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Numerical Modelling of Star Formation in GMCs

Published online by Cambridge University Press:  25 April 2016

John C. Lattanzio  and
J.J. Monaghan
John C. Lattanzio
Affiliation:
Mathematics Department, Monash University, Clayton, VIC 3168
J.J. Monaghan
Affiliation:
Mathematics Department, Monash University, Clayton, VIC 3168
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Abstract

Although stars can be approximated very satisfactorily by spherical models, it is clear from observations of star forming regions that the break-up of molecular gas to form proto-stars is a highly complex process that cannot be approximated simply. As a consequence, the theoretical picture of fragmentation, which is based on assuming that fragmentation occurs in uniform, static, isothermal clouds, is too crude to provide a guide to the star formation process. The alternative is to simulate the fragmentation process numerically with the ultimate aim of evolving the gas to proto-stars. The difficulties involved with this procedure are discussed in this paper. We also discuss our proposed solution to this problem, together with a very preliminary calculation.

Type
Galactic and Stellar
Information
Publications of the Astronomical Society of Australia , Volume 10 , Issue 2 , 1992 , pp. 122 - 124
Copyright
Copyright © Astronomical Society of Australia 1992

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