Mixing in ejecta of supernovae. II. Mixing width of 2D Rayleigh-Taylor instabilities in the helium star models for type Ib/Ic supernovae

Details Mixing in ejecta of supernovae. II. Mixing width of 2D Rayleigh-Taylor instabilities in the helium star models for type Ib/Ic supernovae Mixing in ejecta of supernovae. II. Mixing width of 2D Rayleigh-Taylor instabilities in the helium star models for type Ib/Ic supernovae

Apr 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994a%26as..104..341h&link_type=abstract

Astronomy and Astrophysics Suppl. 104, 341-364 (1994)

Astronomy and Astrophysics

Astrophysics

21

Hydrodynamics, Instabilities, Stars: Interiors, Supernovae: General

Scientific paper

Nonlinear growth of the Rayleigh-Taylor instabilities in the supernova explosions of 3-6Msun_ helium stars are calculated assuming cylindrical symmetry. In order to make a comparison between the calculated results and the observations of type Ib/Ic supernovae with much less numerical ambiguity, the dependence of the mixing width (the length of the mushroom fingers from the bottom to the top) on the mesh resolution is examined by using four different grid systems of 129 x 129, 257 x 257, 513 x 513, and 1025 x 1025. It is found that when the initial velocity perturbation is relatively large (larger than 1% of the expansion velocity), the mixing width depends hardly on the mesh resolution as far as the number of grids exceeds 500 x 500. These converged values of the mixing width would be useful for comparison with observations. The dependencies of the mixing width on the amplitude and mode of initial perturbations are also examined.

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