Coalescence of self-gravitating gaseous masses - A numerical model

Details Coalescence of self-gravitating gaseous masses - A numerical model Coalescence of self-gravitating gaseous masses - A numerical model

Dec 1988

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988azh....65.1155b&link_type=abstract

Astronomicheskii Zhurnal (ISSN 0004-6299), vol. 65, Nov.-Dec. 1988, p. 1155-1163. In Russian.

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Astronomical Models, Coalescing, Galactic Evolution, Galactic Mass, Gas Dynamics, Angular Momentum, Chemical Composition, Gravitational Collapse, Radiant Cooling, Shock Waves

Scientific paper

A criterion of coalescence for self-gravitating gaseous masses of galactic scale with primeval chemical composition and radiative cooling is found using a two-dimensional numerical gas-dynamical model of the non-central supersonic collision of masses. The results of a series of computations are presented for a wide range of impact parameters and relative velocities of collision. It is shown that coalescence can lead to the formation of a gaseous protogalaxy with a considerable amount of angular momentum. The authors discuss briefly an evolutionary scenario for separation within the collapsing and fragmentating protogalaxy of two dynamical subsystems - a rapidly rotating disc and a slowly rotating halo.

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