论文标题
使用混合气体和N体方法建模恒星簇形成期间恒星反馈的影响
Modelling of the Effects of Stellar Feedback during Star Cluster Formation Using a Hybrid Gas and N-Body Method
论文作者
论文摘要
了解恒星簇的形成需要遵循气体和新形成的恒星之间的相互作用。 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.我们在这里描述了这些过程中每个过程中使用的算法。我们表示这个集成的软件包火炬。然后，我们使用这种新颖的数值方法来模拟〜1000颗恒星的几个示例的形成和早期演化，这些簇是由云范围为10^3-10^5 m_sun的云形成的。分析恒星反馈对出生簇的气体和恒星的影响，我们发现在这些示例中，即使存在强烈的反馈，恒星簇也可以弹性。这甚至可以稍微增加浓密的量，牛仔裤通过扫除贝壳而不稳定的气体；因此，恒星风足够强，足以捕获其自己的H II区域显示出适度的恒星形成触发。我们的集群天生中等质量隔离，通过反馈增强的效果，并在其出生气体弹出后保留，与观察结果一致。
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 10^3-10^5 M_sun. 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.
