Inventory of Black Hole Binaries
Inventory of Black Hole Binaries
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黑洞双星盘点
DOI：
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发表时间：
2002
期刊：
影响因子：
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通讯作者：
J. Orosz
中科院分区：
文献类型：
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作者：
K. A. van der Hucht;A. Herrero;C Esteban;Eds;J. Orosz
一小组x射线双星目前为恒星质量黑洞的存在提供了最好的证据。这些物体是相互作用的双星系统，其中x射线是由物质吸积到致密物体（即半径小于几百公里的物体）上产生的。在一些有利的情况下，对伴星的光学研究导致对两个组成部分的动态质量估计。在17个案例中，x射线双星的致密物体的质量已被证明超过了稳定中子星的最大质量（约3 M⊙），这导致了这些物体是黑洞的结论。在这篇文章中，我将回顾这些黑洞双星的基本性质。黑洞是爱因斯坦广义相对论的一种极端表现。作为一名观测天文学家，我将不考虑任何关于黑洞的详细理论，而只考虑如何找到黑洞的实际问题。通常的方法是通过消去过程。在当前的宇宙中，黑洞必须通过垂死恒星的引力坍缩而形成。根据简并核心的质量不同，有三种可能的结果：白矮星、中子星或黑洞。白矮星的质量不能超过众所周知的钱德拉塞卡极限，中子星也有类似的质量上限，通常被认为大约是3 M⊙(Rhoades & Ruffini 1974; Kalogera & Baym 1996)。一旦简并核心的质量超过约3 M⊙，任何已知的力都无法阻止引力坍缩，黑洞必然形成。考虑到这一点，我们对黑洞有了一个相对直接的观测定义：黑洞是一个质量大于三个太阳质量的致密物体，这里的“致密”是指半径小于100公里的物体（即远小于正常恒星的半径）。由于黑洞是黑暗的，人们唯一希望观察它们的方法就是通过它们对周围物质的引力影响。早期试图搜索双星的星表，寻找具有大质量和未被发现的伴星的单行双星，但没有成功（Zel'dovich & Guseynov 1966; Trimble & Thorne 1969）。一种更有效的资源选择方法起源于20世纪60年代，当时……
A small group of X-ray binaries currently provides the best evidence for the existence of stellar-mass black holes. These objects are interacting binary systems where the X-rays arise from accretion of material onto a compact object (i.e. an object with a radius of less than a few hundred km). In some favourable cases, optical studies of the companion star lead to dynamical mass estimates for both components. In 17 cases, the mass of the compact object an X-ray binary has been shown to exceed the maximum mass of a stable neutron star (about 3 M ⊙), which leads to the conclusion that these objects are black holes. In this contribution I will review the basic properties of these black hole binaries. Black holes represent an extreme manifestation of Einstein's theory of general relativity. As an observational astronomer, I will not consider any of the detailed theory of black holes but will instead consider only the practical question of how to find them. The usual route is by the process of elimination. In the current universe, black holes must form via the gravitational collapse of a dying star. Three outcomes are possible, depending on the mass of the degenerate core: a white dwarf, a neutron star, or a black hole. The mass of a white dwarf cannot exceed the well-known Chandrasekhar limit, and a neutron star has a somewhat analogous upper mass limit, generally thought to be on the order of 3 M ⊙ (Rhoades & Ruffini 1974; Kalogera & Baym 1996). Once the mass of the degenerate core exceeds about 3 M ⊙ , no known force can halt the gravitational collapse, and a black hole must be formed. Given this, we have a relatively straightforward observational definition of a black hole: A black hole is a compact object with a mass greater than three solar masses, where " compact " in this context means an object with a radius smaller than about 100 km (i.e. much less than the radius of normal stars). Since black holes are dark, the only way one could hope to observe them is through their gravitational influence on surrounding matter. Early attempts to search catalogs of spectroscopic binaries to look for single-lined binaries with massive and undetected companions were not successful (Zel'dovich & Guseynov 1966; Trimble & Thorne 1969). A far more efficient approach for source selection has its roots in the 1960s when …