Standing Rankine-Hugoniot shocks in accretion and wind flows in Kerr geometry

This paper presents a fully relativistic study on the standing shock formation in thin, stationary, axisymmetric, adiabatic fluid flows in Kerr geometry. We find out the energyangular momentum parameter space for which the flow may develop shocks. The multiplicity of the formal shock location is removed by employing the boundary conditions and stability analysis: the stable shock location is practically unique. The effects of the frame-dragging of a rapid rotating black hole on the shock properties are pointed out. Finally, we discuss the validity of the assumptions made about the flow and conclude that shocks are likely to be common in astrophysical flows.