The formation of high-mass stars and clusters

 

Jonathan C. Tan (University of Florida)

 

 

 

I review the core accretion model of massive star formation, which assumes the process is a scaled-up version of low-mass star formation. The “Turbulent Core Model” invokes collapse from massive cores that are in approximate virial equilibrium, with their internal pressure dominated by turbulence and/or magnetic fields. Additionally, the cores are assumed to be in approximate pressure equilibrium with the surrounding clump environment, which is also a self-gravitating, near-virial-equilibrium gas cloud, but one which ends up fragmenting to form a star cluster, taking at least several free-fall timescales to do so. I discuss how recent observational evidence, including that from Herschel, is constraining these theoretical models.