Great balls of FIRE II: The evolution and destruction of star clusters across cosmic time in a Milky Way-mass galaxy
Great balls of FIRE II: The evolution and destruction of star clusters across cosmic time in a Milky Way-mass galaxy
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FIRE II 的伟大球体：银河系质量星系中星团在整个宇宙时间内的演化和毁灭
DOI：
10.1093/mnras/stad578
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发表时间：
2023
影响因子：
4.8
通讯作者：
Wetzel, Andrew
中科院分区：
文献类型：
--
作者：
Rodriguez, Carl L.;Hafen, Zachary;Grudić, Michael Y.;Lamberts, Astrid;Sharma, Kuldeep;Faucher-Giguère, Claude-André;Wetzel, Andrew
当前一代的星系模拟可以解析单个巨型分子云，即致密星团的前身。但这些年轻的大质量星团的演化命运，以及它们是否能成为许多星系中观察到的古老球状星团（GC），是由内部动力学过程和外部星系效应的复杂相互作用决定的。我们提出了第一个在银河系质量星系的 FIRE-2 MHD 模拟中形成的大质量（N∼105-107）星团的逐星 N 体模型，并从宇宙学模拟中提取了相关的初始条件和潮汐力。我们从 Grudić 等人那里选择了 895 个（∼30%）>6 × 104M 的 YMC。 2022 并使用集群蒙特卡罗代码 CMC 将它们积分为 z= 0。该程序预测了一个具有 148 个 GC 的类似 MW 的系统，主要是在恒星形成的早期突发模式中形成的。与银河系或 M31 中的星团相比，我们的 GC 更年轻、质量更小、核心塌缩程度更高。这是由宿主星系的组装历史和年龄-金属丰度关系造成的：较年轻的星团优先诞生在较强的潮汐场中，并且最初保留的恒星质量黑洞较少，导致它们比较老的星系团更快地失去质量并更快达到核心塌陷。我们的结果表明，GC的质量和核心/半光半径不仅由内部动力学过程决定，而且还由其宿主星系的特定演化历史决定。这些结果强调，利用现实恒星物理进行 N 体研究对于理解 GC 系统的演化和当今特性至关重要。
The current generation of galaxy simulations can resolve individual giant molecular clouds, the progenitors of dense star clusters. But the evolutionary fate of these young massive clusters, and whether they can become the old globular clusters (GCs) observed in many galaxies, is determined by a complex interplay of internal dynamical processes and external galactic effects. We present the first star-by-starN-body models of massive (N∼ 105–107) star clusters formed in a FIRE-2 MHD simulation of a Milky Way-mass galaxy, with the relevant initial conditions and tidal forces extracted from the cosmological simulation. We select 895 (∼30 per cent) of the YMCs with >6 × 104M⊙from Grudić et al. 2022 and integrate them toz= 0 using the cluster Monte Carlo code,CMC. This procedure predicts a MW-like system with 148 GCs, predominantly formed during the early, bursty mode of star formation. Our GCs are younger, less massive, and more core-collapsed than clusters in the Milky Way or M31. This results from the assembly history and age-metallicity relationship of the host galaxy: Younger clusters are preferentially born in stronger tidal fields and initially retain fewer stellar-mass black holes, causing them to lose mass faster and reach core collapse sooner than older GCs. Our results suggest that the masses and core/half-light radii of GCs are shaped not only by internal dynamical processes, but also by the specific evolutionary history of their host galaxies. These results emphasize thatN-body studies with realistic stellar physics are crucial to understanding the evolution and present-day properties of GC systems.