Dynamical evolution of globular clusters after core collapse.
Abstract
This review describes work on the evolution of a stellar system during the phase which starts at the end of core collapse. It begins with an account of the model of Henon, Goodman (1984), and Inagaki and LyndenBell (1983), as well as evaporative models, and modifications to these models which are needed in the core. Next, these models are related to more detailed numerical calculations of gaseous models, FokkerPlanck models, Nbody calculations, etc., and some problems for further work in these directions are outlined. The review concludes with a discussion of the relation between theoretical models and observations of the surface density profiles and statistics of actual globular clusters.
 Publication:

Dynamics of Star Clusters
 Pub Date:
 1985
 Bibcode:
 1985IAUS..113..139H
 Keywords:

 Computational Astrophysics;
 Globular Clusters;
 Gravitational Collapse;
 Stellar Evolution;
 Stellar Motions;
 Stellar Systems;
 Density Distribution;
 FokkerPlanck Equation;
 Many Body Problem;
 MaxwellBoltzmann Density Function;
 Stellar Models;
 Astrophysics;
 Collapse:Globular Clusters;
 Globular Clusters:Collapse;
 Globular Clusters:Dynamics;
 Globular Clusters:Evolution