THE FORMATION AND GRAVITATIONAL-WAVE DETECTION OF MASSIVE STELLAR BLACK HOLE BINARIES
THE FORMATION AND GRAVITATIONAL-WAVE DETECTION OF MASSIVE STELLAR BLACK HOLE BINARIES
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DOI：
10.1088/0004-637x/789/2/120
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发表时间：
2014-03
期刊：
影响因子：
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通讯作者：
K. Belczynski;A. Buonanno;M. Cantiello;Chris L. Fryer;D. Holz;I. Mandel;M. Miller;M. Walczak
中科院分区：
文献类型：
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作者：
K. Belczynski;A. Buonanno;M. Cantiello;Chris L. Fryer;D. Holz;I. Mandel;M. Miller;M. Walczak
如果存在由两个100 M的黑洞组成的双星，它们将成为非常强大的引力波源，可以用先进的LIGO/Virgo地面探测器探测到红移z = 2。关于大质量恒星演化的巨大不确定性排除了对这些大质量黑洞合并速率的确定性预测。我们表明，高达每年数百个检测率，或低至没有检测任何，都是可能的。人们认为产生这些大质量联星的唯一方法是通过致密恒星系统中的动力学相互作用。最近在大麦哲伦星云的R136区域发现了几颗150 M的恒星，这一观点受到了挑战。目前的模型预测，当这种质量的恒星离开主序星时，它们的膨胀不足以让共同的包络演化有效地减少轨道分离。由此产生的黑洞-黑洞双星仍然太宽，无法在哈勃时间内合并。如果这个评估是正确的，孤立的超大质量双星就不会演化成引力波源。然而，存在其他形成渠道。例如，大质量恒星的高度多样性，以及它们在相对密集的恒星协会中的常见形成，为大质量黑洞合并开辟了动力学通道（例如，通过Kozai循环或重复的二元-单一相互作用）。我们确定的关键物理因素，塑造人口非常大质量的黑洞黑洞双星。先进的引力波探测器将对超大质量恒星的形成和演化提供重要的限制。
If binaries consisting of two ∼100 M☉ black holes exist, they would serve as extraordinarily powerful gravitational-wave sources, detectable to redshifts of z ∼ 2 with the advanced LIGO/Virgo ground-based detectors. Large uncertainties about the evolution of massive stars preclude definitive rate predictions for mergers of these massive black holes. We show that rates as high as hundreds of detections per year, or as low as no detections whatsoever, are both possible. It was thought that the only way to produce these massive binaries was via dynamical interactions in dense stellar systems. This view has been challenged by the recent discovery of several ≳ 150 M☉ stars in the R136 region of the Large Magellanic Cloud. Current models predict that when stars of this mass leave the main sequence, their expansion is insufficient to allow common envelope evolution to efficiently reduce the orbital separation. The resulting black hole–black hole binary remains too wide to be able to coalesce within a Hubble time. If this assessment is correct, isolated very massive binaries do not evolve to be gravitational-wave sources. However, other formation channels exist. For example, the high multiplicity of massive stars, and their common formation in relatively dense stellar associations, opens up dynamical channels for massive black hole mergers (e.g., via Kozai cycles or repeated binary-single interactions). We identify key physical factors that shape the population of very massive black hole–black hole binaries. Advanced gravitational-wave detectors will provide important constraints on the formation and evolution of very massive stars.