Gravitational Collapse in Turbulent Molecular Clouds. I. Gasdynamical Turbulence

Details Gravitational Collapse in Turbulent Molecular Clouds. I. Gasdynamical Turbulence Gravitational Collapse in Turbulent Molecular Clouds. I. Gasdynamical Turbulence

1999-11-04

arxiv.org/abs/astro-ph/9911068v2

Astrophys.J.535:887-906,2000

Astronomy and Astrophysics

Astrophysics

Minor revisions in response to referee, thirteen figures, accepted to Astrophys. J

Scientific paper

10.1086/308891

Observed molecular clouds often appear to have very low star formation efficiencies and lifetimes an order of magnitude longer than their free-fall times. Their support is attributed to the random supersonic motions observed in them. We study the support of molecular clouds against gravitational collapse by supersonic, gas dynamical turbulence using direct numerical simulation. Computations with two different algorithms are compared: a particle-based, Lagrangian method (SPH), and a grid-based, Eulerian, second-order method (ZEUS). The effects of both algorithm and resolution can be studied with this method. We find that, under typical molecular cloud conditions, global collapse can indeed be prevented, but density enhancements caused by strong shocks nevertheless become gravitationally unstable and collapse into dense cores and, presumably, stars. The occurance and efficiency of local collapse decreases as the driving wave length decreases and the driving strength increases. It appears that local collapse can only be prevented entirely with unrealistically short wave length driving, but observed core formation rates can be reproduced with more realistic driving. At high collapse rates, cores are formed on short time scales in coherent structures with high efficiency, while at low collapse rates they are scattered randomly throughout the region and exhibit considerable age spread. We suggest that this naturally explains the observed distinction between isolated and clustered star formation.

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