  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.
