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| EPoS Contribution |
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Radiation Hydrodynamics of Super Star Cluster Nuclei
Benny Tsang UT Austin, Austin, US | |
| We still know very little about star formation in the nuclei of super star clusters, the highest-density star formation sites in the universe and the potential birth places of massive black holes. Large distances to these extreme objects and dust obscuration have been limiting our observational access, calling for new campaigns with infrared instruments on 30-meter class telescopes and the JWST. To theoretically predict star formation efficiencies and the primordial mass segregation (the latter is crucial for massive black hole formation), hydrodynamical simulations must realize the multidimensional complexity of dusty, radiation-energized gas on scales < 0.1 pc inside the central nucleus forming O stars. The O stars' radiation repels the incoming gas streams and this is thought to ultimately terminate star formation and expel the residual gas. To study super star cluster formation, we carry out radiation-hydrodynamical simulations of gaseous gravitational collapse in a turbulent, very-high-density interstellar medium. We use the sink particle method in conjunction with a realistic, multi-frequency treatment of stellar radiation. Our Monte-Carlo radiation transport scheme properly handles anisotropic radiation reprocessing and trapping in a highly inhomogeneous turbulent flow. | |
| Collaborators: M. Milosavljevic, U Texas Austin, US |
Suggested Session:
Cluster Formation |