我应该留下还是应该离开：大质量星团中的恒星风保留和驱逐
Should I Stay or Should I Go: Stellar Wind Retention and Expulsion in Massive Star Clusters
摘要：
质量和能量注入整个星团的生命周期有助于气体水库可用于后续的恒星形成和反馈能量预算负责喷射材料从集群。此外，在恒星内部处理并以风的形式喷出的物质有可能增加目前正在形成的恒星或后来从保留的气体库形成的恒星的丰度比。在这里，我们提出了流体动力学模拟，探索了广泛的集群质量，紧凑性，金属丰度和恒星星族年龄组合，以确定有利于恒星风保留或风力驱动的气体驱逐星团的参数空间的范围。我们讨论的恒星风处方的保留和驱逐效力的影响，使用MESA恒星演化模型作为一个试验台，探索如何风保留/驱逐量取决于不同质量和年龄的恒星风之间的混合量。最后，我们总结了在各种紧凑（$σ_v \gtrsim 20 \, {\rm km s^{-1}}$）星团，包括年轻的大质量星团（$10^5 \lesssim M/M_\odot \lesssim 10^7$，$age \lesssim 500$ ~Myrs），中间年龄集群（$10^5 \lesssim M/M_\odot \lesssim 10^7$，$age \approx 1-4$ ~Gyrs）和球状星团（$10^5 \lesssim M/M_\odot \lesssim 10^7$，$age \gtrsim 10$ ~Gyrs）的气体保留和排出的一些影响。
英文摘要：
Mass and energy injection throughout the lifetime of a star cluster contributes to the gas reservoir available for subsequent episodes of star formation and the feedback energy budget responsible for ejecting material from the cluster. In addition, mass processed in stellar interiors and ejected as winds has the potential to augment the abundance ratios of currently forming stars, or stars which form at a later time from a retained gas reservoir. Here we present hydrodynamical simulations that explore a wide range of cluster masses, compactnesses, metallicities and stellar population age combinations in order to determine the range of parameter space conducive to stellar wind retention or wind powered gas expulsion in star clusters. We discuss the effects of the stellar wind prescription on retention and expulsion effectiveness, using MESA stellar evolutionary models as a test bed for exploring how the amounts of wind retention/expulsion depend upon the amount of mixing between the winds from stars of different masses and ages. We conclude by summarizing some implications for gas retention and expulsion in a variety of compact ($σ_v \gtrsim 20 \, {\rm km s^{-1}}$) star clusters including young massive star clusters ($10^5 \lesssim M/M_\odot \lesssim 10^7$, $age \lesssim 500$~Myrs), intermediate age clusters ($10^5 \lesssim M/M_\odot \lesssim 10^7$, $age \approx 1-4$~Gyrs), and globular clusters ($10^5 \lesssim M/M_\odot \lesssim 10^7$, $age \gtrsim 10$~Gyrs).
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