Gravitational collapse of cosmic gas clouds and formation of star clusters

Details Gravitational collapse of cosmic gas clouds and formation of star clusters Gravitational collapse of cosmic gas clouds and formation of star clusters

Oct 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984ap%26ss.105...85b&link_type=abstract

Astrophysics and Space Science (ISSN 0004-640X), vol. 105, no. 1, Oct. 1984, p. 85-97.

Astronomy and Astrophysics

Astrophysics

1

Cosmic Gases, Gravitational Collapse, Protostars, Star Clusters, Stellar Evolution, Density Distribution, Fragmentation, Stellar Mass Accretion, Stellar Models

Scientific paper

The gravitational collapse of cosmic gas clouds and formation of star clusters has been considered. Hoyle's view of successive fragmentation (1953) has been taken as the basic mechanism. The initial masses of protostars have been estimated as the function of their distances from the center of the cluster and the intensity of the magnetic field of the medium. It has been shown that the fragmentation process is greatly inhibited by the presence of a strong magnetic field. A model has been constructed showing how a protostar grows in mass by accretion from the surrounding medium, on the basis of the assumption that as the star moves at random in the cluster it picks up a fraction of the material through which it passes. It has been estimated that a protostar of initial mass of about 0.1 solar mass grows to one of 1.0 solar mass in a time period which ranges from a few multiples of 100,000 yr to a few multiples of 10 Myr, depending on the parameters involved in the accretion process. The number of stars per unit mass range has also been estimated; it is found to be proportional to m exp (-3.3), m being the mass of the star.

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