论文标题
GW190521通过燃气积聚到人口III出生于高红色Minihalos的恒星黑洞残留物
Formation of GW190521 via gas accretion onto Population III stellar black hole remnants born in high-redshift minihalos
论文作者
论文摘要
最近的重力波合并事件GW190521挑战了我们对恒星质量黑洞（BH）形成的理解。推断主要和次级BH均落入配对稳定性（PI）质量间隙内。在这里，我们建议通过在高红移（$ z> 10 $）Minihalos的Minihalos中的人口III（POP〜III）星人的BH残留物来形成这种二进制物。一旦母晕延长到原子冷却极限，即使在光环的密集中央区域中的气体积聚发作也可能会使POP〜III III残留BHS的质量高于PI限制。从BBH开始，初始质量为O（100）$ {\ rm m _ {\ odot}} $，我们发现它只需要在原子 - 冷却晕的内部几个PC中花费大约100〜Myr才能在原子 - 冷却晕的内部几个PC上向Accrete添加到Accporte向50〜 $ {\ rm m _ {\ odot}} $ compemble of Inality of Interals of Interals of Interals and System a System a System a System a System a System a System a System a System a System a System a System。二进制沉入其母晕致密内部区域的动力学摩擦时间尺度比增加其质量以高于PI限制所需的积分时间尺度是可比或短的。一旦进入光环的核心，二进制可以进入Hyper-Eddington积聚的阶段，在那里只需几千年才能通过积聚超过PI限制。更大的BBH可以通过该通道形成，并通过提高低频灵敏度的检测器可检测。单个POP〜III BH残留物也将通过积聚生长，后来可能会动态形成二进制文件。从GW190521 $ 0.13^{+0.3} _ { - 0.11} \ rm Gpc^{ - 3} yr^} yr^{ - 1} $。
The recent gravitational wave merger event, GW190521, has challenged our understanding of the stellar-mass black hole (BH) formation. The primary and secondary BH are both inferred to fall inside the pair-instability (PI) mass gap. Here we propose that the formation of such binaries is possible through gas accretion onto the BH remnants of Population III (Pop~III) stars born in high-redshift ($z>10$) minihalos. Once the parent halo has grown to the atomic-cooling limit, even brief episodes of gas accretion in the dense central regions of the halo can increase the masses of Pop~III remnant BHs above the PI limit. Starting with a BBH with an initial mass of O(100) ${\rm M_{\odot}}$ we find that it would only need to spend about 100~Myr in the inner few pc of an atomic-cooling halo to accrete about 50~${\rm M_{\odot}}$ of material and resemble a system similar to GW190521. The dynamical friction timescale for the binary to sink to the dense inner region of its parent halo is comparable or shorter than the accretion timescale required to increase their mass above the PI limit. Once in the core of the halo, the binary can enter a phase of hyper-Eddington accretion, where it would only take a few thousand years to exceed the PI limit through accretion. Even more massive BBHs could form through this channel, and be detectable by detectors with improved low-frequency sensitivity. Single Pop~III BH remnants would also grow through accretion and could later form binaries dynamically. As little as a few percent of Pop~III BH remnants may be sufficient to match the rate of massive BBH mergers inferred from GW190521 of $0.13^{+0.3}_{-0.11}\rm Gpc^{-3} yr^{-1}$.
