Thermally Driven Outflows from Pair-Plasma Pressure Mediated Shock Surfaces around Schwarzschild Black Holes

Abstract

Introducing a spherical, steady, self-supported pair-plasma pressure mediated shock surface around a Schwarzschild black hole as the effective physical atmosphere which may be responsible for the generation of astrophysical mass outflows from relativistic quasi-spherical accretion, we calculate the mass outflow rate $R_{\dot{m}}$ by simultaneously solving the set of equations governing transonic polytropic accretion and isothermal winds. $R_{\dot{m}}$ is computed in terms of {\it only three} inflow parameters, which, as we believe, has been done for the first time in our work. We then study the dependence of $R_{\dot{m}}$ on various inflow as well as shock parameters and establish the fact that the outflow rate is essentially controlled by the post-shock proton temperature.

10 two-column pages. 8 black and white post-script figures. Published in MNRAS

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