Modeling of the Effects of Stellar Feedback during Star Cluster Formation Using a Hybrid Gas and N-Body Method
Modeling of the Effects of Stellar Feedback during Star Cluster Formation Using a Hybrid Gas and N-Body Method
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DOI：
10.3847/1538-4357/abc011
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发表时间：
2020-03
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影响因子：
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通讯作者：
J. E. Wall;M. M. Low-M.;S. McMillan;R. Klessen;S. Zwart;A. Pellegrino
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文献类型：
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作者：
J. E. Wall;M. M. Low-M.;S. McMillan;R. Klessen;S. Zwart;A. Pellegrino
理解星团的形成需要准确地跟踪气体和新形成的恒星之间的相互作用。因此，我们耦合磁流体动力学代码FLASH的N体代码ph 4和恒星演化代码SeBa使用天体物理多用途软件环境（AMUSE）模拟恒星动力学，演化，碰撞N体动力学和形成的二进制和高阶多系统，同时实现恒星反馈的形式在FLASH中的辐射，恒星风，超新星。我们在这里描述的算法用于每个这些过程。我们将此集成包命名为Torch。然后，我们使用这种新的数值方法来模拟的形成和早期演化的几个例子的疏散星团的1000颗恒星形成的云的质量范围为103 M <$-105 M <$。分析恒星反馈对纳塔尔星团的气体和恒星的影响，我们发现，在这些例子中，即使在强烈反馈的存在下，恒星星团也能承受破坏。这甚至可以通过清扫壳层而略微增加致密的金斯不稳定气体的数量;因此，足够强大的恒星风可以捕获自己的H ii区域，从而适度触发星星的形成。我们的星系团在出生时就有适度的质量分离，这种效应会被反馈增强，并在排出它们的纳塔尔气体后保留下来，这与观测结果一致。
Understanding the formation of stellar clusters requires following the interplay between gas and newly formed stars accurately. We therefore couple the magnetohydrodynamics code FLASH to the N-body code ph4 and the stellar evolution code SeBa using the Astrophysical Multipurpose Software Environment (AMUSE) to model stellar dynamics, evolution, and collisional N-body dynamics and the formation of binary and higher-order multiple systems, while implementing stellar feedback in the form of radiation, stellar winds, and supernovae in FLASH. We here describe the algorithms used for each of these processes. We denote this integrated package Torch. We then use this novel numerical method to simulate the formation and early evolution of several examples of open clusters of ∼1000 stars formed from clouds with a mass range of 103 M⊙ to 105 M⊙. Analyzing the effects of stellar feedback on the gas and stars of the natal clusters, we find that in these examples, the stellar clusters are resilient to disruption, even in the presence of intense feedback. This can even slightly increase the amount of dense, Jeans unstable gas by sweeping up shells; thus, a stellar wind strong enough to trap its own H ii region shows modest triggering of star formation. Our clusters are born moderately mass segregated, an effect enhanced by feedback, and retained after the ejection of their natal gas, in agreement with observations.