Hydrodynamics of Accretion onto Black Holes

Details Hydrodynamics of Accretion onto Black Holes Hydrodynamics of Accretion onto Black Holes

1998-11-03

arxiv.org/abs/astro-ph/9811048v2

Astronomy and Astrophysics

Astrophysics

Figs 1 & 2 replaced with corrected figures. 9 pages, 3 Postscript figures. Plain tex. Review talk presented at 31st COSPAR mee

Scientific paper

10.1016/S0273-1177(98)00127-6

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,dot m)] where l is the luminosity in units of the Eddington luminosity, dot m is the similarly defined mass accretion rate and e is the efficiency defined by e equiv L/dot M c^2 = l/dot m. We discuss the domains on these planes where solutions are known or expected to be unstable to either spherical or on-spherical perturbations. Preliminary analysis indicates that a preheating instability will occur along the polar direction of the advection dominated flow for e \gsim 10^{-2}.

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