论文标题
来自年轻大型和开放式恒星簇的丽莎来源
LISA sources from young massive and open stellar clusters
论文作者
论文摘要
我研究了年轻的大规模（YMC）和开放型星团（OCS）在组装恒星质量二元黑洞（BBH）中的潜在作用，这些黑洞（BBHS）可以通过即将出现的LISA任务被发现为持续的重力波（GW）来源。明星簇内部的充满活力的动力相互作用使它们成为组装BBH和其他类型的双层二进制组合的工厂，这些二进制经历了一般性偏爱（GR）灵感和合并。这种灵感的初始阶段通常会扫过丽莎GW乐队。在这里，从一组块质量的恒星簇的进化模型中研究了这样的LISA来源，范围超过$ 10^4M_ \ ODOT-10^5M_ \ ODOT $，代表了当地宇宙的金属富含金属和金属畅通的YMC和中级OC。这些模型通过长期，直接，相对论的多体计算的发展，其中包含了最新的恒星进化和残余形成模型。基于使用此类模型簇构建的本地宇宙的模型，显示YMC和中年OCS将在当前的宇宙时代以GW频率在$ 10^{ - 3} { - 3} {\ rm〜hz} {\ rm〜hz} - 10^{ - 1^{ - 1} { - 1} { - 1} {\ rm〜hz $ rm〜hz（\ rm〜hz）中，在$ 10^{ - 3} {\ rm〜hz} {\ rm〜hz（\ rm〜hz）中产生几种10至100s lisa bbh源。 $> 5 $，假设传教士的寿命为5年或10年。这种Lisa BBHS的总质量将具有双峰分布，通常是偏心的（$ \ lyssim0.7 $），尽管可以进行质量 - 空气对称系统，但通常具有相似的组件质量。从本质上讲，YMC和OCS的当今可检索的Lisa可检测BBH将有1000秒。这样，YMC和OCS将为Lisa检测到的恒星质量BBH人群提供重要的贡献。这些BBH中的一小部分（$ <5 $％）会经历GR Inspral，以使其在Mission Timespan内部进入Ligo-Virgo GW频段和合并； $ <15 $％的时间将在两倍的时间内。
I study the potential role of young massive (YMCs) and open star clusters (OCs) in assembling stellar-mass binary black holes (BBHs) which would be detectable as persistent gravitational-wave (GW) sources by the forthcoming LISA mission. The energetic dynamical interactions inside star clusters make them factories of assembling BBHs and other types of double-compact binaries that undergo general-relativistic (GR) inspiral and merger. The initial phase of such inspirals would, typically, sweep through the LISA GW band. Here, such LISA sources are studied from a set of evolutionary models of star clusters with masses ranging over $10^4M_\odot-10^5M_\odot$ that represent YMCs and intermediate-aged OCs in metal-rich and metal-poor environments of the Local Universe. These models are evolved with long-term, direct, relativistic many-body computations incorporating state-of-the-art stellar-evolutionary and remnant-formation models. Based on models of Local Universe constructed with such model clusters, it is shown that YMCs and intermediate-aged OCs would yield several 10s to 100s of LISA BBH sources at the current cosmic epoch with GW frequency within $10^{-3}{\rm~Hz} - 10^{-1}{\rm~Hz}$ and signal-to-noise-ratio (S/N) $>5$, assuming a mission lifetime of 5 or 10 years. Such LISA BBHs would have a bimodal distribution in total mass, be generally eccentric ($\lesssim0.7$), and typically have similar component masses although mass-asymmetric systems are possible. Intrinsically, there would be 1000s of present-day, LISA-detectable BBHs from YMCs and OCs. That way, YMCs and OCs would provide a significant and the dominant contribution to the stellar-mass BBH population detectable by LISA. A small fraction, $<5$%, of these BBHs would undergo GR inspiral to make it to LIGO-Virgo GW frequency band and merge, within the mission timespan; $<15$% would do so within twice the timespan.
