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

来源：

Interacting Binaries: Accretion, Evolution, and Outcomes | 2005年 / 797卷

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

页码：295 / 300

页数：6

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