Advection-dominated accretion flows in the Kerr metric. II. Steady state global solutions

In a previous paper, we have written equations describing steady state, optically thin, advection-dominated accretion onto a Kerr black hole. In this paper, we survey the numerical solutions to these equations. We find that the temperature and density of the gas in the inner part of the accretion how depend strongly on the black hole spin parameter a. The rate of angular momentum accretion is also shown to depend on a; for a greater than an equilibrium spin parameter a(eq), the black hole is de-spun by the accretion how. We also investigate the dependence of the how on the angular momentum transport efficiency alpha, the advected fraction of the dissipated energy f, and the adiabatic index gamma. We find solutions for -1 < a < 1, 10(-4) less than or equal to alpha less than or equal to 0.44, 0.01 less than or equal to f less than or equal to 1, and 4/3 < gamma < 5/3. For low values of alpha and f, the inner part of the flow exhibits a pressure maximum and appears similar to equilibrium thick disk solutions.