Hydrodynamics of Accretion onto Black Holes

Spherical and axisymmetric accretion onto black holes is discussed. Physical processes in various families of solutions are explained and their characteristics are summarized. Recently discovered solutions of axisymmetric flow provide us with various radiation efficiency and spectrum, which may successfully model diverse accretion systems. Possible role of preheating is also speculated. The various families of solutions can be plotted as trajectories on the plane of (l, e) [or (l, ṁ)] where l is the luminosity in units of the Eddington luminosity, ṁ is the similarly defined mass accretion rate and e is the efficiency defined by e ≡ L/Ṁc = l/ṁ. We discuss the domains on these planes where solutions are known or expected to be unstable to either spherical or non-spherical perturbations. Preliminary analysis indicates that a preheating instability will occur along the polar direction of the advection dominated flow for e >∼ 10−2.