Simulating black hole white dwarf encounters
Simulating black hole white dwarf encounters
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模拟黑洞与白矮星的相遇
DOI：
10.1016/j.cpc.2008.01.031
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发表时间：
2008
期刊：
影响因子：
--
通讯作者：
Marius Dan
中科院分区：
文献类型：
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作者：
S. Rosswog;E. Ramirez;W. Hix;Marius Dan
潜伏在星系中心的超大质量黑洞和含有几个太阳质量的黑洞的恒星双星系统的存在已经毫无疑问地确定了。近年来，球状星星团中可能存在中等质量（1000 M）的黑洞的观点越来越受到人们的信任，但还没有确凿的证据。这一假说的一个吸引人的特点是不仅有可能破坏太阳型恒星，而且有可能破坏致密的白色矮星。在近距离的碰撞中，白色矮星可以被充分压缩而发生热核爆炸。伴随着柔和的瞬态X射线信号的暗热核爆炸的探测将是星团中存在中等质量黑洞的有力证据。在本文中，我们专注于用于模拟整个中断过程的数值技术，从初始的抛物线轨道，在潮汐压缩过程中的核能释放，随后的喷射新鲜合成的材料和黑洞周围的吸积盘的形成过程。
The existence of supermassive black holes lurking in the centers of galaxies and of stellar binary systems containing a black hole with a few solar masses has been established beyond reasonable doubt. The idea that black holes of intermediate masses (∼1000M⊙) may exist in globular star clusters has gained credence over recent years but no conclusive evidence has been established yet. An attractive feature of this hypothesis is the potential to not only disrupt solar-type stars but also compact white dwarf stars. In close encounters the white dwarfs can be sufficiently compressed to thermonuclearly explode. The detection of an underluminous thermonuclear explosion accompanied by a soft, transient X-ray signal would be compelling evidence for the presence of intermediate mass black holes in stellar clusters. In this paper we focus on the numerical techniques used to simulate the entire disruption process from the initial parabolic orbit, over the nuclear energy release during tidal compression, the subsequent ejection of freshly synthesized material and the formation process of an accretion disk around the black hole.