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

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.