The Stellar Mass Spectrum from Non-Isothermal Gravoturbulent Fragmentation
Identifying the processes that determine the initial mass function of stars (IMF) is a fundamental problem in star formation theory. One of the major uncertainties is the exact chemical state of the star forming gas and its influence on the dynamical evolution. Most simulations of star forming clusters use an isothermal equation of state (EOS). We address these issues and study the effect of a piecewise polytropic EOS on the formation of stellar clusters in turbulent, selfgravitating molecular clouds using three-dimensional, smoothed particle hydrodynamics simulations.
KeywordsCritical Density Molecular Cloud Stellar Mass Initial Mass Function Result Mass Spectrum
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