Radiating Bondi and Cooling Site Flows
Abstract
Steady accretion of a radiating gas onto a central mass point is described and compared to classic Bondi accretion. Radiation losses are essential for accretion flows to be observed. Unlike Bondi flows, radiating Bondi flows pass through a sonic point at a finite radius and become supersonic near the center. The morphology of all radiating flows is described by a single dimensionless parameter proportional to {\dot{M}}/MT_s where T_{s} is the gas temperature at the sonic point. In radiating Bondi flows the relationship between the mass accretion rate and central mass, {\dot{M}} \propto M^p with p ~ 1, differs significantly from the quadratic dependence in classical Bondi flows, {\dot{M}} \propto M^2. Mass accretion rates onto galaxy or clustercentered black holes estimated from traditional and radiating Bondi flows are significantly different. In radiating Bondi flows the gas temperature increases at large radii, as in the cores of many galaxy groups and clusters, allowing radiating Bondi flows to merge naturally with gas arriving from their cluster environments. Some radiating flows cool completely before reaching the center of the flow, and this also occurs in cooling site flows, in which there is no central gravitating mass.
 Publication:

The Astrophysical Journal
 Pub Date:
 August 2012
 DOI:
 10.1088/0004637X/754/2/154
 arXiv:
 arXiv:1206.4585
 Bibcode:
 2012ApJ...754..154M
 Keywords:

 accretion;
 accretion disks;
 black hole physics;
 hydrodynamics;
 magnetohydrodynamics: MHD;
 Astrophysics  Cosmology and Nongalactic Astrophysics
 EPrint:
 9 pages with 3 figures