Astronomy and Astrophysics – Astronomy
Scientific paper
Feb 1991
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991pasj...43..147h&link_type=abstract
Astronomical Society of Japan, Publications (ISSN 0004-6264), vol. 43, no. 1, 1991, p. 147-168. Research supported by Institute
Astronomy and Astrophysics
Astronomy
114
Accretion Disks, Black Holes (Astronomy), Neutron Stars, Stellar Mass Accretion, Oscillations, Stellar Models, Thermal Stability
Scientific paper
Numerical simulations were performed in order to examine the time evolution of thermally unstable accretion disks which surround a black hole or a weakly magnetized neutron star. Optically thick, slim transonic accretion disk models are used. The radial-azimuthal component of a viscous stress tensor is assumed to have the form -alpha(beta exp q)P, where beta is the ratio of the gas pressure to the total pressure, P, with constants alpha and q. Three cases (q = 0, 0.25, and 0.5) are examined. For q = 0, the disks exhibit burstlike oscillations. For q = 0.25, in comparison with the case of q = 0, the amplitude of the oscillations is much smaller and their period much shorter. For q = 0.5, the disks are stable.
Honma Fumio
Kato Shoji
Matsumoto Ryoji
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