On the Occurrence of Stream Overflow in Cataclysmic Variables with Accretion Disks
On the Occurrence of Stream Overflow in Cataclysmic Variables with Accretion Disks
复制标题
吸积盘灾变变量中流溢出的发生
DOI：
10.1086/306621
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发表时间：
1999
期刊：
影响因子：
--
通讯作者：
F. Hessman
中科院分区：
文献类型：
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作者：
F. Hessman
在激变变数中，我考虑了吸积流物质流过吸积盘边缘的情况。如果来自次星的流比吸积盘的边缘在几何上更厚，那么一部分流物质就可以在吸积盘的上方和下方流动。α模型盘的垂直结构计算结果表明，溢出量是盘的一般热状态(例如，冷的和光学厚的或热的和光的薄的)的敏感函数，而不是盘粘度参数α的值，也可能不是盘半径(即轨道周期)的值。利用质量传输率和研究系统的轨道参数，我估计了一些单独天体的溢出量，并表明观测上显著的溢流量应该主要发生在具有冷外盘的静止的矮新星中。
I consider the occurrence of the flow of accretion stream material past the edge of an accretion disk in cataclysmic variables. If the stream from the secondary star is geometrically thicker than the rim of the accretion disk, some fraction of the stream material can flow over and under the disk. The results of vertical-structure calculations for α-model disks indicate that the amount of overflow is a sensitive function of the general thermal state of the disk (e.g., cold and optically thick or warm and optically thin) but not of the value of the disk viscosity parameter α and probably not of the disk radius (i.e., the orbital period). Using the mass-transfer rates and the orbital parameters of well-studied systems, I estimate the amount of overflow for a number of individual objects and show that observationally significant stream overflow should mainly occur in quiescent dwarf novae with cold outer disks.