Rotational Instability in Supersonic Accretion Flows

Details Rotational Instability in Supersonic Accretion Flows Rotational Instability in Supersonic Accretion Flows

Jan 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008aipc..968..420l&link_type=abstract

ASTROPHYSICS OF COMPACT OBJECTS: International Conference on Astrophysics of Compact Objects. AIP Conference Proceedings, Volum

Astronomy and Astrophysics

Astrophysics

Accretion And Accretion Disks, Planetary Bow Shocks, Interplanetary Shocks, Black Holes

Scientific paper

We studied the structure formed around black holes as a consequence of one-dimensional, quasi-spherical, supersonic accretion flows. The structure accompanies an accretion shock, inside which the flow is subsonic and is dissipated by viscosity. We found that the viscous angular momentum transfer induces ∂l/∂r<0 close to the accretion shock, where l is the specific angular momentum and r is the radius from the black hole. Hence, the flow there is subject to rotational instability.

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