On one type of models of spherical stellar clusters.
Abstract
The estimates of the time of star transitions between halo and core in spherical clusters as a result of stellar encounters are given. Numerical integration of grossevolution equations for quasistationary and nonstationary (in a regular field) stellar clusters has been performed. There are three possible types of "halocore" structure evolution in the quasistationary stellar clusters depending upon the initial conditions. All the open stellar clusters evolve near a certain sequence in the space of grossparameters ξ and μ during the most of their lifetime. The parameters ξ and μ are the ratio of core radius to halo radius and the ratio of core mass to halo mass, respectively. The majority of open clusters must be concentrated near the sequence ξ = ξ(μ). This sequence corresponds to the balance of rates of transitions between core and halo during the cluster relaxation. The results of comparison of the author's cluster model calculations with observations and numerical Nbody experiments are discussed.
 Publication:

Kinematika i Fizika Nebesnykh Tel
 Pub Date:
 October 1991
 Bibcode:
 1991KFNT....7...75D
 Keywords:

 Gravitational Effects;
 Star Clusters;
 Stellar Cores;
 Stellar Evolution;
 Center Of Mass;
 Numerical Integration;
 RungeKutta Method;
 Astrophysics