Self-shielding clumps in starburst clusters
Jan Palou\v{s}, Richard W\"unsch, So\v{n}a Ehlerov\'a, Guillermo, Tenorio-Tagle
TL;DR
This paper investigates the formation and evolution of self-shielding clumps in young, massive star clusters, focusing on thermal instability, mass accumulation, and the role of heating efficiency in their development.
Contribution
It introduces a model for the formation of self-shielded clumps in starburst clusters considering thermal instability and wind heating efficiency effects.
Findings
Clumps can become self-shielded during their infall towards the cluster center.
Heating efficiency significantly influences clump formation and evolution.
Thermal instability leads to localized cooling and pressure reduction in cluster winds.
Abstract
Young and massive star clusters above a critical mass form thermally unstable clumps reducing locally the temperature and pressure of the hot 10~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.
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