Rotating accretion flows around black holes: convection and variability

被引:198
作者
Igumenshchev, IV [1 ]
Abramowicz, MA
机构
[1] Gothenburg Univ, S-41296 Gothenburg, Sweden
[2] Chalmers Univ Technol, S-41296 Gothenburg, Sweden
[3] Astron Inst, Moscow 109017, Russia
[4] NORDITA, DK-2100 Copenhagen 0, Denmark
[5] SISSA, Lab Interdisciplinare, I-34014 Trieste, Italy
[6] ICTP, Trieste, Italy
关键词
accretion; accretion discs; black hole physics; convection; hydrodynamics; instabilities; methods; numerical;
D O I
10.1046/j.1365-8711.1999.02220.x
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
Numerical, two-dimensional, time-dependent hydrodynamical models of geometrically thick accretion discs around black holes are presented. Accretion flows with non-effective radiation cooling (ADAFs) can be both convectively stable or unstable depending on the value of the viscosity parameter alpha. The high-viscosity flows (alpha similar or equal to 1) are stable and have a strong equatorial inflow and bipolar outflows. The low-viscosity flows (alpha less than or similar to 0.1) are convectively unstable and this induces quasi-periodic variability, with typical time-scales in the observed range of quasiperiodic oscillations.
引用
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页码:309 / 320
页数:12
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