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arXiv 0908.3910astro-ph.SRastro-ph.GA
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大质量恒星和星团的同时形成

The Simultaneous Formation of Massive Stars and Stellar Clusters

Rowan J. Smith, Steven Longmore, Ian Bonnell

备注：
Accepted for publication in MNRAS. 11 pages, 9 figures and 3 tables
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摘要：

我们发现大质量恒星和星团是同时形成的，形成中的星团的全球演化是使中心恒星变得大质量的原因。我们预测，大质量恒星形成的团块，如莫特等人在2007年观察到的，收缩和质量增长导致大质量恒星的形成。这是因为质量不断地从大半径输送到中心的原恒星上，这些原恒星可以通过吸积变得巨大。使用SPH模拟的大质量恒星形成团块在一个巨大的分子云，我们表明，团块最初是扩散和对流，并成为更加集中，因为他们崩溃。我们的数据的模拟干涉观测提供了一个解释，为什么年轻的大质量恒星形成区显示更多的子结构比老的。在我们的模型中，质量最大的恒星是在最紧密的星团中发现的。大质量恒星吸积的大部分质量最初以低密度分布在整个星团中，后来由于全球性的下降而汇集到恒星中。即使有辐射反馈，也不会形成大质量的前星核。原始的核心是中等质量的，并在原恒星阶段获得额外的质量。我们还发现，形成低质量恒星的核心存在于高质量恒星吸积的体积内，但在很大程度上不受这个过程的影响。

英文摘要：

We show that massive stars and stellar clusters are formed simultaneously, the global evolution of the forming cluster is what allows the central stars to become massive. We predict that massive star forming clumps, such as those observed in Motte et al. 2007, contract and grow in mass leading to the formation of massive stars. This occurs as mass is continually channeled from large radii onto the central proto-stars, which can become massive through accretion. Using SPH simulations of massive star forming clumps in a Giant Molecular Cloud, we show that clumps are initially diffuse and filamentary, and become more concentrated as they collapse. Simulated interferometry observations of our data provide an explanation as to why young massive star forming regions show more substructure than older ones. The most massive stars in our model are found within the most bound cluster. Most of the mass accreted by the massive stars was originally distributed throughout the clump at low densities, and was later funneled to the star due to global in-fall. Even with radiative feedback no massive pre-stellar cores are formed. The original cores are of intermediate mass and gain their additional mass in the proto-stellar stage. We also find that cores which form low mass stars exist within the volume from which the high mass stars accrete, but are largely unaffected by this process.

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