Dynamics of the transition from a thin accretion disk to an advection-dominated accretion flow

被引:37
作者
Manmoto, T [1 ]
Kato, S
Nakamura, KE
Narayan, R
机构
[1] Univ Calif Santa Barbara, Inst Theoret Phys, Santa Barbara, CA 93106 USA
[2] Nara Sangyo Univ, Sango, Nara 6308503, Japan
[3] Kyoto Univ, Dept Astron, Sakyo Ku, Kyoto 6068502, Japan
[4] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA
关键词
accretion; accretion disks; black hole physics; hydrodynamics; turbulence;
D O I
10.1086/308273
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
We consider an optically thin advection-dominated accretion flow (ADAF) that is connected at a finite transition radius to an outer optically thick, geometrically thin disk. We include turbulent energy transport and examine ADAF models that satisfy the following boundary conditions at the transition radius: (1) the temperature of the gas is much lower than the virial temperature, (2) the rotation is super-Keplerian, and (3) the net radial flux of energy is outward. We numerically solve the height-integrated viscous hydrodynamic equations with these boundary conditions. We find that the Bernoulli parameter is positive for a wide range of radius, indicating that outflows may be possible from ADAFs. Turbulent energy transport enhances the Bernoulli parameter. We compare our numerical global solutions with two published analytical solutions. We find that the solution of Honma represents the transition region well, while the self-similar solution of Narayan & Yi works better away from the transition. However, neither analytical solution is able to represent the density or angular momentum profile in the inner region of the ADAF, where the flow makes a sonic transition.
引用
收藏
页码:127 / 137
页数:11
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