论文标题
年轻大型和开放式恒星簇IV中的恒星质量黑洞IV：更新的恒星进化和黑洞旋转模型，并与Ligo-Virgo O1/O2合并数据进行比较
Stellar-mass black holes in young massive and open stellar clusters IV: updated stellar-evolutionary and black hole spin models and comparisons with the LIGO-Virgo O1/O2 merger-event data
论文作者
论文摘要
I present a set of long-term, direct, relativistic many-body computations of model dense stellar clusters with up-to-date stellar-evolutionary, supernova (SN), and remnant natal-kick models, including pair instability and pulsation pair instability supernova (PSN and PPSN), using an updated version of NBODY7 N-body simulation program. N体模型还包括基于BHS的基于恒星进化的出生旋转以及基于数值相对论的二进制黑洞（BBH）合并的处理。这些在直接的N体模拟中首次允许第二代BBH合并。一组65个进化模型具有初始质量$ 10^4M_ \ odot-10^5m_ \ odot $，尺寸为1 pc-3 PC，金属$ 0.0001-0.02 $，具有原始二进制的大型恒星，它们代表年轻的大型簇（YMC）（YMC）（YMC），并且代表大量的开放式Clusters（OC）。这样的模型产生了动态分配的BBH合并，与观察到的质量，质量比，有效自旋参数和LVC O1/O2合并事件的最终旋转非常吻合，前提是BHS天生低或没有旋转，但在接受BBH合并或物质收集后，旋转却是旋转的。特别是，自然复制了GW170729合并事件的明显更高的质量，有效自旋参数和最终自旋，以及O3事件GW190412的质量不对称性。计算出的模型产生了巨大的，$ \ sim100m_ \ odot $ bbh合并在“ PSN GAP”中具有主要质量，并且也产生涉及“质量间隙”中残留物的合并。他们还建议YMC和OC会产生LISA可检测到的持久的，局部的GW来源。此类簇还能够产生偏心的Ligo-Virgo合并。
I present a set of long-term, direct, relativistic many-body computations of model dense stellar clusters with up-to-date stellar-evolutionary, supernova (SN), and remnant natal-kick models, including pair instability and pulsation pair instability supernova (PSN and PPSN), using an updated version of NBODY7 N-body simulation program. The N-body model also includes stellar evolution-based natal spins of BHs and treatments of binary black hole (BBH) mergers based on numerical relativity. These, for the first time in a direct N-body simulation, allow for second-generation BBH mergers. The set of 65 evolutionary models have initial masses $10^4M_\odot-10^5M_\odot$, sizes 1 pc-3 pc, metallicity $0.0001-0.02$, with the massive stars in primordial binaries and they represent young massive clusters (YMC) and moderately massive open clusters (OC). Such models produce dynamically-paired BBH mergers that agree well with the observed masses, mass ratios, effective spin parameters, and final spins of the LVC O1/O2 merger events, provided BHs are born with low or no spin but spin up after undergoing a BBH merger or matter accretion onto it. In particular, the distinctly higher mass, effective spin parameter, and final spin of GW170729 merger event is naturally reproduced, as also the mass asymmetry of the O3 event GW190412. The computed models produce massive, $\sim100M_\odot$ BBH mergers with primary mass within the 'PSN gap' and also yield mergers involving remnants in the 'mass gap'. They also suggest that YMCs and OCs produce persistent, Local-Universe GW sources detectable by LISA. Such clusters are also capable of producing eccentric LIGO-Virgo mergers.
