Collapse of the spherical stellar system

Details Collapse of the spherical stellar system Collapse of the spherical stellar system

Mar 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984ap%26ss.100..319i&link_type=abstract

Astrophysics and Space Science (ISSN 0004-640X), vol. 100, no. 1-2, March 1984, p. 319-328.

Astronomy and Astrophysics

Astrophysics

11

Density Distribution, Galactic Evolution, Gravitational Collapse, Star Clusters, Stellar Evolution, Stellar Systems, Halos, Hubble Constant

Scientific paper

A new numerical method is proposed for solving problems connected with the evolution of spherical clusters. The method is based upon the solution of algebraic equations describing the motions of spherical shells. The stages of the collapse of a typical cluster are considered. The initial configuration is taken as a system with a uniform density distribution and with velocities much less than the virial ones. The model close to a stationary one has been obtained. The mass of the stationary cluster comprises about 60 percent of the initial one. The density distribution of the outer part of the cluster approximately corresponds to a profile proportional to R to the power of -3.3.

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