a000020.mp4 (640x480) [63.0 MB] || a000020.dv (720x480) [1.1 GB] || a000020.mpg (352x240) [43.7 MB] || ",
            "hits": 58
        },
        {
            "id": 21,
            "url": "http://svs.gsfc.nasa.gov/21/",
            "result_type": "Visualization",
            "release_date": "1994-10-19T12:00:00-04:00",
            "title": "SEDS-II: Final Dynamic State",
            "description": "An animation of the subsatellite dynamics of Small Expendable Deployer System Mission II || a000021.00005_web.png (720x480) [335.6 KB] || a000021_thm.png (80x40) [3.0 KB] || a000021_pre.jpg (320x238) [4.7 KB] || a000021_pre_searchweb.jpg (320x180) [27.6 KB] || a000021.webmhd.webm (960x540) [7.8 MB] || a000021.dv (720x480) [346.5 MB] || a000021.mp4 (640x480) [19.6 MB] || a000021.mpg (352x240) [13.4 MB] || ",
            "hits": 57
        },
        {
            "id": 22,
            "url": "http://svs.gsfc.nasa.gov/22/",
            "result_type": "Visualization",
            "release_date": "1994-10-19T12:00:00-04:00",
            "title": "SEDS-II: First 120 Minutes",
            "description": "An animation of the subsatellite dynamics of Small Expendable Deployer System Mission II || a000022.00005_web.png (720x480) [338.6 KB] || a000022_thm.png (80x40) [3.3 KB] || a000022_pre.jpg (320x238) [4.7 KB] || a000022_pre_searchweb.jpg (320x180) [27.0 KB] || a000022.webmhd.webm (960x540) [27.1 MB] || a000022.dv (720x480) [844.8 MB] || a000022.mp4 (640x480) [48.6 MB] || a000022.mpg (352x240) [33.0 MB] || ",
            "hits": 50
        },
        {
            "id": 36,
            "url": "http://svs.gsfc.nasa.gov/36/",
            "result_type": "Visualization",
            "release_date": "1994-10-03T12:00:00-04:00",
            "title": "1992 Daily Ozone from Nimbus-7",
            "description": "In this animation of total ozone, the luminance values of the colors bounding areas of missing data are used in interpolating over these regions.  The missing data are mapped to the grayscale portion of the color map. || ",
            "hits": 50
        },
        {
            "id": 37,
            "url": "http://svs.gsfc.nasa.gov/37/",
            "result_type": "Visualization",
            "release_date": "1994-10-03T12:00:00-04:00",
            "title": "1993 Daily Ozone from Nimbus-7",
            "description": "In this animation of total ozone, the luminance values of the colors bounding areas of missing data are used in interpolating over these regions.  The missing data are mapped to the grayscale portion of the color map. || ",
            "hits": 17
        },
        {
            "id": 38,
            "url": "http://svs.gsfc.nasa.gov/38/",
            "result_type": "Visualization",
            "release_date": "1994-10-03T12:00:00-04:00",
            "title": "1993 Daily Ozone from Meteor-3",
            "description": "In this animation of total ozone, the luminance values of the colors bounding areas of missing data are used in interpolating over these regions.  The missing data are mapped to the grayscale portion of the color map. || ",
            "hits": 25
        },
        {
            "id": 60,
            "url": "http://svs.gsfc.nasa.gov/60/",
            "result_type": "Visualization",
            "release_date": "1994-05-20T12:00:00-04:00",
            "title": "Nonlinear Studies of Coronal Heating by the Resonant Absorption of Alfven Waves",
            "description": "A series of animations showing various quantities from a coronal heating simulation || a000060.00005_web.png (720x480) [280.0 KB] || a000060_thm.png (80x40) [3.6 KB] || a000060_pre.jpg (320x238) [5.4 KB] || a000060_pre_searchweb.jpg (320x180) [25.3 KB] || a000060.webmhd.webm (960x540) [48.4 MB] || a000060.dv (720x480) [653.3 MB] || a000060.mp4 (640x480) [37.5 MB] || a000060.mpg (352x240) [29.3 MB] || ",
            "hits": 58
        },
        {
            "id": 15,
            "url": "http://svs.gsfc.nasa.gov/15/",
            "result_type": "Visualization",
            "release_date": "1994-04-01T12:00:00-05:00",
            "title": "SEDS-I: Subsatellite in motion (30 frames/second)",
            "description": "An animation of the subsatellite dynamics of Small Expendable Deployer System Mission I || a000015.00005_web.png (720x480) [357.8 KB] || a000015_thm.png (80x40) [4.1 KB] || a000015_pre.jpg (320x238) [5.3 KB] || a000015_pre_searchweb.jpg (320x180) [33.9 KB] || a000015.webmhd.webm (960x540) [33.9 MB] || a000015.dv (720x480) [905.5 MB] || a000015.mp4 (640x480) [51.9 MB] || a000015.mpg (352x240) [35.6 MB] || ",
            "hits": 56
        },
        {
            "id": 16,
            "url": "http://svs.gsfc.nasa.gov/16/",
            "result_type": "Visualization",
            "release_date": "1994-04-01T12:00:00-05:00",
            "title": "SEDS-I: Subsatellite in motion (6 frames/second)",
            "description": "An animation of the subsatellite dynamics of Small Expendable Deployer System Mission I. (The online version of this animation is shown at 30 frames-sec, but the tape version is at 6 frames-sec.) || a000016.00005_web.png (720x480) [357.6 KB] || a000016_thm.png (80x40) [4.1 KB] || a000016_pre.jpg (320x238) [5.3 KB] || a000016_pre_searchweb.jpg (320x180) [33.9 KB] || a000016.webmhd.webm (960x540) [115.8 MB] || a000016.dv (720x480) [4.4 GB] || a000016.mp4 (640x480) [250.0 MB] || a000016.mpg (352x240) [35.6 MB] || ",
            "hits": 56
        },
        {
            "id": 17,
            "url": "http://svs.gsfc.nasa.gov/17/",
            "result_type": "Visualization",
            "release_date": "1994-04-01T12:00:00-05:00",
            "title": "SEDS-I: Subsatellite in motion (every 10th frame)",
            "description": "An animation of the subsatellite dynamics of Small Expendable Deployer System Mission I || a000017.00005_web.png (720x480) [354.3 KB] || a000017_thm.png (80x40) [4.2 KB] || a000017_pre.jpg (320x238) [5.5 KB] || a000017_pre_searchweb.jpg (320x180) [35.0 KB] || a000017.webmhd.webm (960x540) [4.0 MB] || a000017.dv (720x480) [102.8 MB] || a000017.mp4 (640x480) [5.9 MB] || a000017.mpg (352x240) [3.8 MB] || ",
            "hits": 56
        },
        {
            "id": 39,
            "url": "http://svs.gsfc.nasa.gov/39/",
            "result_type": "Visualization",
            "release_date": "1994-02-12T12:00:00-05:00",
            "title": "Rayleigh-Taylor Instabilities in Supernovae Explosions: Density",
            "description": "The following calculation shows the development and evolution of Rayleigh-Taylor instabilities which develop behind the supernova blast wave on a time scale of a few hours. The initial model was chosen to provide a good representation for the progenitor star for Supernova 1987A. The calculation was performed using the Piecewise-Parabolic Method for hydrodynamics on a two-dimensional spherical grid with rotational symmetry about the vertical axis and equatorial symmetry about the horizontal axis.The grid contained 800 zones in the radial direction and 400 zones in the angular diraction and was allowed to expand homologously with the explosion to maintain as high a resolution as possible in the unstable layer during the evolution. The following sequences show the evolution of the density distribution as well as the distribution of hydrogen, helium, and oxygen within the ejecta to illustrate the amount of mixing caused by the instability. Each sequence shows the evolution in two reference frames.In the first frame, the size of the plot expands with time as the grid expands. For the second reference frame, the size of the plot is kept fixed with the time so that more detail can be seen in the unstable layer. || ",
            "hits": 57
        },
        {
            "id": 40,
            "url": "http://svs.gsfc.nasa.gov/40/",
            "result_type": "Visualization",
            "release_date": "1994-02-12T12:00:00-05:00",
            "title": "Rayleigh-Taylor Instabilities in Supernovae Explosions: Hydrogen Mass Fraction",
            "description": "The following calculation shows the development and evolution of Rayleigh-Taylor instabilities which develop behind the supernova blast wave on a time scale of a few hours. The initial model was chosen to provide a good representation for the progenitor star for Supernova 1987A. The calculation was performed using the Piecewise-Parabolic Method for hydrodynamics on a two-dimensional spherical grid with rotational symmetry about the vertical axis and equatorial symmetry about the horizontal axis.The grid contained 800 zones in the radial direction and 400 zones in the angular diraction and was allowed to expand homologously with the explosion to maintain as high a resolution as possible in the unstable layer during the evolution. The following sequences show the evolution of the density distribution as well as the distribution of hydrogen, helium, and oxygen within the ejecta to illustrate the amount of mixing caused by the instability. Each sequence shows the evolution in two reference frames.In the first frame, the size of the plot expands with time as the grid expands. For the second reference frame, the size of the plot is kept fixed with the time so that more detail can be seen in the unstable layer. || ",
            "hits": 60
        },
        {
            "id": 41,
            "url": "http://svs.gsfc.nasa.gov/41/",
            "result_type": "Visualization",
            "release_date": "1994-02-12T12:00:00-05:00",
            "title": "Rayleigh-Taylor Instabilities in Supernovae Explosions: Partial Density of Hydrogen",
            "description": "The following calculation shows the development and evolution of Rayleigh-Taylor instabilities which develop behind the supernova blast wave on a time scale of a few hours. The initial model was chosen to provide a good representation for the progenitor star for Supernova 1987A. The calculation was performed using the Piecewise-Parabolic Method for hydrodynamics on a two-dimensional spherical grid with rotational symmetry about the vertical axis and equatorial symmetry about the horizontal axis.The grid contained 800 zones in the radial direction and 400 zones in the angular diraction and was allowed to expand homologously with the explosion to maintain as high a resolution as possible in the unstable layer during the evolution. The following sequences show the evolution of the density distribution as well as the distribution of hydrogen, helium, and oxygen within the ejecta to illustrate the amount of mixing caused by the instability. Each sequence shows the evolution in two reference frames.In the first frame, the size of the plot expands with time as the grid expands. For the second reference frame, the size of the plot is kept fixed with the time so that more detail can be seen in the unstable layer. || ",
            "hits": 52
        },
        {
            "id": 42,
            "url": "http://svs.gsfc.nasa.gov/42/",
            "result_type": "Visualization",
            "release_date": "1994-02-12T12:00:00-05:00",
            "title": "Rayleigh-Taylor Instabilities in Supernovae Explosions: Helium Mass Fraction",
            "description": "The following calculation shows the development and evolution of Rayleigh-Taylor instabilities which develop behind the supernova blast wave on a time scale of a few hours. The initial model was chosen to provide a good representation for the progenitor star for Supernova 1987A. The calculation was performed using the Piecewise-Parabolic Method for hydrodynamics on a two-dimensional spherical grid with rotational symmetry about the vertical axis and equatorial symmetry about the horizontal axis.The grid contained 800 zones in the radial direction and 400 zones in the angular diraction and was allowed to expand homologously with the explosion to maintain as high a resolution as possible in the unstable layer during the evolution. The following sequences show the evolution of the density distribution as well as the distribution of hydrogen, helium, and oxygen within the ejecta to illustrate the amount of mixing caused by the instability. Each sequence shows the evolution in two reference frames.In the first frame, the size of the plot expands with time as the grid expands. For the second reference frame, the size of the plot is kept fixed with the time so that more detail can be seen in the unstable layer. || ",
            "hits": 55
        },
        {
            "id": 43,
            "url": "http://svs.gsfc.nasa.gov/43/",
            "result_type": "Visualization",
            "release_date": "1994-02-12T12:00:00-05:00",
            "title": "Rayleigh-Taylor Instabilities in Supernovae Explosions: Partial Density of Helium",
            "description": "The following calculation shows the development and evolution of Rayleigh-Taylor instabilities which develop behind the supernova blast wave on a time scale of a few hours. The initial model was chosen to provide a good representation for the progenitor star for Supernova 1987A. The calculation was performed using the Piecewise-Parabolic Method for hydrodynamics on a two-dimensional spherical grid with rotational symmetry about the vertical axis and equatorial symmetry about the horizontal axis.The grid contained 800 zones in the radial direction and 400 zones in the angular diraction and was allowed to expand homologously with the explosionto maintain as high a resolution as possible in the unstable layer during the evolution. The following sequences show the evolution of the density distribution as well as the distribution of hydrogen, helium, and oxygen within the ejecta to illustrate the amount of mixing caused by the instability. Each sequence shows the evolution in two reference frames.In the first frame, the size of the plot expands with time as the grid expands. For the second reference frame, the size of the plot is kept fixed with the time so that more detail can be seen in the unstable layer. || ",
            "hits": 43
        },
        {
            "id": 44,
            "url": "http://svs.gsfc.nasa.gov/44/",
            "result_type": "Visualization",
            "release_date": "1994-02-12T12:00:00-05:00",
            "title": "Rayleigh-Taylor Instabilities in Supernovae Explosions: Oxygen Mass Fraction",
            "description": "The following calculation shows the development and evolution of Rayleigh-Taylor instabilities which develop behind the supernova blast wave on a time scale of a few hours. The initial model was chosen to provide a good representation for the progenitor star for Supernova 1987A. The calculation was performed using the Piecewise-Parabolic Method for hydrodynamics on a two-dimensional spherical grid with rotational symmetry about the vertical axis and equatorial symmetry about the horizontal axis.The grid contained 800 zones in the radial direction and 400 zones in the angular diraction and was allowed to expand homologously with the explosion to maintain as high a resolution as possible in the unstable layer during the evolution. The following sequences show the evolution of the density distribution as well as the distribution of hydrogen, helium, and oxygen within the ejecta to illustrate the amount of mixing caused by the instability. Each sequence shows the evolution in two reference frames.In the first frame, the size of the plot expands with time as the grid expands. For the second reference frame, the size of the plot is kept fixed with the time so that more detail can be seen in the unstable layer. || ",
            "hits": 21
        },
        {
            "id": 45,
            "url": "http://svs.gsfc.nasa.gov/45/",
            "result_type": "Visualization",
            "release_date": "1994-02-12T12:00:00-05:00",
            "title": "Rayleigh-Taylor Instabilities in Supernovae Explosions: Partial Density of Oxygen",
            "description": "The following calculation shows the development and evolution of Rayleigh-Taylor instabilities which develop behind the supernova blast wave on a time scale of a few hours. The initial model was chosen to provide a good representation for the progenitor star for Supernova 1987A. The calculation was performed using the Piecewise-Parabolic Method for hydrodynamics on a two-dimensional spherical grid with rotational symmetry about the vertical axis and equatorial symmetry about the horizontal axis.The grid contained 800 zones in the radial direction and 400 zones in the angular diraction and was allowed to expand homologously with the explosion to maintain as high a resolution as possible in the unstable layer during the evolution. The following sequences show the evolution of the density distribution as well as the distribution of hydrogen, helium, and oxygen within the ejecta to illustrate the amount of mixing caused by the instability. Each sequence shows the evolution in two reference frames.In the first frame, the size of the plot expands with time as the grid expands. For the second reference frame, the size of the plot is kept fixed with the time so that more detail can be seen in the unstable layer. || ",
            "hits": 48
        },
        {
            "id": 46,
            "url": "http://svs.gsfc.nasa.gov/46/",
            "result_type": "Visualization",
            "release_date": "1994-02-12T12:00:00-05:00",
            "title": "Instabilities in Very Young Neutron Stars: Density",
            "description": "This simulation shows the first 20 milliseconds in the life of a neutron star which is formed in a Type II supernova. After an initial collapse phase, the neutron star becomes unstable to convection. The resulting convective motions destroy the spherical symmetry of the star and rapidly mix the inner regions. In addition, the neutrino flux from the neutron star will be non-spherical and will be significantly enhanced by the convective motions. This may have major implications for the Type II supernova mechanism. The calculation was performed using the Piecewise-Parabolic Method for hydrodynamics. The computational grid contained 300 zones in radius and 200 zones in angle. The inner 200 zones in radius were uniformly spaced, ranging from the inner boundary at 25 km to 175 km. The outer 100 zones were non-uniformly spaced and stretched to 2000 km. Only the inner 200 zones are plotted. The inner boundary was treated as a hard sphere. At the outer boundary, zero gradients for all the variables were assumed. Periodic boundary conditions were used along the sides of the grid. The following sequence shows the density evolution for 20 milliseconds after the shock stalls. The density is plotted on a log scale. Values range from 10^9 gm/cm^3 at the outer boundary to 1.4 x 10^12 gm/cm^3 at the inner boundary. || ",
            "hits": 52
        },
        {
            "id": 47,
            "url": "http://svs.gsfc.nasa.gov/47/",
            "result_type": "Visualization",
            "release_date": "1994-02-12T12:00:00-05:00",
            "title": "Instabilities in Very Young Neutron Stars: Temperature",
            "description": "This simulation shows the first 20 milliseconds in the life of a neutron star which is formed in a Type II supernova. After an initial collapse phase, the neutron star becomes unstable to convection. The resulting convective motions destroy the spherical symmetry of the star and rapidly mix the inner regions. In addition, the neutrino flux from the neutron star will be non-spherical and will be significantly enhanced by the convective motions. This may have major implications for the Type II supernova mechanism. The calculation was performed using the Piecewise-Parabolic Method for hydrodynamics. The computational grid contained 300 zones in radius and 200 zones in angle. The inner 200 zones in radius were uniformly spaced, ranging from the inner boundary at 25 km to 175 km. The outer 100 zones were non-uniformly spaced and stretched to 2000 km. Only the inner 200 zones are plotted. The inner boundary was treated as a hard sphere. At the outer boundary, zero gradients for all the variables were assumed. Periodic boundary conditions were used along the sides of the grid. The following sequence shows the temperature structure for 20 milliseconds after the shock stalls. The minimum temperature is approximately 1.35 MeV. The maximum temperature varies from 6 MeV at the beginning of the calculation to 10 MeV at the later times. || ",
            "hits": 56
        },
        {
            "id": 48,
            "url": "http://svs.gsfc.nasa.gov/48/",
            "result_type": "Visualization",
            "release_date": "1994-02-12T12:00:00-05:00",
            "title": "Instabilities in Very Young Neutron Stars: Electron Fraction",
            "description": "This simulation shows the first 20 milliseconds in the life of a neutron star which is formed in a Type II supernova. After an initial collapse phase, the neutron star becomes unstable to convection. The resulting convective motions destroy the spherical symmetry of the star and rapidly mix the inner regions. In addition, the neutrino flux from the neutron star will be non-spherical and will be significantly enhanced by the convective motions. This may have major implications for the Type II supernova mechanism. The calculation was performed using the Piecewise-Parabolic Method for hydrodynamics. The computational grid contained 300 zones in radius and 200 zones in angle. The inner 200 zones in radius were uniformly spaced, ranging from the inner boundary at 25 km to 175 km. The outer 100 zones were non-uniformly spaced and stretched to 2000 km. Only the inner 200 zones are plotted. The inner boundary was treated as a hard sphere. At the outer boundary, zero gradients for all the variables were assumed. Periodic boundary conditions were used along the sides of the grid. The following sequence shows the mixing of composition which results from the convective motions. The variable plotted is the electron fraction Ye, which ranges from 0.2 to 0.5. || ",
            "hits": 55
        },
        {
            "id": 1381,
            "url": "http://svs.gsfc.nasa.gov/1381/",
            "result_type": "Visualization",
            "release_date": "1994-02-12T12:00:00-05:00",
            "title": "Instabilities in Very Young Neutron Stars: Density",
            "description": "This simulation shows the first 20 milliseconds in the life of a neutron star which is formed in a Type II supernova. After an initial collapse phase, the neutron star becomes unstable to convection. The resulting convective motions destroy the spherical symmetry of the star and rapidly mix the inner regions. In addition, the neutrino flux from the neutron star will be non-spherical and will be significantly enhanced by the convective motions. This may have major implications for the Type II supernova mechanism. The calculation was performed using the Piecewise-Parabolic Method for hydrodynamics. The computational grid contained 300 zones in radius and 200 zones in angle. The inner 200 zones in radius were uniformly spaced, ranging from the inner boundary at 25 km to 175 km. The outer 100 zones were non-uniformly spaced and stretched to 2000 km. Only the inner 200 zones are plotted. The inner boundary was treated as a hard sphere. At the outer boundary, zero gradients for all the variables were assumed. Periodic boundary conditions were used along the sides of the grid. The following sequence shows the density evolution for 20 milliseconds after the shock stalls. The density is plotted on a log scale. Values range from 10^9 gm/cm^3 at the outer boundary to 1.4 x 10^12 gm/cm^3 at the inner boundary. || ",
            "hits": 21
        },
        {
            "id": 1382,
            "url": "http://svs.gsfc.nasa.gov/1382/",
            "result_type": "Visualization",
            "release_date": "1994-02-12T12:00:00-05:00",
            "title": "Instabilities in Very Young Neutron Stars: Temperature",
            "description": "This simulation shows the first 20 milliseconds in the life of a neutron star which is formed in a Type II supernova. After an initial collapse phase, the neutron star becomes unstable to convection. The resulting convective motions destroy the spherical symmetry of the star and rapidly mix the inner regions. In addition, the neutrino flux from the neutron star will be non-spherical and will be significantly enhanced by the convective motions. This may have major implications for the Type II supernova mechanism. The calculation was performed using the Piecewise-Parabolic Method for hydrodynamics. The computational grid contained 300 zones in radius and 200 zones in angle. The inner 200 zones in radius were uniformly spaced, ranging from the inner boundary at 25 km to 175 km. The outer 100 zones were non-uniformly spaced and stretched to 2000 km. Only the inner 200 zones are plotted. The inner boundary was treated as a hard sphere. At the outer boundary, zero gradients for all the variables were assumed. Periodic boundary conditions were used along the sides of the grid. The following sequence shows the temperature structure for 20 milliseconds after the shock stalls. The minimum temperature is approximately 1.35 MeV. The maximum temperature varies from 6 MeV at the beginning of the calculation to 10 MeV at the later times. || ",
            "hits": 29
        },
        {
            "id": 1383,
            "url": "http://svs.gsfc.nasa.gov/1383/",
            "result_type": "Visualization",
            "release_date": "1994-02-12T12:00:00-05:00",
            "title": "Instabilities in Very Young Neutron Stars: Electron Fraction",
            "description": "This simulation shows the first 20 milliseconds in the life of a neutron star which is formed in a Type II supernova. After an initial collapse phase, the neutron star becomes unstable to convection. The resulting convective motions destroy the spherical symmetry of the star and rapidly mix the inner regions. In addition, the neutrino flux from the neutron star will be non-spherical and will be significantly enhanced by the convective motions. This may have major implications for the Type II supernova mechanism. The calculation was performed using the Piecewise-Parabolic Method for hydrodynamics. The computational grid contained 300 zones in radius and 200 zones in angle. The inner 200 zones in radius were uniformly spaced, ranging from the inner boundary at 25 km to 175 km. The outer 100 zones were non-uniformly spaced and stretched to 2000 km. Only the inner 200 zones are plotted. The inner boundary was treated as a hard sphere. At the outer boundary, zero gradients for all the variables were assumed. Periodic boundary conditions were used along the sides of the grid. The following sequence shows the mixing of composition which results from the convective motions. The variable plotted is the electron fraction Ye, which ranges from 0.2 to 0.5. || ",
            "hits": 26
        },
        {
            "id": 23,
            "url": "http://svs.gsfc.nasa.gov/23/",
            "result_type": "Visualization",
            "release_date": "1994-01-14T12:00:00-05:00",
            "title": "Changes in Glacier Bay: Glacier Fly Up",
            "description": "Flying up Glacier Bays Muir Inlet, ending at the Muir Glacier || a000023.00005_web.png (720x480) [515.3 KB] || a000023_thm.png (80x40) [5.7 KB] || a000023_pre.jpg (320x238) [8.3 KB] || a000023_pre_searchweb.jpg (320x180) [60.0 KB] || a000023.webmhd.webm (960x540) [3.1 MB] || a000023.dv (720x480) [72.3 MB] || a000023.mp4 (640x480) [4.0 MB] || a000023.mpg (352x240) [2.5 MB] || ",
            "hits": 48
        },
        {
            "id": 24,
            "url": "http://svs.gsfc.nasa.gov/24/",
            "result_type": "Visualization",
            "release_date": "1994-01-14T12:00:00-05:00",
            "title": "Changes in Glacier Bay: Glacier Zoom In",
            "description": "Zooming in from a full image of Glacier Bay to a closeup of the Muir Glacier || a000024.00005_web.png (720x480) [698.7 KB] || a000024_thm.png (80x40) [7.1 KB] || a000024_pre.jpg (320x238) [15.0 KB] || a000024_pre_searchweb.jpg (320x180) [84.8 KB] || a000024.webmhd.webm (960x540) [3.6 MB] || a000024.dv (720x480) [54.0 MB] || a000024.mp4 (640x480) [3.1 MB] || a000024.mpg (352x240) [2.0 MB] || ",
            "hits": 44
        },
        {
            "id": 8,
            "url": "http://svs.gsfc.nasa.gov/8/",
            "result_type": "Visualization",
            "release_date": "1993-12-17T12:00:00-05:00",
            "title": "Topological Features of a Compressible Plasma Vortex Sheet: 6 Cases",
            "description": "The Voyager and Pioneer Spacecraft have detected large-scale quasi-periodic plasma fluctuations in the outer heliosphere beyond 20 AU. A plasma vortex sheet model can explain these fluctuations and the observed correlations between various physical variables. The large scale outer heliosphere is modeled by solving the 3-D compressible magnetohydrodynamic equations involving three interacting shear layers.Computations were done on a Cray computer at the NASA Center for Computational Sciences.Six cases are animated: Weak magnetic field and strong magnetic field, each at three values of tau, the vortex street characteristic time. Contours of density are shown as dark transparent 'tubes'. Critical points of the velocity field are represented by 'Glyphs'. Vortex cores are shown in orange and blue. || ",
            "hits": 75
        }
    ]
}