A new method to create initially mass segregated star clusters in virial equilibrium

Abstract

Mass segregation stands as one of the most robust features of the dynamical evolution of self-gravitating star clusters. In this paper we formulate parametrised models of mass segregated star clusters in virial equilibrium. To this purpose we introduce mean inter-particle potentials for statistically described unsegregated systems and suggest a single-parameter generalisation of its form which gives a mass-segregated state. We describe an algorithm for construction of appropriate star cluster models. Their stability over several crossing-times is verified by following the evolution by means of direct N-body integration.

9 pages, 8 figures, accepted for publication in MNRAS

References in corpus (7)

• On the variation of the Initial Mass Function
• Star formation through gravitational collapse and competitive accretion
• A dynamical origin for early mass segregation in young star clusters
• The secrets of the nearest starburst cluster: II. The present-day mass function in NGC 3603
• Formation and evolution of clumpy tidal tails around globular clusters
• Parameters of core-collapse
• Central energy equipartition in multi-mass models of globular clusters

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