S315.7.03 — Models and Simulations of Star Cluster Formation

Date & Time

Aug 5th at 2:40 PM until 3:05 PM




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Author(s): Philip Myers1
Institution(s): 1. Harvard-Smithsonian CfA
We review recent progress in describing the physical processes of star cluster formation, with theoretical models and numerical simulations. In many recent studies, supersonic, turbulent flows assemble and structure the gas into a network of clumps, filaments, and cores. Once enough mass is assembled, self-gravity acts on the large scale to contract the system and on the small scale to condense filaments and cores to the point of forming single stars, multiples, groups, and subclusters. Recently formed stars provide energy and momentum through ionization, radiative heating, winds, and outflows. This feedback inhibits formation of low mass stars, reduces the gas mass available for protostar accretion, and eventually disperses most of the protocluster gas.