Inter-cluster velocity structures of star cluster complexes
Inter-cluster velocity structures of star cluster complexes
复制标题
星团复合体的星团间速度结构
DOI：
10.1017/s1743921319007634
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发表时间：
2019
期刊：
影响因子：
--
通讯作者：
Fujii Michiko S.
中科院分区：
文献类型：
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作者：
Lorenz Roth;H. Todd Smith;Kazuo Yoshioka;Tracy M. Becker;Aljona Blocker;Nathaniel J. Cunningham;Nickolay Ivchenko;Kurt D. Retherford;Joachim Saur;Michael Velez;Fuminori Tsuchiya;Fujii Michiko S.
星星团通常是以恒星团系统的形式诞生的，其中包括几个恒星团。这样的星团复合体可能是由湍流分子云形成的。由于盖亚数据发布2为我们提供了已知星团复合体中单个恒星的高质量速度数据，我们现在可以将观测到的星团复合体的速度结构与模拟的速度结构进行比较。我们进行了一系列的N-体模拟的星团复合物的形成从湍流分子云。我们测量了我们模拟的星团复合体的星团间速度色散，并将其与船底座区域和NGC 2264进行了比较。我们发现船底座区域和NGC 2264分别由质量为104 × 105 M <$3和104 × 104 M <$3的分子云形成。在我们的模拟中，我们还发现，在复杂的最大集群质量（Mc，最大）如下，其中Mg是初始气体质量。
Star clusters are often born as star-cluster systems, which include several stellar clumps. Such star-cluster complexes could have formed from turbulent molecular clouds. Since Gaia Data Release 2 provided us high quality velocity data of individual stars in known star-cluster complexes, we now can compare the velocity structures of the observed star-cluster complexes with simulated ones. We performed a series of N-body simulations for the formation of star-cluster complexes starting from turbulent molecular clouds. We measured the inter-cluster velocity dispersions of our simulated star-cluster complexes and compared them with the Carina region and NGC 2264. We found that the Carina region and NGC 2264 formed from molecular clouds with a mass of ∼4 × 105M⊙ and ∼4 × 104M⊙, respectively. In our simulations, we also found that the maximum cluster mass (Mc,max) in the complex follows , where Mg is the initial gas mass.