{ "count": 27, "next": null, "previous": null, "results": [ { "id": 14956, "url": "https://svs.gsfc.nasa.gov/14956/", "result_type": "Produced Video", "release_date": "2026-01-26T16:00:00-05:00", "title": "Space Weather Effects Animations", "description": "Solar flares, coronal mass ejections, solar particle events, and the solar wind form the recipe for space weather that affects life on Earth and astronauts in space. A farmer stops their planting operations due to poor GPS signal for their autonomous tractor. A power grid manager changes the configuration of their network to ensure a blackout doesn’t occur due to voltage instability. A pilot switches to back-up communication equipment due to loss of high-frequency radio. A commercial internet company providing service to the military must change the orbit of their spacecraft to avoid a collision due to increased atmospheric drag.These are a few examples of the ways the Sun influences our everyday lives. This is what we define as space weather – the conditions of the space environment driven by the Sun and it’s impacts on objects in the solar system. Learn more about space weather: https://science.nasa.gov/space-weather-2/ || ", "hits": 574 }, { "id": 14907, "url": "https://svs.gsfc.nasa.gov/14907/", "result_type": "Produced Video", "release_date": "2025-09-30T14:00:00-04:00", "title": "What is space weather?", "description": "Though it is almost 100 million miles away from Earth, the Sun influences our daily lives in ways you may not realize.A farmer stops their planting operations due to poor GPS signal for their autonomous tractor. A power grid manager changes the configuration of their network to ensure a blackout doesn’t occur due to voltage instability. A pilot switches to back-up communication equipment due to loss of high-frequency radio. A commercial internet company providing service to the military must change the orbit of their spacecraft to avoid a collision due to increased atmospheric drag.These are a few examples of the ways the Sun influences our everyday lives. This is what we define as space weather – the conditions of the space environment driven by the Sun and its impacts on objects in the solar system. || ", "hits": 234 }, { "id": 5423, "url": "https://svs.gsfc.nasa.gov/5423/", "result_type": "Visualization", "release_date": "2024-11-27T11:00:00-05:00", "title": "Gravity waves disturbing the stratospheric polar vortex", "description": "Animation 1: Changes in temperature and height on the surface of 850 Kelvin potential temperature. The mountain generated gravity waves create strong cooling  as the gravity waves propagate through the stratosphere, while the polar vortex (the cold blue ring) evolves to become colder. || stratospher850_039_T.02498_print.jpg (1024x576) [108.0 KB] || stratospher850_039_T.02498_searchweb.png (320x180) [50.4 KB] || stratospher850_039_T.02498_thm.png (80x40) [4.2 KB] || stratospher850_039_T_1080p30.mp4 (1920x1080) [52.0 MB] || stratospher850_039_T [0 Item(s)] || stratospher850_039_T.mp4 (3840x2160) [148.7 MB] || stratospher850_039_T.mp4.hwshow || ", "hits": 105 }, { "id": 13852, "url": "https://svs.gsfc.nasa.gov/13852/", "result_type": "Produced Video", "release_date": "2021-05-26T10:00:00-04:00", "title": "NASA’s Roman Mission to Probe Cosmic Secrets Using Exploding Stars", "description": "NASA’s upcoming Nancy Grace Roman Space Telescope will see thousands of exploding stars called supernovae across vast stretches of time and space. Using these observations, astronomers aim to shine a light on several cosmic mysteries, providing a window onto the universe’s distant past and hazy present.Credit: NASA's Goddard Space Flight CenterMusic: \"Relentless Data\" from Universal Production MusicWatch this video on the NASA Goddard YouTube channel.Complete transcript available. || Supernova_IA_1285_print.jpg (1024x576) [53.0 KB] || Supernova_IA_1285.png (3840x2160) [5.0 MB] || Supernova_IA_1285_searchweb.png (320x180) [46.9 KB] || Supernova_IA_1285_thm.png (80x40) [4.6 KB] || 13852_Roman_Standard_Candle_Supernovae_1080_Best.webm (1920x1080) [28.3 MB] || 13852_Roman_Standard_Candle_Supernovae_1080.mp4 (1920x1080) [136.7 MB] || 13852_Roman_Standard_Candle_Supernovae_1080_Best.mp4 (1920x1080) [654.2 MB] || 13852RomanStandardCandleSupernovaeCaptionsFix.en_US.srt [4.7 KB] || 13852RomanStandardCandleSupernovaeCaptionsFix.en_US.vtt [4.7 KB] || 13852_Roman_Standard_Candle_Supernovae_ProRes_1920x1080_2997.mov (1920x1080) [3.2 GB] || ", "hits": 113 }, { "id": 20344, "url": "https://svs.gsfc.nasa.gov/20344/", "result_type": "Animation", "release_date": "2021-05-26T10:00:00-04:00", "title": "Type Ia Supernovae Animations", "description": "White Dwarf establishing shot. || WDStar_4k_60fps_ProRes.00600_print.jpg (1024x576) [27.4 KB] || WDStar_4k_60fps_ProRes.00600_searchweb.png (320x180) [30.7 KB] || WDStar_4k_60fps_ProRes.00600_thm.png (80x40) [3.2 KB] || WDStar_4k_60fps_h264.mp4 (3840x2160) [37.3 MB] || WDStar_4k (3840x2160) [0 Item(s)] || WDStar_4k_60fps_ProRes.webm (3840x2160) [4.1 MB] || WDStar_4k_60fps_ProRes.mov (3840x2160) [3.0 GB] || ", "hits": 348 }, { "id": 10662, "url": "https://svs.gsfc.nasa.gov/10662/", "result_type": "Produced Video", "release_date": "2021-04-14T00:00:00-04:00", "title": "Webb Science Simulations: Planetary Systems and Origins of Life", "description": "Supercomputer simulations of planeratry evolution. Part 1: Turbulent Molecular Cloud Nebula with Protostellar ObjectsThe Advanced Visualization Laboratory (AVL) at the National Center for Supercomputing Applications (NCSA) collaborated with NASA and Drs. Alexei Kritsuk and Michael Norman to visualize a computational data set of a turbulent molecular cloud nebula forming protostellar objects and accretion disks approximately 100 AU in diameter, on the order of the size of our solar system. AVL used its Amore software to interpolate and render the Adaptive Mesh Refinement (AMR) simulation generated from ENZO code for cosmology and astrophysics. The AMR simulation was developed by Drs. Kritsuk and Norman at the Laboratory for Computational Astrophysics. The AMR simulation generated more than 2 terabytes of data and follows star formation processes in a self-gravitating turbulent molecular cloud with a dynamic range of half-a-million in linear scale, resolving both the large-scale filamentary structure of the molecular cloud (~5 parsec) and accretion disks around emerging young protostellar objects (down to 2 AU). Part 2: Protoplanetary Disk and Planet FormationThe Advanced Visualization Laboratory (AVL) at the National Center for Supercomputing Applications (NCSA) collaborated with NASA and Dr. Aaron Boley to visualize the 16,000 year evolution of a young, isolated protoplanetary disk which surrounds a newly-formed protostar. The disk forms spiral arms and a dense clump as a result of gravitational collapse. Dr. Aaron Boley developed this computational model to investigate the response of young disks to mass accretion from their surrounding envelopes, including the direct formation of planets and brown dwarfs through gravitational instability. The main formation mechanism for gas giant planets has been debated within the scientific community for over a decade. One of these theories is 'direct formation through gravitational instability.' If the self-gravity of the gas overwhelms the disk's thermal pressure and the stabilizing effect of differential rotation, the gas closest to the protostar rotates faster than gas farther away. In this scenario, regions of the gaseous disk collapse and form a planet directly. The study, presented in Boley (2009), explores whether mass accretion in the outer regions of disks can lead to such disk fragmentation. The simulations show that clumps can form in situ at large disk radii. If the clumps survive, they can become gas giants on wide orbits, e.g., Fomalhaut b, or even more massive objects called brown dwarfs. Whether a disk forms planets at large radii and, if so, the number of planets that form, depend on how much of the envelope mass is distributed at large distances from the protostar. The results of the simulations suggest that there are two modes of gas giant planet formation. The first mode occurs early in the disk's lifetime, at large radii, and through the disk instability mechanism. After the main accretion phase is over, gas giants can form in the inner disk, over a period of a million years, through the core accretion mechanism, which researchers are addressing in other studies.Thanks to R. H. Durisen, L. Mayer, and G. Lake for comments and discussions relating to this research. This study was supported in part by the University of Zurich, Institute for Theoretical Physics, and by a Swiss Federal Grant. Resources supporting this work were provided by the NASA High-End Computing (HEC) Program through the NASA Advanced Supercomputing (NAS) Division at Ames Research Center.AVL at NCSA, University of Illinois. || ", "hits": 218 }, { "id": 40348, "url": "https://svs.gsfc.nasa.gov/gallery/esddatafor-societal-benefits/", "result_type": "Gallery", "release_date": "2018-04-24T00:00:00-04:00", "title": "ESD data for Societal Benefit", "description": "No description available.", "hits": 233 }, { "id": 12807, "url": "https://svs.gsfc.nasa.gov/12807/", "result_type": "Produced Video", "release_date": "2018-01-11T14:10:00-05:00", "title": "Debris Disks Generate Spirals, Rings and Arcs in Simulations", "description": "Astronomers thought patterns spotted in disks around young stars could be planetary signposts. But is there another explanation? A new simulation performed on NASA's Discover supercomputing cluster shows how the dust and gas in the disk could form those patterns no planets needed.Credit: NASA's Goddard Space Flight CenterMusic: \"Hyperborea\" from Killer Tracks.Watch this video on the NASA Goddard YouTube channel.Complete transcript available. || 12807_Disk_Simulation_4k_still_print.jpg (1024x576) [241.9 KB] || 12807_Disk_Simulation_4k_still.jpg (3840x2160) [2.4 MB] || 12807_Disk_Simulation_4k_still_thm.png (80x40) [4.5 KB] || 12807_Disk_Simulation_4k_still_searchweb.png (320x180) [71.2 KB] || 12807_Disk_Simulation_ProRes_1920x1080_2997.mov (1920x1080) [1.5 GB] || 12807_Disk_Simulation_H264_1080p.mov (1920x1080) [263.9 MB] || 12807_Disk_Simulation_H264_1080.m4v (1920x1080) [131.7 MB] || 12807_Disk_Simulation_ProRes_1920x1080_2997.webm (1920x1080) [15.3 MB] || 12807_Disk_Simulation_SRT_Captions.en_US.srt [2.1 KB] || 12807_Disk_Simulation_SRT_Captions.en_US.vtt [2.0 KB] || ", "hits": 52 }, { "id": 30872, "url": "https://svs.gsfc.nasa.gov/30872/", "result_type": "Hyperwall Visual", "release_date": "2017-08-24T00:00:00-04:00", "title": "Where Does Lightning Strike?", "description": "Lightning flash counts are accumulated to create a long-term average lightning flash rate. || ligtning_v1_720p.01138_print.jpg (1024x576) [116.7 KB] || ligtning_v1_720p.01138_searchweb.png (180x320) [44.9 KB] || ligtning_v1_720p.01138_thm.png (80x40) [3.6 KB] || ligtning_v1_1080p.mp4 (1920x1080) [22.0 MB] || ligtning_v1_720p.mp4 (1280x720) [10.3 MB] || ligtning_v1_720p.webm (1280x720) [4.1 MB] || ", "hits": 189 }, { "id": 11302, "url": "https://svs.gsfc.nasa.gov/11302/", "result_type": "Produced Video", "release_date": "2013-07-12T14:00:00-04:00", "title": "Debris Disks Make Patterns Without Planets", "description": "A study by NASA scientists sounds a cautionary note in interpreting rings and spiral arms as signposts for new planets. Thanks to interactions between gas and dust, a debris disk may, under the right conditions, produce narrow rings on its own, no planets needed.Many young stars known to host planets also possess disks containing dust and icy grains, particles produced by collisions among asteroids and comets also orbiting the star. These debris disks often show sharply defined rings or spiral patterns, features that could signal the presence of orbiting planets. Astronomers study the structures as a way to better understand the physical properties of known planets and possibly uncover new ones. When the mass of gas is roughly equal to the mass of dust, the two interact in a way that leads to clumping in the dust and the formation of patterns. Effectively, the gas shepherds the dust into the kinds of structures astronomers would expect to see if a planet were present.Lyra and Kuchner refer to this as the photoelectric instability and developed a simulation to explore its effects. This animation shows how the process alters the density of dust in a debris disk and rapidly leads to the formation of rings, arcs and oval structures. || ", "hits": 65 }, { "id": 10896, "url": "https://svs.gsfc.nasa.gov/10896/", "result_type": "Produced Video", "release_date": "2012-01-24T00:00:00-05:00", "title": "Bubbles In The Sky", "description": "Ever notice how in many parts of the world, puffy, cauliflower-shaped cumulus clouds are more common in the summer? There's a reason for this: thermal convection. In winter, the sun has less time to heat the surface and cause instability in the atmosphere. But during the summer, heat from the sun warms the land surfaces so much that pockets of hot air—scientists call them thermals—bubble upward much like steam in a pot of boiling water. As the hot air rises, the water vapor trapped within condenses into microscopic cloud droplets. If the air is humid enough, rapidly changing cumulus clouds puff up in the atmosphere, sometimes bulging to heights above 39,000 feet. Watch in the visualizations below—based on a climate model that simulated cloud formation during a Southern Hemisphere summer—how cumulus clouds pop up over the forests of Africa and South America. || ", "hits": 63 }, { "id": 10815, "url": "https://svs.gsfc.nasa.gov/10815/", "result_type": "Produced Video", "release_date": "2011-09-01T00:00:00-04:00", "title": "Surfing Waves On The Sun", "description": "Cue the surfing music. Scientists have spotted the iconic surfer's wave rolling through the atmosphere of the sun. This makes for more than just a nice photo-op: the waves hold clues as to how energy moves through that atmosphere, known as the corona. Since scientists know how these kinds of waves—initiated by a Kelvin-Helmholtz instability if you're being technical—disperse energy in the water, they can use this information to better understand the corona. This in turn, may help solve an enduring mystery of why the corona is thousands of times hotter than originally expected. Seeing the big waves suggests they can cascade down to smaller forms of turbulence too. Scientists believe that the friction created by turbulence—the simple rolling of material over and around itself—could help add heating energy to the corona. Look for the waves rolling around the edges of the expanding dark spots in this visualization from the Solar Dynamics Observatory, captured on April 8, 2010. || ", "hits": 51 }, { "id": 10745, "url": "https://svs.gsfc.nasa.gov/10745/", "result_type": "Produced Video", "release_date": "2011-06-07T09:00:00-04:00", "title": "SDO Catches Surf Waves on the Sun", "description": "Scientists have spotted the iconic surfer's wave rolling through the atmosphere of the sun. This makes for more than just a nice photo-op: the waves hold clues as to how energy moves through that atmosphere, known as the corona. Since scientists know how these kinds of waves — initiated by a Kelvin-Helmholtz instability if you're being technical — disperse energy in the water, they can use this information to better understand the corona. This in turn, may help solve an enduring mystery of why the corona is thousands of times hotter than originally expected.Kelvin-Helmholtz instabilities occur when two fluids of different densities or different speeds flow by each other. In the case of ocean waves, that's the dense water and the lighter air. As they flow past each other, slight ripples can be quickly amplified into the giant waves loved by surfers. In the case of the solar atmosphere, which is made of a very hot and electrically charged gas called plasma, the two flows come from an expanse of plasma erupting off the sun's surface as it passes by plasma that is not erupting. The difference in flow speeds and densities across this boundary sparks the instability that builds into the waves. In order to confirm this description, the team developed a computer model to see what takes place in the region. Their model showed that these conditions could indeed lead to giant surfing waves rolling through the corona. Seeing the big waves suggests they can cascade down to smaller forms of turbulence too. Scientists believe that the friction created by turbulence — the simple rolling of material over and around itself — could help add heating energy to the corona. The analogy is the way froth at the top of a surfing wave provides friction that will heat up the wave. || ", "hits": 29 }, { "id": 20096, "url": "https://svs.gsfc.nasa.gov/20096/", "result_type": "Animation", "release_date": "2007-01-11T00:00:00-05:00", "title": "THEMIS Launch and Deployment", "description": "THEMIS (Time History of Events and Microscale Interactions durind Substorms) answers fundamental outstanding questions regarding the magnetospheric substorm instability, a dominant mechanism of transport and explosive release of solar wind energy within Geospace. THEMIS will elucidate which magnetotail process is responsible for substorm onset at the region where substorm auroras map (~10Re): (i) a local disruption of the plasma sheet current or (ii) that current's interaction with the rapid influx of plasma emanating from lobe flux annihilation at ~25Re. Correlative observations from long-baseline (2-25 Re) probe conjunctions, will delineate the causal relationship and macroscale interaction between the substorm components. THEMIS's five identical probes measure particles and fields on orbits which optimize tail-aligned conjunctions over North America. || ", "hits": 60 }, { "id": 2905, "url": "https://svs.gsfc.nasa.gov/2905/", "result_type": "Visualization", "release_date": "2004-02-12T12:00:00-05:00", "title": "Global Sea Surface Temperature from June, 2002 to September, 2003 (WMS)", "description": "The temperature of the surface of the world's oceans provides a clear indication of the state of the Earth's climate and weather. The AMSR-E instrument on the Aqua satellite measures the temperature of the top 1 millimeter of the ocean every day, even through the clouds. In this visualization sequence covering the period from June, 2002, to September, 2003, the most obvious effects are the north-south movement of warm regions across the equator due to the seasonal movement of the sun and the seasonal advance and retreat of the sea ice near the North and South poles. It is also possible to see the Gulf Stream, the warm river of water that parallels the east coast of the United States before heading towards northern Europe, in this data. Around January 1, 2003, a cooler than normal region of the ocean appears just to the west of Peru as part of a La Niña and flows westward, driven by the trade winds. The waves that appear on the edges of this cooler area are called tropical instability waves and can also be seen in the equatorial Atlantic Ocean about the same time. || ", "hits": 55 }, { "id": 2906, "url": "https://svs.gsfc.nasa.gov/2906/", "result_type": "Visualization", "release_date": "2004-02-12T12:00:00-05:00", "title": "Global Sea Surface Temperature Anomalies from June, 2002 to September, 2003 (WMS)", "description": "The temperature of the surface of the world's oceans provides a clear indication of the state of the Earth's climate and weather. The AMSR-E instrument on the Aqua satellite measures the temperature of the top 1 millimeter of the ocean every day, even through the clouds. If the average sea surface temperature for a particular date is subtracted from the measured temperature for that date, the resulting sea surface temperature anomaly can be used to accurately assess the current state of the oceans. The anomaly can serve as an early warning system for weather phenomena and can be used to indicate forthcoming problems with fish populations and coral reef health. In this visualization of the anomaly covering the period from June, 2002, to September, 2003, the most obvious effects are a successive warming and cooling along the equator to the west of Peru, the signature of an El Niño/La Niña cycle. Around January 1, 2003, a cooler than normal region of the ocean appears in this region as part of a La Niña and flows westward, driven by the trade winds. The waves that appear on the edges of this cooler area are called tropical instability waves. || ", "hits": 17 }, { "id": 2907, "url": "https://svs.gsfc.nasa.gov/2907/", "result_type": "Visualization", "release_date": "2004-02-12T12:00:00-05:00", "title": "Hurricane Regions Indicated by Sea Surface Temperature from June 2002 to September 2003 (WMS)", "description": "The temperature of the world's ocean surface provides a clear indication of the regions where hurricanes and typhoons form, since they can only form when the sea surface temperature exceeds 82 degrees F (27.8 degrees C). The AMSR-E instrument on the Aqua satellite measures the temperature of the top 1 millimeter of the ocean every day, even through the clouds. In this visualization of AMSR-E data covering the period from June, 2002, to September, 2003, areas with surface temperatures greater than 82 degrees F are shown in yellow and orange, while sea surface temperatures below 82 degrees F are shown in blue. The region in the Atlantic from the Caribbean to the equator only exceeds the critical temperature during late summer and early fall in the Northern Hemisphere, the period known as Hurricane Season. It is also possible to see the Gulf Stream, the warm river of water that parallels the east coast of the United States before heading towards northern Europe, in this data. Around January 1, 2003, a cooler than normal region of the ocean appears just to the west of Peru as part of an La Niña and flows westward, driven by the trade winds. The waves that appear on the edges of this cooler area are called tropical instability waves and can also be seen in the equatorial Atlantic Ocean about the same time. || ", "hits": 25 }, { "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": 259 }, { "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": 75 }, { "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": 60 }, { "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": 38 }, { "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": 41 }, { "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": 36 }, { "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": 8 }, { "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": 35 }, { "id": 8, "url": "https://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": 95 }, { "id": 9, "url": "https://svs.gsfc.nasa.gov/9/", "result_type": "Visualization", "release_date": "1993-12-17T12:00:00-05:00", "title": "Topological Features of a Compressible Plasma Vortex Sheet - a Model of the Outer Heliospheric Wind", "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 densityare shown as dark transparent 'tubes'. Critical points of the velocity field are represented by 'Glyphs'. Vortex cores are shown in orange and blue. || ", "hits": 64 } ] }