M. Park, and J. Ostriker. (1998)cite arxiv:astro-ph/9811048
Comment: Figs 1 and 2 replaced with corrected figures. 9 pages, 3 Postscript
figures. Plain tex. Review talk presented at 31st COSPAR meeting (1996).
Revised version will appear in Adv. in Space Research.
Abstract
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 10^-2.
cite arxiv:astro-ph/9811048
Comment: Figs 1 and 2 replaced with corrected figures. 9 pages, 3 Postscript
figures. Plain tex. Review talk presented at 31st COSPAR meeting (1996).
Revised version will appear in Adv. in Space Research
%0 Generic
%1 Park1998
%A Park, Myeong-Gu
%A Ostriker, Jeremiah P.
%D 1998
%K Accretion Black Hole
%T Hydrodynamics of Accretion onto Black Holes
%U http://arxiv.org/abs/astro-ph/9811048
%X 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 10^-2.
@misc{Park1998,
abstract = { 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}.
},
added-at = {2009-06-08T15:57:58.000+0200},
author = {Park, Myeong-Gu and Ostriker, Jeremiah P.},
biburl = {https://www.bibsonomy.org/bibtex/25477dfb1a1dcf2279aaa12393c33031f/ad4},
description = {Hydrodynamics of Accretion onto Black Holes},
interhash = {f8942b5cf45d3dc34edf82e5c027db5e},
intrahash = {5477dfb1a1dcf2279aaa12393c33031f},
keywords = {Accretion Black Hole},
note = {cite arxiv:astro-ph/9811048
Comment: Figs 1 and 2 replaced with corrected figures. 9 pages, 3 Postscript
figures. Plain tex. Review talk presented at 31st COSPAR meeting (1996).
Revised version will appear in Adv. in Space Research},
timestamp = {2009-06-08T15:57:58.000+0200},
title = {{H}ydrodynamics of {A}ccretion onto {B}lack {H}oles},
url = {http://arxiv.org/abs/astro-ph/9811048},
year = 1998
}