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.Comment: Talk given at the Strasbourg meeting Massive Star Clusters in
November 1999; 7 pages, 3 figures xv-8bit giffed and tarred (= 100Kbytes);
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