Modeling of stellar wind from fast rotating stars

Abstract

Two-dimensional (2D) axisymmetric hydrodynamic model for the stellar wind outflow from a fast rotating star is created. Nonuniform distribution of the pressure over the surface of the star corresponding to the condition of equilibrium in every point of plasma in the gravitational and centrifugal fields is taken into account. We also take into account the turbulence of the flow excited in the wind at Reynolds numbers [Formula: see text]. Calculations show the formation of the disklike outflow from the surface of the star at the equator which rather quickly (on the scale of the order of the radius of the star) expands into polar regions. Huge vertex is formed at high latitudes where high level of turbulence makes possible efficient diffusion of the angular moment. At the same time the turbulence is not excited at the equator. This prevents formation of the large scale disklike outflow at the equatorial plane. Dependence of the mass flux outflow on the velocity of the star rotation is obtained.