Mathematical Modeling of the Evolution of Compact Astrophysical Gas Objects

Abstract

In the current study, the vortex structures that occur in one of the most common astrophysical objects such as massive stars and accretion disks are investigated using mathematical modeling methods. Modeling of convective processes with the formation of vortex structures in massive stars of various masses, rotating and being possessed in the self-gravitation conditions is carried out. Modeling uses a gas-dynamic model of an inviscid perfect gas. The numerical technique is based on the finite-difference approximation of the conservation laws for the additive characteristics of the environment for a finite volume. Direct calculation of gravitational forces is used by summing up the interaction between all the finite volumes in the area of integration. For the objects with different mass and rotation speed, visualized pictures of the vortex structure are given. Modeling of the processes of formation of large-scale vortex structures in accretionary stellar disks with different disk thickness is also carried out. Self-gravitation of the matter of a disk rotating in the field of the gravity of a compact central object is not taken into consideration. The numerical technique is based on the explicit, conservative, and monotone in the linear approximation Godunov-type Roe-Einfeldt-Osher scheme, which approximates with order no higher than the third the conservation laws of the characteristics of the environment. For the disks with different thicknesses, visualized pictures of the vortex structure are given. Evolutionary calculations are carried out on the basis of parallel algorithms implemented on the computational complex of the cluster architecture.