A mathematical model of the initial stage in the formation of a disk galaxy

Details A mathematical model of the initial stage in the formation of a disk galaxy A mathematical model of the initial stage in the formation of a disk galaxy

Feb 1986

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986ap%26ss.119..201b&link_type=abstract

(IAU, Asian-Pacific Regional Meeting, 3rd, Kyoto, Japan, Sept. 30-Oct. 5, 1984) Astrophysics and Space Science (ISSN 0004-640X),

Astronomy and Astrophysics

Astrophysics

Astronomical Models, Cosmic Gases, Disk Galaxies, Galactic Evolution, Gravitational Collapse, Galactic Bulge, Interstellar Magnetic Fields, Mathematical Models, Rotating Fluids, Stellar Evolution

Scientific paper

The collapse of a homogeneous, initially spheroidal halo under self gravitation, has been considered. A thick stellar disk is formed within a time-scale <3×109yr. Brisk star formation takes place while the collapse of the gaseous disk is still in progress. This gives rise to the halo stars with low metal content and high Z-motion. A bulge is formed at the centre simultaneously. This is the first phase of formation of a disk galaxy. The thin disk is formed at a later stage as the remaining primordial gas and the gas released by the evolution of stars in the thick disk gradually settles on to it. The presented model is rather a crude one.

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