RADIATING BONDI AND COOLING SITE FLOWS

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 th...

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Published inThe Astrophysical journal Vol. 754; no. 2; pp. 1 - 7
Main Authors MATHEWS, William G, FULAI GUO
Format Journal Article
LanguageEnglish
Published Bristol IOP 01.08.2012
Subjects
Accretion
ACCRETION DISKS
ASTRONOMY
ASTROPHYSICS
ASTROPHYSICS, COSMOLOGY AND ASTRONOMY
BLACK HOLES
Bonding
COOLING
Earth, ocean, space
Exact sciences and technology
Galactic clusters
GALAXIES
GALAXY CLUSTERS
Gas temperature
Gravitation
MAGNETOHYDRODYNAMICS
MASS
Mathematical analysis
MORPHOLOGY
Sonics
Magnetohydrodynamics
Accretion
Black holes
accretion, accretion disks
Accretion rate
Cooling flow
hydrodynamics
Accretion disks
Galaxy clusters
Point mass
black hole physics
Gas flow
Morphology
Cosmology
Galaxy groups
magnetohydrodynamics (MHD)
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Summary: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 M/MT sub(s) where T sub(s) is the gas temperature at the sonic point. In radiating Bondi flows the relationship between the mass accretion rate and central mass, M [is proportional to] M super(p) with p ~ 1, differs significantly from the quadratic dependence in classical Bondi flows, M [is proportional to] M super(2). Mass accretion rates onto galaxy or cluster-centered 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.
Bibliography:ObjectType-Article-1
SourceType-Scholarly Journals-1
ObjectType-Feature-2
content type line 23
ISSN:0004-637X
1538-4357
DOI:10.1088/0004-637X/754/2/154