Dynamical evolution of star clusters with top-heavy IMF. Issue Volume 14:Issue S351(2019) (May 2019)

• Record Type: Journal Article
• Authors: Haghi, Hosein; Safaei, Ghasem; Zonoozi, Akram H.; Kroupa, Pavel
• Editors: Bragaglia, Angela; Davies, Melvyn; Sills, Alison; Vesperini, Enrico
• Is Part Of: Proceedings of the International Astronomical Union. Volume 14:Issue S351(2019)
• Page Start: 447
• Page End: 450
• Publication Date: 2019-05
• Subjects: star clusters, -- N-body simulation, -- initial mass function; Astronomy -- Congresses; Astronomy -- Periodicals; 520
• DOI: 10.1017/S174392131900704X
• Languages: English
• ISSNs: 1743-9213

Abstract

Abstract: Several observational and theoretical studies suggest that the initial mass function (IMF) slope for massive stars in globular clusters (GCs) depends on the initial cloud density and metallicity, such that the IMF becomes increasingly top-heavy with decreasing metallicity and increasing the gas density of the forming object. Using N-body simulations of GCs starting with a top-heavy IMF and undergo early gas expulsion within a Milky Way-like potential, we show how such a cluster would evolve. By varying the degree of top-heaviness, we calculate the dissolution time and the minimum cluster mass needed for the cluster to survive after 12 Gyr of evolution.