The Formation of Massive Stars from Turbulent Cores

Abstract

Observations indicate that massive stars form in regions of very high surface density, ~1 g cm^-2. Clusters containing massive stars and globular clusters have a comparable column density. The total pressure in clouds of such a column density is P/k~10^8-10^9 K cm^-3, far greater than that in the diffuse ISM or the average in GMCs. Observations show that massive star-forming regions are supersonically turbulent, and we show that the molecular cores out of which individual massive stars form are as well. The protostellar accretion rate in such a core is approximately equal to the instantaneous mass of the star divided by the free-fall time of the gas that is accreting onto the star (Stahler, Shu, & Taam 1980). The star-formation time in this Turbulent Core model for massive star formation is several mean free-fall timesscales of the core, but is about equal to that of the region in which the core is embedded. The typical time for a massive star to form is about 10^5 yr and the accretion rate is high enough to overcome radiation pressure due to the luminosity of the star. For the typical case we consider, in which the cores out of which the stars form have a density structure varying as r^{-1.5}, the protostellar accretion rate grows linearly with time. We calculate the evolution of the radius of a protostar and determine the accretion luminosity. At the high accretion rates that are typical in regions of massive star formation, protostars join the main sequence at about 20 solar masses. We apply these results to predict the properties of protostars thought to be powering several observed hot molecular cores, including the Orion hot core and W3(H2O). In the Appendixes, we discuss the pressure in molecular clouds and we argue that ``logatropic'' models for molecular clouds are incompatible with observation.Comment: ApJ accepted; 28 pages, some clarification of the text, results unchange

What physics determines the peak of the IMF? Insights from the structure of cores in radiation-magnetohydrodynamic simulations

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