Mixing in ejecta of supernovae. I - General properties of two-dimensional Rayleigh-Taylor instabilities and mixing width in ejecta of supernovae

Details Mixing in ejecta of supernovae. I - General properties of two-dimensional Rayleigh-Taylor instabilities and mixing width in ejecta of supernovae Mixing in ejecta of supernovae. I - General properties of two-dimensional Rayleigh-Taylor instabilities and mixing width in ejecta of supernovae

May 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992apj...390..230h&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 390, no. 1, May 1, 1992, p. 230-252. Research supported by Institute of Spa

Statistics

Computation

40

Ejecta, Hydrodynamics, Stellar Interiors, Supernova 1987A, Taylor Instability, Computational Astrophysics, Mixing, Scaling Laws

Scientific paper

Nonlinear growth of 2D Rayleigh-Taylor (R-T) instabilities are numerically studied to apply to the mixing in the supernova ejecta. Highly refined calculations of mixing in the realistic model of SN 1987A with a better code and various mesh resolutions are presented. It is shown that mixing width (or the extent of mixing) due to Rayleigh-Taylor instabilities is still too small to account for the observations even with relatively large initial perturbation. The mixing width is found to depend only slightly on the mesh resolution when the initial amplitude is larger than about 5 percent of the expansion speed. To clarify the basic properties of the R-T instabilities and the dependence of the mixing width on the initial density structure, initial perturbation, and numerical resolution, highly simplified ideal models of R-T instabilities of compressible gas with an adiabatic constant of 4/3 are considered. It is found that, when the initial amplitude of the velocity perturbation is larger than 1 percent of the sound speed, the mixing width in time depends mainly on the initial amplitudes and the density ratio.

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