Accretion powered spherical wind in general relativity

Using full general relativistic calculations, we investigate the possibilit y of generation of mass out ow from spherical accretion onto non-rotating b lack holes. Introducing a relativistic hadronic-pressure-supported steady, standing, spherically-symmetric shock surface around a Schwarzschild black hole as the effective physical barrier that may be responsible for the gene ration of spherical wind, we calculate the mass out ow rate R-(m) over dot in terms of three accretion parameters and one out ow parameter by simultan eously solving the set of general relativistic hydrodynamic equations descr ibing spherically symmetric, transonic, polytropic accretion and wind aroun d a Schwarzschild black hole. Not only do we provide a sufficiently plausib le estimation of R-(m) over dot, we also successfully study the dependence and variation of this rate on various physical parameters governing the ow. Our calculation indicates that independent of initial boundary conditions, the baryonic matter content of this shock-generated wind always correlates with post-shock ow temperature.