arXiv 2409.202712024-09-30astro-ph.GA

正在膨胀的极年轻星团质量-半径关系的演化

The evolution of the mass--radius relation of expanding very young star clusters

Jian-Wen Zhou, Pavel Kroupa, Wenjie Wu

备注：: 8 pages, 10 figures, Accepted for publication on A&A

AI总结：

本文通过直接 N 体模拟研究嵌入星团气体驱逐后的早期膨胀，证明 Pfalzner et al. 的质量-半径关系可由 Marks & Kroupa 初始关系经膨胀演化得到，并发现不同观测星团的质量-尺寸关系斜率相似，暗示其诞生于 Plummer 分布轮廓。

摘要：

嵌入星团的初始质量-半径关系是理解恒星在其中形成的嵌入星团演化为通过疏散星团阶段释放进入银河系场这一过程的一个至关重要的边界条件。Marks & Kroupa 推导出的嵌入星团初始质量-半径关系与 Pfalzner et al. 所提出的关系存在显著差异。本文使用直接 N 体模拟来模拟嵌入星团在残余气体被驱逐后的早期膨胀过程。从多个来源收集到的年龄最大为数百万年的星团半径观测数据与 N 体模型拟合良好，这意味着这些观测到的极年轻星团很可能正处于膨胀状态。我们表明，Pfalzner et al. 的质量-半径关系反映了嵌入星团在遵循 Marks & Kroupa 初始质量-半径关系之后的膨胀过程。我们还提出，即使是在 ATLASGAL 团块中带有 HII 区的嵌入星团，可能也已经开始膨胀。本文收集的所有来自不同观测的星团都显示出具有相似斜率的质量-尺寸关系，这可能表明所有星团诞生时都具有类似于 Plummer 相空间分布函数的轮廓。

英文摘要：

The initial mass--radius relation of embedded star clusters is an essentially important boundary condition for understanding the evolution of embedded clusters in which stars form to their release into the galactic field via an open star cluster phase. The initial mass--radius relation of embedded clusters deduced by Marks \& Kroupa is significantly different from the relation suggested by Pfalzner et al. Here, direct N-body simulations are used to model the early expansion of embedded clusters after the expulsion of their residual gas. The observational data of radii of up to a few~Myr old clusters collated from various sources are found to be well fit by the N-body models, implying these observed very young clusters to most likely be in an expanding state. We show that the mass-radius relation of Pfalzner et al. reflects the expansion of embedded clusters following the initial mass-radius relation of Marks \& Kroupa. We also suggest that even the embedded clusters in ATLASGAL clumps with HII regions are probably already in expansion. All here collected clusters from different observations show a mass-size relation with a similar slope, which may indicate that all clusters were born with a profile resembling that of the Plummer phase-space distribution function.

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