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The first gravitational-wave source from the isolated evolution of two stars in the 40-100 solar mass range

机译：来自40-100太阳质量范围内两颗恒星的孤立演化的第一个重力波源

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摘要

The merger of two massive (about 30 solar masses) black holes has been detected in gravitational waves(1). This discovery validates recent predictions(2-4) that massive binary black holes would constitute the first detection. Previous calculations, however, have not sampled the relevant binary-black-hole progenitors-massive, low-metallicity binary stars-with sufficient accuracy nor included sufficiently realistic physics to enable robust predictions to better than several orders of magnitude(5-10). Here we report high-precision numerical simulations of the formation of binary black holes via the evolution of isolated binary stars, providing a framework within which to interpret the first gravitational-wave source, GW150914, and to predict the properties of subsequent binary-black-hole gravitational-wave events. Our models imply that these events form in an environment in which the metallicity is less than ten per cent of solar metallicity, and involve stars with initial masses of 40-100 solar masses that interact through mass transfer and a common-envelope phase. These progenitor stars probably formed either about 2 billion years or, with a smaller probability, 11 billion years after the Big Bang. Most binary black holes form without supernova explosions, and their spins are nearly unchanged since birth, but do not have to be parallel. The classical field formation of binary black holes we propose, with low natal kicks (the velocity of the black hole at birth) and restricted common-envelope evolution, produces approximately 40 times more binary-black-holes mergers than do dynamical formation channels involving globular clusters(11); our predicted detection rate of these mergers is comparable to that from homogeneous evolution channels(12-15). Our calculations predict detections of about 1,000 black-hole mergers per year with total masses of 20-80 solar masses once second-generation ground-based gravitational-wave observatories reach full sensitivity.
机译：在引力波中检测到两个大质量黑洞（约30个太阳质量）的合并（1）。这一发现证实了最近的预测（2-4），即大量的二元黑洞将构成首次检测。然而，先前的计算还没有以足够的精度对相关的双黑洞前体，大质量，低金属度的双星进行采样，也没有包括足够现实的物理学来使鲁棒的预测好于几个数量级（5-10）。在这里，我们报告了通过孤立的双星的演化形成的双黑洞的高精度数值模拟，为解释第一个重力波源GW150914以及预测随后的双黑星的性质提供了一个框架。空穴重力波事件。我们的模型表明，这些事件是在金属度不到太阳金属度的10％的环境中形成的，并且涉及质量初始值为40-100太阳质量的恒星，这些质量通过传质和共包络相相互作用。这些祖先恒星可能形成于大爆炸之后约20亿年，或者可能性较小，约为110亿年。大多数二元黑洞都是在没有超新星爆炸的情况下形成的，自出生以来它们的自旋几乎没有变化，但不必是平行的。我们提出的二元黑洞的经典场形成具有较低的出生时踢动（出生时黑洞的速度）和受限制的共同包络演化，所产生的二元黑洞合并的数量大约是涉及球状的动态形成通道的合并数量的40倍簇（11）;我们对这些合并的预测发现率与同类进化渠道的预测率相当（12-15）。我们的计算预测，一旦第二代地面重力波观测站达到最高灵敏度，每年将检测到约1000个黑洞合并，总质量为20-80太阳质量。

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  • 来源
    《Nature》 |2016年第7608期|512-515|共4页
  • 作者

    Belczynski Krzysztof; Holz Daniel E.; Bulik Tomasz; OShaughnessy Richard;

  • 作者单位

    Warsaw Univ, Astron Observ, Ujazdowskie 4, PL-00478 Warsaw, Poland;

    Univ Chicago, Enrico Fermi Inst, Dept Phys, Dept Astron & Astrophys, 5640 S Ellis Ave, Chicago, IL 60637 USA|Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA;

    Warsaw Univ, Astron Observ, Ujazdowskie 4, PL-00478 Warsaw, Poland;

    Rochester Inst Technol, Ctr Computat Relat & Gravitat, Rochester, NY 14623 USA;

  • 收录信息 美国《科学引文索引》(SCI);美国《工程索引》(EI);美国《生物学医学文摘》(MEDLINE);美国《化学文摘》(CA);
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