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Rayleigh-Taylor Instabilities in Supernovae Explosions: Density
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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.
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Evolution of the density in a supernova explosion, in both a fixed reference frame and in the blast wave reference frame
Duration: 15.0 seconds
Available formats:
352x240 (29.97 fps)
MPEG-1
2 MB
160x80
PNG
29 KB
80x40
PNG
9 KB
320x238
JPEG
5 KB
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| Animation Number: | 39 |
| Animators: | Bruce Fryxell (Lead) |
| | Pamela ONeil |
| Studio: | SVS |
| Completed: | 1994-02-12 |
| Scientists: | Bruce Fryxell (University of Arizona) |
| | Ewald Muller (Max Planck) |
| | Dave Arnett (University of Arizona) |
| Series: | Supernovae Instabilities |
| Video: | SVS1994-0006 * |
Keywords:
SVS
>> Rayleigh-Taylor
DLESE
>> Space science
SVS
>> Supernovae
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| Science paper: | Fryxell, B. A., Muller, E., and Arnett, D., 1989, Hydrodynamics and Nuclear Burning (MPI Astrophys. Rep. 449; Garching: MPI Astrophys) |
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Please give credit for this item to
NASA/Goddard Space Flight Center
Scientific Visualization Studio |
*Please note: the SVS does not fulfill requests for copies of the tapes in our library. On some of our animation pages, there is a direct link to a video distribution service from which tapes, handled by the Public Affairs Office (PAO)/Goddard TV, including some of our animations may be ordered. General information on this service can be found here. |
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