Numerical experiments on galaxy formation. I - Introduction and first results

Details Numerical experiments on galaxy formation. I - Introduction and first results Numerical experiments on galaxy formation. I - Introduction and first results

Mar 1981

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1981apj...244..467m&link_type=abstract

Astrophysical Journal, Part 1, vol. 244, Mar. 1, 1981, p. 467-475.

Other

6

Astronomical Models, Dynamic Models, Galactic Evolution, Gravitational Collapse, Interstellar Gas, Stellar Evolution, Galactic Mass, Galactic Structure, Gas Dynamics, Gravitational Fields, Mathematical Models

Scientific paper

The large, fully three-dimensional n-body programs designed for numerical experiments on the dynamics of galaxies have been used for investigations of protogalactic collapses. The dynamical aspects of galaxy formation dominate in this approach. The present experiments start from a large rotating gaseous mass that is made up of many gas clouds. The large mass collapses because it is out of equilibrium. Stars form as the collapse proceeds. The problem is formulated, limiting-case examples are described, and results from simple 'first cut' models are given. Results with no star formation are contrasted with results for very rapid star formation. All models with gas formed thin disklike structures; some were circular, while others were oval. The principal result from the simple models is that stars continue to form rapidly even after the gas has been depleted to unacceptably low levels (1% of the galactic mass in gas).

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