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arXiv · astro-ph/0308263

Formation of globular clusters in galaxy mergers

Kenji Bekki·Warrick J. Couch·Duncan A. Forbes·M. A. 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.

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Kenji Bekki, Warrick J. Couch, Duncan A. Forbes, M. A. Beasley. 2003-08-15. Formation of globular clusters in galaxy mergers. https://arxiv.org/abs/astro-ph/0308263

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