A 15.65-solar-mass black hole in an eclipsing binary in the nearby spiral galaxy M 33
A 15.65-solar-mass black hole in an eclipsing binary in the nearby spiral galaxy M 33
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DOI：
10.1038/nature06218
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发表时间：
2007-10
期刊：
影响因子：
64.8
通讯作者：
J. Orosz;J. McClintock;R. Narayan;C. Bailyn;J. Hartman;L. Macri;Jiefeng Liu;W. Pietsch;R. Remill
中科院分区：
文献类型：
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作者：
J. Orosz;J. McClintock;R. Narayan;C. Bailyn;J. Hartman;L. Macri;Jiefeng Liu;W. Pietsch;R. Remill
恒星质量的黑洞是在x射线发射的双星系统中发现的，它们的质量可以从伴星的动力学来确定。恒星演化模型很难在质量超过太阳十倍的近距离双星中产生黑洞（bbb10；参考文献），这与迄今为止已知的质量最大的恒星黑洞的质量都在一个标准差10以内的事实是一致的。在这里，我们报告了最近发现的m33 X-7系统中黑洞的质量为（15.65±1.45），该系统位于邻近的梅西耶33星系（m33）中，是唯一已知的位于食双星中的黑洞。为了产生如此巨大的黑洞，在核心的氦聚变完成之前，祖恒星必须保留其外层的大部分。另一方面，为了使黑洞在目前3.45天的轨道上围绕它的（70.0±6.9）伴星运行，必须有一个“共同包络”的进化阶段，在这个阶段，系统失去了大量的质量。我们发现，在M 33 X-7中不可能发生常见的包层阶段，除非在其演化过程中从其祖先那里损失的质量比通常在大质量恒星演化模型中假设的要少一个数量级。
Stellar-mass black holes are found in X-ray-emitting binary systems, where their mass can be determined from the dynamics of their companion stars,,. Models of stellar evolution have difficulty producing black holes in close binaries with masses more than ten times that of the Sun (> 10; ref.), which is consistent with the fact that the most massive stellar black holes known so far, all have masses within one standard deviation of 10. Here we report a mass of (15.65±1.45) for the black hole in the recently discovered system M 33 X-7, which is located in the nearby galaxy Messier 33 (M 33) and is the only known black hole that is in an eclipsing binary. To produce such a massive black hole, the progenitor star must have retained much of its outer envelope until after helium fusion in the core was completed. On the other hand, in order for the black hole to be in its present 3.45-day orbit about its (70.0±6.9) companion, there must have been a ‘common envelope’phase of evolution in which a significant amount of mass was lost from the system. We find that the common envelope phase could not have occurred in M 33 X-7 unless the amount of mass lost from the progenitor during its evolution was an order of magnitude less than what is usually assumed in evolutionary models of massive stars,,.