The Stellar IMF as a Property of Turbulence
We propose to interpret the stellar IMF as a property of the turbulence in the star-forming gas. Gravitationally unstable density enhancements in the turbulent flow collapse and form stars. Their mass distribution can be derived analytically from the power spectrum of the turbulent flow and the isothermal shock jump conditions in the magnetized gas.
KeywordsMach Number Mass Distribution Initial Mass Function Intermittent Nature Stellar Cluster
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