Collapse of the Spherical Stellar System
Abstract
A new numerical method is proposed for solving the problems connected with the evolution of spherical clusters. The method is based upon the solution of the algebraic equations describing the motions of spherical shells. The stage of the collapse of a typical cluster is 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% of the initial one. The density distribution of the outer part of the cluster approximately corresponds to a profile of ρ ∝R ^{3.3}.
 Publication:

Astrophysics and Space Science
 Pub Date:
 March 1984
 DOI:
 10.1007/BF00651607
 Bibcode:
 1984Ap&SS.100..319I
 Keywords:

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