{
    "count": 21,
    "next": null,
    "previous": null,
    "results": [
        {
            "id": 97,
            "url": "https://svs.gsfc.nasa.gov/97/",
            "result_type": "Visualization",
            "release_date": "1996-02-08T12:00:00-05:00",
            "title": "Images of Earth and Space: The Role of Visualization in NASA Science",
            "description": "This compilation video contains visualizations of Earth and Space Sciences resulting from supercomputer models. The excerpted visualizations include: Ocean Planet, El Niño, Ozone 1991, Clouds, Changes in Glacier Bay, Alaska, Biosphere, Lunar Topography from the Clementine Mission, Musculoskeletal Modeling Dynamic Simulations, Simulations of the Breakup and Dynamical Evolution of Comet Shoemaker-Levy 9, Convective Penetration in Stellar Interiors, Topological Features of a Compressible Plasma Vortex Sheet: A Model for the Outer Heliospheric Solar Wind, R-Aquarii Jet, The Evolution of Distorted Black Holes, Rayleigh-Taylor Instability in a Supernova, Galaxy Harassment, N-Body Simulation of the Cold Dark Matter Cosmology. || ",
            "hits": 107
        },
        {
            "id": 39,
            "url": "https://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": 86
        },
        {
            "id": 40,
            "url": "https://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": 62
        },
        {
            "id": 41,
            "url": "https://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": 47
        },
        {
            "id": 42,
            "url": "https://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": 48
        },
        {
            "id": 43,
            "url": "https://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": 39
        },
        {
            "id": 44,
            "url": "https://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": 15
        },
        {
            "id": 45,
            "url": "https://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": 39
        },
        {
            "id": 46,
            "url": "https://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": 80
        },
        {
            "id": 47,
            "url": "https://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": 110
        },
        {
            "id": 48,
            "url": "https://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": 53
        },
        {
            "id": 1381,
            "url": "https://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": 16
        },
        {
            "id": 1382,
            "url": "https://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": 40
        },
        {
            "id": 1383,
            "url": "https://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": 10
        },
        {
            "id": 1,
            "url": "https://svs.gsfc.nasa.gov/1/",
            "result_type": "Visualization",
            "release_date": "1990-07-10T12:00:00-04:00",
            "title": "Tidal Streams in Massive X-ray Binary Systems",
            "description": "A tiny neutron star orbits incessantly around a massive star with a diameter a million times larger than its own.  The high luminosity of the massive star drives a strong wind from its surface.  The neutron star crashes through this wind at over 300 kilometers per second.  The gravity and X-ray luminosity of the neutron star act to disrupt the wind, producing an extended wake of dense gas trailing behind the neutron star.  In this simulation, the tidal distortion of the primary star and the resultant tidal stream is shown.  The numerical simulations depicted here were computed using the Cray X-MP 48 at the National Center for Supercomputing Applications, University of Illinois, Urbana-Champaign. || ",
            "hits": 90
        },
        {
            "id": 2,
            "url": "https://svs.gsfc.nasa.gov/2/",
            "result_type": "Visualization",
            "release_date": "1990-07-10T12:00:00-04:00",
            "title": "Tidal Streams in Massive X-ray Binary Systems: Neutron Star Close-up",
            "description": "A tiny neutron star orbits incessantly around a massive star with a diameter a million times larger than its own.  The high luminosity of the massive star drives a strong wind from its surface.  The neutron star crashes through this wind at over 300 kilometers per second.  The gravity and X-ray luminosity of the neutron star act to disrupt the wind, producing an extended wake of dense gas trailing behind the neutron star.  In this simulation, the tidal distortion of the primary star and the resultant tidal stream is shown.  The numerical simulations depicted here were computed using the Cray X-MP 48 at the National Center for Supercomputing Applications, University of Illinois, Urbana-Champaign. || ",
            "hits": 66
        },
        {
            "id": 3,
            "url": "https://svs.gsfc.nasa.gov/3/",
            "result_type": "Visualization",
            "release_date": "1990-07-10T12:00:00-04:00",
            "title": "Stellar Wind Disruption by an Orbiting Neutron Star",
            "description": "A tiny neutron star orbits incessantly around a massive star with a diameter a million times larger than its own.  The high luminosity of the massive star drives a strong wind from its surface.  The neutron star crashes through this wind at over 300 kilometers per second.  The gravity and X-ray luminosity of the neutron star act to disrupt the wind, producing an extended wake of dense gas trailing behind the neutron star.The numerical simulations depicted here were computed using the Cray X-MP 48 at the National Center for Supercomputing Applications, University of Illinois, Urbana-Champaign. || ",
            "hits": 101
        },
        {
            "id": 4,
            "url": "https://svs.gsfc.nasa.gov/4/",
            "result_type": "Visualization",
            "release_date": "1990-07-10T12:00:00-04:00",
            "title": "Stellar Wind Disruption by an Orbiting Neutron Star: Low X-Ray Luminosity",
            "description": "A tiny neutron star orbits incessantly around a massive star with a diameter a million times larger than its own.  The high luminosity of the massive star drives a strong wind from its surface.  The neutron star crashes through this wind at over 300 kilometers per second.  The gravity and X-ray luminosity of the neutron star act to disrupt the wind, producing an extended wake of dense gas trailing behind the neutron star.  This simulation, in the reference frame of the neutron star, shows conditions of low X-ray luminosity. in which there is a small accretion radius, a slight asymmetry, and short timescales for variability.The numerical simulations depicted here were computed using the Cray X-MP 48 at the National Center for Supercomputing Applications, University of Illinois, Urbana-Champaign. || ",
            "hits": 82
        },
        {
            "id": 5,
            "url": "https://svs.gsfc.nasa.gov/5/",
            "result_type": "Visualization",
            "release_date": "1990-07-10T12:00:00-04:00",
            "title": "Stellar Wind Disruption by an Orbiting Neutron Star: Moderate X-Ray Luminosity",
            "description": "A tiny neutron star orbits incessantly around a massive star with a diameter a million times larger than its own.  The high luminosity of the massive star drives a strong wind from its surface.  The neutron star crashes through this wind at over 300 kilometers per second.  The gravity and X-ray luminosity of the neutron star act to disrupt the wind, producing an extended wake of dense gas trailing behind the neutron star.  This simulation, in the reference frame of the neutron star, shows conditions of low X-ray luminosity. in which there is a large accretion radius, significant asymmetry, and long timescales for variability.The numerical simulations depicted here were computed using the Cray X-MP 48 at the National Center for Supercomputing Applications, University of Illinois, Urbana-Champaign. || ",
            "hits": 70
        },
        {
            "id": 6,
            "url": "https://svs.gsfc.nasa.gov/6/",
            "result_type": "Visualization",
            "release_date": "1990-07-10T12:00:00-04:00",
            "title": "Stellar Wind Disruption by an Orbiting Neutron Star: High X-Ray Luminosity",
            "description": "A tiny neutron star orbits incessantly around a massive star with a diameter a million times larger than its own. The high luminosity of the massive star drives a strong wind from its surface. The neutron star crashes through this wind at over 300 kilometers per second. The gravity and X-ray luminosity of the neutron star act to disrupt the wind, producing an extended wake of dense gas trailing behind the neutron star. This simulation, in the reference frame of the neutron star, shows conditions of high X-ray luminosity, in which there is a weak bow shock, no oscillation, and a large photoionization wake. The numerical simulations depicted here were computed using the Cray X-MP 48 at the National Center for Supercomputing Applications, University of Illinois, Urbana-Champaign. || ",
            "hits": 62
        },
        {
            "id": 7,
            "url": "https://svs.gsfc.nasa.gov/7/",
            "result_type": "Visualization",
            "release_date": "1990-07-10T12:00:00-04:00",
            "title": "Stellar Wind Disruption by an Orbiting Neutron Star: Neutron Star Close-up",
            "description": "A tiny neutron star orbits incessantly around a massive star with a diameter a million times larger than its own.  The high luminosity of the massive star drives a strong wind from its surface.  The neutron star crashes through this wind at over 300 kilometers per second.  The gravity and X-ray luminosity of the neutron star act to disrupt the wind, producing an extended wake of dense gas trailing behind the neutron star.  The large scale structure seen in the accretion wake is powered by the release of gravitational potential energy near the surface of the neutron star.The numerical simulations depicted here were computed using the Cray X-MP 48 at the National Center for Supercomputing Applications, University of Illinois, Urbana-Champaign. || ",
            "hits": 76
        }
    ]
}