| Issue |
A&A
Volume 608, December 2017
|
|
|---|---|---|
| Article Number | A114 | |
| Number of page(s) | 7 | |
| Section | Astrophysical processes | |
| DOI | https://doi.org/10.1051/0004-6361/201730803 | |
| Published online | 13 December 2017 | |
Hot accretion flow with anisotropic viscosity
1 Key Laboratory for Research in Galaxies and Cosmology, Shanghai Astronomical Observatory, Chinese Academy of Sciences, 80 Nandan Road, 200030 Shanghai, PR China
e-mail: mcwu@shao.ac.cn; dfbu@shao.ac.cn
2 Key Laboratory for Research in Galaxies and Cosmology, Department of Astronomy, University of Science and Technology of China, Hefei, 230026 Anhui, PR China
Received: 17 March 2017
Accepted: 16 September 2017
In extremely low accretion rate systems, the ion mean-free path can be much larger than the gyroradius. Therefore, gas pressure is anisotropic with respect to magnetic field lines. The effects of pressure anisotropy can be modeled by an anisotropic viscosity with respect to magnetic field lines. Angular momentum can be transferred by anisotropic viscosity. In this paper, we investigate hot accretion flow with anisotropic viscosity. We consider the case that anisotropic viscous stress is much larger than Maxwell stress. We find that the flow is convectively unstable. We also find that the mass inflow rate decreases towards a black hole. Wind is very weak; its mass flux is 10−15% of the mass inflow rate. The inward decrease of inflow rate is mainly due to convective motions. This result may be useful to understand the accretion flow in the Galactic Center Sgr A* and M 87 galaxy.
Key words: accretion, accretion disks / black hole physics / hydrodynamics / ISM: jets and outflows / conduction
© ESO, 2017
Open Access article, published by EDP Sciences, under the terms of the Creative Commons Attribution License (http://creativecommons.org/licenses/by/4.0),
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