Rotational Instability in Supersonic Accretion Flows
We studied the structure formed around black holes as a consequence of one-dimensional, quasi-spherical, supersonic accretion flows. The structure accompanies an accretion shock, inside which the flow is subsonic and is dissipated by viscosity. We found that the viscous angular momentum transfer induces ? l/ ?r<0 close to the accretion shock, where/ is the specific angular momentum and r is the radius from the black hole. Hence, the flow there is subject to rotational instability.
accretion accretion disks instabilities
Seong-Jae Lee Dongsu Ryu
Department of Astronomy and Space Science, Chungnam National University, Republic of South Korea
国际会议
紧凑型物体的天体物理学国际会议(International Conference on Astrophysics of Compact Objects)
安徽黄山
英文
420-422
2007-07-01(万方平台首次上网日期,不代表论文的发表时间)