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research
Counter-rotating Accretion Disks
Authors
R. V. E. Lovelace
Ray T. P.
+3Â more
Shakura N. I.
Shakura N. I.
Tom Chou
Publication date
1 January 1996
Publisher
'University of Chicago Press'
Doi
Cite
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on
arXiv
Abstract
We consider accretion disks consisting of counter-rotating gaseous components with an intervening shear layer. Configurations of this type may arise from the accretion of newly supplied counter-rotating gas onto an existing co-rotating gas disk. For simplicity we consider the case where the gas well above the disk midplane is rotating with angular rate
+
Ω
+\Omega
+
Ω
and that well below has the same properties but is rotating with rate
−
Ω
-\Omega
−
Ω
. Using the Shakura-Sunyaev alpha turbulence model, we find self-similar solutions where a thin (relative to the full disk thickness) equatorial layer accretes very rapidly, essentially at free-fall speed. As a result the accretion speed is much larger than it would be for an alpha disk rotating in one direction. Counter-rotating accretion disks may be a transient stage in the formation of counter-rotating galaxies and in the accretion of matter onto compact objects.Comment: 7 pages, 3 figures, aas2pp4.sty, submitted to Ap
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Last time updated on 01/04/2019