The Impact of Rotation on Cluster Dynamics
Abstract
Description
The evolution of rotating, isolated clusters of stars up to core-collapse is investigated with n-body numerical codes. The simulations start off from axisymmetric generalisations of King profiles, with added global angular momentum. In this contribution I report on results obtained for two sets of single-mass cluster simulations. These confirm the more rapid evolution of even mildly-rotating clusters. A model is presented with rotational energy comparable to omega-Centauri's; it reaches core-collapse in less than half the time required for non-rotating model clusters.
Talk given at the Strasbourg meeting Massive Star Clusters in November 1999; 7 pages, 3 figures xv-8bit giffed and tarred (= 100Kbytes); newpasp style file included
Talk given at the Strasbourg meeting Massive Star Clusters in November 1999; 7 pages, 3 figures xv-8bit giffed and tarred (= 100Kbytes); newpasp style file included