Evolutionary roads leading to low effective spins, high black hole masses, and O1/O2 rates for LIGO/Virgo binary black holes-猫眼课题宝

DOI：

10.1051/0004-6361/201936528

发表时间：

2017-06

期刊：

Astronomy & Astrophysics

影响因子：

6.5

通讯作者：

中科院分区：

物理与天体物理2区

文献类型：

作者：

K. Belczynski;J. Klencki;C. Fields;A. Olejak;E. Berti;G. Meynet;C. Fryer;D. Holz;R. O’Shaughnessy;D. Brown;T. Bulik;Samuel Leung;K. Nomoto;P. Madau;R. Hirschi;S. R. Jones;S. Mondal;M. Chruslinska;P. Drozda;D. Gerosa;Zoheyr Doctor;M. Giersz;S. Ekstrom;C. Georgy;A. Askar;D. Wysocki;T. Natan;W. Farr;G. Wiktorowicz;M. Miller;B. Farr;J. Lasota

O 1/O2运行后报告的所有十个LIGO/Virgo二元黑洞（BH-BH）合并都具有接近零的有效自旋。对此只有三种可能的解释。如果BH自旋的大小很大，那么：（i）两个BH自旋矢量必须接近轨道平面，或者（ii）BH的自旋角动量必须方向相反且大小相似。那么也有可能（iii）BH自旋幅度很小。我们认为第三个假设的框架内的经典孤立的二进制演变的BH-BH合并形成的情况。我们测试了大质量恒星中角动量传输的三种模型：经向流的适度有效传输（如日内瓦代码中所采用的）、泰勒-斯普鲁特磁力发电机的有效传输（如梅萨代码中所实现的），以及非常有效的传输（如Fuller等人提出的）来计算纳塔尔BH自旋我们允许二进制的演变，以增加BH自旋通过吸积和帐户的潜在自旋的恒星通过潮汐相互作用。此外，我们更新了恒星起源BH质量的计算，包括对星星形成历史和宇宙时间内化学演化的修正。我们发现，我们可以同时匹配所观察到的BH-BH合并率密度和BH质量和BH-BH有效自旋。具有有效角动量输运的模型受到青睐。更新的恒星质量加权气相金属丰度演变现在使用在我们的模型似乎是关键，以获得更好的再现LIGO/室女座合并率估计。如果合并的GW 170729拥有一个质量超过50 M的BH，那么在对不稳定脉动超新星阶段的质量损失可能会被高估。我们还估计率黑洞中子星星（BH-NS）合并从最近的LIGO/室女座观测。如果，事实上。大质量恒星的角动量传输是有效的，那么任何（电磁波或引力波）对快速旋转的BH的观察将表明祖星星的潮汐旋转非常有效（均匀演化，通过情况A质量转移形成高质量X射线双星，或在近距离双星中的沃尔夫-拉叶星星被近距离伴星自旋），黑洞的显著质量吸积，或通过两个或多个黑洞的合并形成黑洞（在密集的星团中）。

All ten LIGO/Virgo binary black hole (BH-BH) coalescences reported following the O1/O2 runs have near-zero effective spins. There are only three potential explanations for this. If the BH spin magnitudes are large, then: (i) either both BH spin vectors must be nearly in the orbital plane or (ii) the spin angular momenta of the BHs must be oppositely directed and similar in magnitude. Then there is also the possibility that (iii) the BH spin magnitudes are small. We consider the third hypothesis within the framework of the classical isolated binary evolution scenario of the BH-BH merger formation. We test three models of angular momentum transport in massive stars: a mildly efficient transport by meridional currents (as employed in the Geneva code), an efficient transport by the Tayler-Spruit magnetic dynamo (as implemented in the MESA code), and a very-efficient transport (as proposed by Fuller et al.) to calculate natal BH spins. We allow for binary evolution to increase the BH spins through accretion and account for the potential spin-up of stars through tidal interactions. Additionally, we update the calculations of the stellar-origin BH masses, including revisions to the history of star formation and to the chemical evolution across cosmic time. We find that we can simultaneously match the observed BH-BH merger rate density and BH masses and BH-BH effective spins. Models with efficient angular momentum transport are favored. The updated stellar-mass weighted gas-phase metallicity evolution now used in our models appears to be key for obtaining an improved reproduction of the LIGO/Virgo merger rate estimate. Mass losses during the pair-instability pulsation supernova phase are likely to be overestimated if the merger GW170729 hosts a BH more massive than 50 M⊙. We also estimate rates of black hole-neutron star (BH-NS) mergers from recent LIGO/Virgo observations. If, in fact. angular momentum transport in massive stars is efficient, then any (electromagnetic or gravitational wave) observation of a rapidly spinning BH would indicate either a very effective tidal spin up of the progenitor star (homogeneous evolution, high-mass X-ray binary formation through case A mass transfer, or a spin- up of a Wolf-Rayet star in a close binary by a close companion), significant mass accretion by the hole, or a BH formation through the merger of two or more BHs (in a dense stellar cluster).

Evolutionary roads leading to low effective spins, high black hole masses, and O1/O2 rates for LIGO/Virgo binary black holes

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