Statistics – Computation
Scientific paper
Feb 1984
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984apj...277..744r&link_type=abstract
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 277, Feb. 15, 1984, p. 744-767.
Statistics
Computation
114
Astronomical Models, Galactic Structure, Mean Free Path, Spiral Galaxies, Star Formation, Density Wave Model, Gravitational Effects, H Ii Regions, Interstellar Matter, Many Body Problem, Supernova Remnants
Scientific paper
The authors present a model of the interstellar medium (ISM) 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). In the presence of a spiral-perturbed galactic gravitational field, the cloud distribution responds with a strong global density wave (galactic shock), with clouds concentrated in spiral arms. The appearance of large cloud-particle clumps in the spiral arms of the computations suggests how easily real clouds can agglomerate into giant complexes in spiral arms. The population of young stellar associations in the model exhibits a coherent spiral pattern in all cases for which cloud collisions are an important star formation mechanism. In contrast, a case for which sequential star formation dominates is unsteady and shows only transient spiral structure.
Hausman Mark A.
Roberts William W. Jr.
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