Hydrodynamics of the Stream-Disk Impact in Interacting Binaries
Hydrodynamics of the Stream-Disk Impact in Interacting Binaries
复制标题
相互作用双星中流-盘撞击的流体动力学
DOI：
10.1086/305149
复制
发表时间：
1997
期刊：
影响因子：
--
通讯作者：
M. Livio
中科院分区：
文献类型：
--
作者：
P. Armitage;M. Livio
我们使用流体动力学模拟提供定量估计的影响，吸积流的磁盘上的相互作用的双星。对于低吸积率，有效的辐射冷却的热点区域可以发生，流的影响的主要后果是流溢出朝向较小的磁盘半径。流很好地描述了弹道轨迹，但更大的气体质量被扫起，并以较小的速度溢出，但仍然是高度超音速。如果冷却效率低，仍然会发生溢流，但盘缘内部没有相干流。定性地，所产生的结构表现为沿沿着盘缘向下游延伸的凸起。我们计算的溢出组件的质量分数和速度作为重要的系统参数的函数，并讨论了X射线观测和多普勒层析成像的灾难性的变量，低质量的X射线双星，超软X射线源的结果的影响。
We use hydrodynamic simulations to provide quantitative estimates of the effects of the impact of the accretion stream on disks in interacting binaries. For low accretion rates, efficient radiative cooling of the hotspot region can occur, and the primary consequence of the stream impact is stream overflow toward smaller disk radii. The stream is well described by a ballistic trajectory, but larger masses of gas are swept up and overflow at smaller, but still highly supersonic, velocities. If cooling is inefficient, overflow still occurs, but there is no coherent stream inward of the disk rim. Qualitatively, the resulting structure appears as a bulge extending downstream along the disk rim. We calculate the mass fraction and velocity of the overflowing component as a function of the important system parameters, and discuss the implications of the results for X-ray observations and Doppler tomography of cataclysmic variables, low-mass X-ray binaries, and supersoft X-ray sources.