Computation of Mass Outflow Rate from Relativistic Quasi-Spherical Accretion onto Black Holes

We compute mass outflow rate $R_{\dot m}$ from relativistic matter accreting quasi-spherically onto Schwarzschild black holes. Taking the pair-plasma pressure mediated shock surface as the {\it effective} boundary layer (of the black hole) from where bulk of the outflow is assumed to be generated, computation of this rate is done using combinations of exact transonic inflow and outflow solutions. We find that $R_{\dot m}$ depends on the initial parameters of the flow, the polytropic index of matter, the degree of compression of matter near the shock surface and on the location of the shock surface itself. We thus not only study the variation of the mass outflow rate as a function of various physical parameters governing the problem but also provide a sufficiently plausible estimation of this rate.