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Star formation in a density-wave-dominated, cloudy interstellar medium

Published online by Cambridge University Press:  04 August 2017

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We present a model of the interstellar medium in spiral galaxies. The ISM is simulated by a system of particles, representing gas clouds. It is a probabilistic N-body system in which “cloud” particles orbit ballistically, undergo dissipative collisions with other clouds, and experience velocity-boosting interactions with expanding supernova remnants (SNRs). Associations of protostars may form in clouds following collisions or SNR interactions (thus allowing sequential star formation); these associations take finite times before becoming active and undergoing their own SN events (Roberts and Hausman, 1983; Hausman and Roberts, 1983).

Type
PART III: Dynamics and Evolution
Information
Symposium - International Astronomical Union , Volume 106: The Milky Way Galaxy , 1985 , pp. 567 - 570
Copyright
Copyright © Reidel 1985 

References

Hausman, M. A., and Roberts, W. W., 1983, Ap. J. (in preparation).Google Scholar
Roberts, W. W., and Hausman, M. A., 1983, Ap. J. (submitted for publication).Google Scholar