Formation of Globular Clusters in Galaxy Mergers

K. Bekki, W. Couch, D. Forbes, M. Beasley
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Abstract

Our numerical simulations first demonstrate that the pressure of ISM in a major merger becomes so high ($>$ $10^5$ $\rm k_{\rm B}$ K $\rm cm^{-3}$) that GMCs in the merger can collapse to form globular clusters (GCs) within a few Myr. The star formation efficiency within a GMC in galaxy mergers can rise up from a few percent to $\sim$ 80 percent, depending on the shapes and the temperature of the GMC. This implosive GC formation due to external high pressure of warm/hot ISM can be more efficient in the tidal tails or the central regions of mergers. The developed clusters have King-like profile with the effective radius of a few pc. The structural, kinematical, and chemical properties of these GC systems can depend on orbital and chemical properties of major mergers.
星系合并中球状星团的形成
我们的数值模拟首先表明,在一次大型合并中,ISM的压力变得如此之高($>$ 10^5$ $\rm k_{\rm B}$ K $\rm cm^{-3}$),以至于合并中的gmc可以在几个Myr内坍缩形成球状星团(gc)。在星系合并中,GMC内的恒星形成效率可以从百分之几上升到百分之八十,这取决于GMC的形状和温度。这种内爆式气相岩形成是由温暖/热ISM的外部高压引起的,在潮汐尾或合并的中心区域更有效。发达的星团具有国王型轮廓,有效半径为几个pc。这些GC系统的结构、运动学和化学性质取决于主要合并的轨道和化学性质。
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