Three Dimensional Numerical Modelling of Convective Instability by Supernova Explosion with Nested Grids Scheme on Multiprocessors Systems

We carried out three dimensional hydrodynamical simulations to study development large scale convective inst ability into a protoneutron st ar by supernova expolsion II type. The initial st at e is rot ating protoneutron st ar with excess ent ropy at the cent re. On the last stage of collapse of the iron core of a star the proc ess of nonequilibrium neutronization of matter provides high ent ropy and great mean energy of th e neutrinos in the central part of the protoneutron star. The hydrodynamically unstable configurat ion of a protoneutron star is formed. The st at ement of th e problem consist s in studing the development of the nonuniformity scale of the entropy distribution. The cent ral density and central temperat ure was t aken to be ρ = 1014g/cm3 and T =1011 K. On the boundary of numerical region we keep initi al equilibrium values of all vari ables. The weak solid-body rot ation of protoneutron star was t aken into account, with the ratio of the rot ational kinetic energy T to the gravitat ional energy |W| being T|W| = 0.01. The coordinate system was chosen so that the plane of rot ation of the star coinced with the xy plane. It was assumed that relativistic degenerate electrons and an ideal nonr elativist ic Fermi gas of nucleons contribute to the equat ion of a state of substance inside the star. The excess ent ropy was produced close to the center of the star and had funct ional form S =S 0 +(S ′ − S 0)exp {−|r − r 0|/|b|}, S ′ = 3S 0 and r 0 =0.