The Gravitational Collapse of Filaments: 1D RHD Simulations

Details The Gravitational Collapse of Filaments: 1D RHD Simulations The Gravitational Collapse of Filaments: 1D RHD Simulations

Dec 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999sf99.proc..193o&link_type=abstract

Star Formation 1999, Proceedings of Star Formation 1999, held in Nagoya, Japan, June 21 - 25, 1999, Editor: T. Nakamoto, Nobeyam

Mathematics

Metric Geometry

Scientific paper

We have performed radiation hydrodynamics (RHD) simulations in 1D axisymmetric geometry to study the gravitational collapse of the molecular clouds in star forming regions. Our results clearly show that the temperature of collapsing filamentary clouds depends on the heating rate and the cooling rate. Although the isothermality of the cloud in optically thin regime has been commonly assumed, we conclude the assumption is incorrect. A transition from the isothermal state to the non-isothermal state occurs when the cloud density exceeds the critical density at which the heating rate becomes equal to the cooling rate. The critical density depends not only on the optical depth but also on the temperature of the cloud.

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