Stability of slim, transonic accretion disk models

Details Stability of slim, transonic accretion disk models Stability of slim, transonic accretion disk models

Apr 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991pasj...43..261h&link_type=abstract

Astronomical Society of Japan, Publications (ISSN 0004-6264), vol. 43, no. 2, 1991, p. 261-273. Research supported by Institute

Computer Science

Numerical Analysis

20

Accretion Disks, Black Holes (Astronomy), Neutron Stars, Thermal Stability, Transonic Flow, Computerized Simulation, Numerical Analysis, Radial Distribution, S Curves

Scientific paper

There is a possibility that accretion disks around a neutron star or a black hole show nonlinear oscillations caused by thermal instability, similar to dwarf nova outbursts. In connection with this possibility, the stability of accretion disks with high accretion rates is of importance. For disks with a high accretion rate, the heat is generated by viscosity close to the transonic part of the flow; not only is it locally radiated away, as in the standard Shakura-Sunyaev (1973,1976) model, but also it is very efficiently transported by advection. The stability properties of such slim, transonic accretion disks were examined by means of numerical simulations. The results of simulations suggest that the disks are globally stable. Some possible reasons for the global stability are briefly discussed.

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