Hostname: page-component-745bb68f8f-d8cs5 Total loading time: 0 Render date: 2025-01-24T18:25:43.876Z Has data issue: false hasContentIssue false
  • English
  • Français

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
Get access Rights & Permissions [Opens in a new window]

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

Access options

Get access to the full version of this content by using one of the access options below. (Log in options will check for institutional or personal access. Content may require purchase if you do not have access.)

References

Fowler, W. and Hoyle, F., 1963, Roy. Obs. Bull., No. 67.Google Scholar
Goldreich, P. and Lynden-Bell, D., 1965, Mon. Not. R. astr. Soc., 130, 125.CrossRefGoogle Scholar
Hachisu, I. and Eriguchi, Y., 1985, Astr. Astrophys., 143, 355.Google Scholar
Hoyle, F., 1953, Astrophys. J., 118, 513.CrossRefGoogle Scholar
Hunter, C., 1970a, Astrophys. J., 162, 97.CrossRefGoogle Scholar
Hunter, C., 1970b, Astrophys. J., 162, 445.CrossRefGoogle Scholar
Keto, E. R. and Lattanzio, J. C, 1989, Astrophys. J., 346, 182.CrossRefGoogle Scholar
Keto, E. R., Lattanzio, J. C. and Monaghan, J. J., 1991, Astrophys. J., 383, 639.CrossRefGoogle Scholar
Larson, R. B., 1985, Mon. Not. Roy. astr. Soc., 214, 379.CrossRefGoogle Scholar
Lattanzio, J. C. and Henriksen, R. N., 1988, Mon. Not. R. astr. Soc., 232, 565.CrossRefGoogle Scholar
Miyama, S. M., Hayashi, C. and Narita, S., 1984, Astrophys. J., 279, 621.CrossRefGoogle Scholar
Monaghan, J. J. and Lattanzio, J. C, 1991, Astrophys. J., 375, 177.CrossRefGoogle Scholar
Monaghan, J. J. and Varnas, S., 1988, Mon. Not. Roy. astr. Soc., 231, 515.CrossRefGoogle Scholar
Murray, S. D. and Lin, D. N. C, 1989, Astrophys. J., 339, 933.CrossRefGoogle Scholar
Stahler, S. W., 1983, Astrophys. J., 268, 165.CrossRefGoogle Scholar
Toomre, A., 1964, Astrophys. J., 139, 1217.CrossRefGoogle Scholar