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 that may be responsible for the generation of astrophysical mass outflows from relativistic quasi-spherical accretion, we calculate the mass outflow rate R _̇ by simultaneously solving the set of equations governing transonic polytropic accretion and isothermal winds. R _̇ is computed in terms of only three inflow parameters, which, we believe, has been done for the first time in our work. We then study the dependence of R _̇ 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.