Three-Dimensional Simulation of Supernova Explosion and Growth of Instabilities

Abstract

From the observational results of supernova 1987A and its interpretation, mixing in the ejecta becomes more and more important. Some group have already performed two dimensional and three dimensional numerical simulation of supernova explosion and analyze the instability of the ejecta. Two dimensional mesh calculation is done by Dr. D. Arnett and Dr. B. Fryxell. They showed that instability occurs at near the density gap and mushroom like pattern is formed. Three dimensional mesh calculation is done by Dr. E. Müller et al. and our group. Dr. Müller et al. show that there is not enough time for evolving the instability to sufficiently large in the case of N=3 poly tropic star. In our simulation, number of meshes is twice in each direction as large as Dr. Muller’s. The results of N=3 star is essentially the same as them. SPH approach is done by Dr. M. Nagasawa et al. They showed that in the N=3 model Rayleigh-Taylor instability grows up to nonlinear stage and expanding shell fragments. Dr. W. Benz and Dr. F. Thielemann also performed three dimensional computation by SPH code.