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Evolving a 10⁶ solar mass star along the Hayashi track: Exploring the mass-radius relation of a proto globular cluster cloud

Anna Sippel, Swinburne University
Advisors: Norman Murray

Abstract: We explore the mass-radius relation of a proto globular cluster cloud. This is motivated by the finding that observed clusters in the mass range 10⁴- 10⁶ solar masses show no systematic variation of radius with mass, while clusters with masses larger than 3 10⁶ solar masses have an increasing size with increasing mass. Murray (2009) show that those massive clusters were optically thick to far-infrared radiation when they formed, leading for the size of them set by a balance between radiation pressure (powered by accretion) and gravity. We aim to create a model of such a proto cluster cloud (before its fragmentation) to investigate this theory, and use MESA to do so.

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