Rotation, Statistical Dynamics and Kinematics of Globular Clusters

TL;DR

This paper explores the dynamics and evolution of globular clusters, focusing on rotation, mass segregation, and statistical equilibria, and discusses the formation of stellar streams in the galaxy's halo.

Contribution

It introduces a new model for the rotational evolution of globular clusters and generalizes Newton's N-body problem without violent relaxation.

Findings

Rotation proportional to square root of density during core collapse

Energy balance in globular clusters' dynamical main sequence

New statistical equilibrium in N-body problem

Abstract

Evolution with mass segregation and the evolution of the rotation of cores are both discussed for self-similar core collapse. Evolution with angular velocity proportional to the square root of the density is predicted. On the Dynamical Main Sequence of globular clusters the energy emission from binaries balances the energy expended in expanding the halo. Newton's exactly solved N-body problem is then given, along with recent generalisations, all of which have no violent relaxation, but a new type of statistical equilibrium is discussed. Finally, we set the creation of streams in the Galaxy's halo in the historical context of their discovery.