论文标题
后坐力对Ligo/处女座目录的黑洞合并的启示
Implications of recoil kicks for black hole mergers from LIGO/Virgo catalogs
论文作者
论文摘要
Ligo/处女座协作的第一和第二引力瞬态目录包括第三次观察跑步的第一，第二和上半年的50美元确认合并事件。我们计算赋予合并残余的后坐力的分布，并估计其在各种天体物理环境中的保留概率，这是最大祖细胞自旋的函数（$χ_ {\ rm max} $），假设Ligo/Pirgo二进制黑洞（BBH）合并催化了动态的二进制黑洞（BBH）合并是由动态的Addynical Asspondy of Adynical Advission in a Prodyical Advission in a Prodiatical Advission in n of Andens of Ands of odyical Advission。 We find that the distributions of average recoil kicks are peaked at about $150$ km s$^{-1}$, $250$ km s$^{-1}$, $350$ km s$^{-1}$, $600$ km s$^{-1}$, for maximum progenitor spins of $0.1$, $0.3$, $0.5$, $0.8$, respectively.仅在银河核星团以及最庞大的球状簇和超级明星簇中发现，只有具有逃逸速度$ \ gtrsim 100 $ km s $ s $ s $ s $^{ - 1} $，可以有效地保留Ligo/virgo BBH的合并保留，即使是$ umucoutitor spins $ um um um um um um um um um um umax $ _ {对于高祖细胞旋转（$χ_ {\ rm max} \ gtrsim 0.5 $），只有最庞大的核星簇才能保留合并产品。我们还表明，有效自旋的估计值和GW170729，GW190412，GW190519和GW190620的残留旋转值，如果它们的祖细胞中等旋转，则可以再现了GW190620的估计值（\χ_{\ rm max} \ rm max} \ gtrsim 0.3 $ 0.3 $ gw190519，如果它们的祖细胞中等旋转。旋转（$χ_ {\ rm max} \ gtrsim 0.8 $）。另外，如果至少一个祖细胞已经是第二代BH，则可以解释其中的一些事件。
The first and second Gravitational Wave Transient Catalogs by the LIGO/Virgo Collaboration include $50$ confirmed merger events from the first, second, and first half of the third observational runs. We compute the distribution of recoil kicks imparted to the merger remnants and estimate their retention probability within various astrophysical environments as a function of the maximum progenitor spin ($χ_{\rm max}$), assuming that the LIGO/Virgo binary black hole (BBH) mergers were catalyzed by dynamical assembly in a dense star cluster. We find that the distributions of average recoil kicks are peaked at about $150$ km s$^{-1}$, $250$ km s$^{-1}$, $350$ km s$^{-1}$, $600$ km s$^{-1}$, for maximum progenitor spins of $0.1$, $0.3$, $0.5$, $0.8$, respectively. Only environments with escape speed $\gtrsim 100$ km s$^{-1}$, as found in galactic nuclear star clusters as well as in the most massive globular clusters and super star clusters, could efficiently retain the merger remnants of the LIGO/Virgo BBH population even for low progenitor spins ($χ_{\rm max}=0.1$). In the case of high progenitor spins ($χ_{\rm max}\gtrsim 0.5$), only the most massive nuclear star clusters can retain the merger products. We also show that the estimated values of the effective spin and of the remnant spin of GW170729, GW190412, GW190519, and GW190620 can be reproduced if their progenitors were moderately spinning ($χ_{\rm max}\gtrsim 0.3$), while for GW190517 if the progenitors were rapidly spinning ($χ_{\rm max}\gtrsim 0.8$). Alternatively, some of these events could be explained if at least one of the progenitors is already a second-generation BH, originated from a previous merger.
