We discuss the results of N-body simulations of intermediate-mass young star clusters (SCs) with three different metallicities (Z = 0.01, 0.1 and 1 Z(circle dot)), including metallicity-dependent stellar evolution recipes and metallicity-dependent prescriptions for stellar winds and remnant formation. The initial half-mass relaxation time of the simulated young SCs (similar to 10 Myr) is comparable to the lifetime of massive stars. We show that mass-loss by stellar winds influences the reversal of core collapse and the expansion of the half-mass radius. In particular, the post-collapse re-expansion of the core is weaker for metal-poor SCs than for metal-rich SCs, because the former lose less mass (through stellar winds) than the latter. As a consequence, the half-mass radius expands faster in metal-poor SCs. The difference in the half-light radius between metal-poor SCs and metal-rich SCs is (up to a factor of 2) larger than the difference in the half-mass radius.
http://hdl.handle.net/20.500.11767/11743
Titolo: | Impact of metallicity on the evolution of young star clusters |
Autori: | Mapelli M.; Bressan A |
Rivista: | |
Data di pubblicazione: | 2013 |
Volume: | 430 |
Fascicolo: | 4 |
Pagina iniziale: | 3120 |
Pagina finale: | 3127 |
Digital Object Identifier (DOI): | 10.1093/mnras/stt119 |
Fulltext via DOI: | 10.1093/mnras/stt119 |
Appare nelle tipologie: | 1.1 Journal article |
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