Formation of the "precessional" spiral wave in the cool accretion disk in semidetached binaries

被引:0
|
作者
Bisikalo, DV [1 ]
Boyarchuk, AA [1 ]
Kaygorodov, PV [1 ]
Kuznetsov, OA [1 ]
Matsuda, T [1 ]
机构
[1] Inst Astron, Moscow 119017, Russia
关键词
binary stars; accretion disk; gas-dynamical modeling;
D O I
暂无
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
We suggest that an additional spiral density wave can exist in the inner parts of the cool accretion disk, where gas-dynamical perturbations are negligible. This spiral wave is due to the retrograde precession of the streamlines in the binary system. The results of a three-dimensional gas-dynamical simulation have shown that a considerable increase in the accretion rate (by an order of magnitude) is associated with the formation of the "precessional" spiral wave. Basing on this fact we suggest a new mechanism for the superoutbursts and superhumps in binaries.
引用
收藏
页码:295 / 300
页数:6
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