Abstract
Abstract Gaseous models have proven to be a computationally cheap and reliable tool to investigate the dynamical behaviour of globular clusters. But to compete with other approaches for modelling the evolution of star clusters various important effects have to be taken into account. These are for example the dynamical effects of a stellar mass spectrum, stellar evolution, a consistent treatment of the tidal field of the galaxy, or primordial binaries. Here we report on the effects of a mass spectrum and stellar evolution on the dynamical evolution of the cluster's post-collapse evolution (gravothermal oscillations) and show how only small changes in the mass loss rate can change the internal dynamics of the cluster.
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