http://arxiv.org/abs/1601.03857
Young and massive star clusters above a critical mass form thermally unstable clumps reducing locally the temperature and pressure of the hot 10$^{7}$~K cluster wind. The matter reinserted by stars, and mass loaded in interactions with pristine gas and from evaporating circumstellar disks, accumulate on clumps that are ionized with photons produced by massive stars. We discuss if they may become self-shielded when they reach the central part of the cluster, or even before it, during their free fall to the cluster center. Here we explore the importance of heating efficiency of stellar winds.
J. Palous, R. Wunsch, S. Ehlerova, et. al.
Mon, 18 Jan 16
34/50
Comments: 2 pages, 4 figures, IAU Symposium 316: Formation, Evolution, and Survival of Massive Star Clusters
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