Abstract
The sequence of events determining the initial stages of star formation is analyzed in framework of the self-enrichment scenario. The computations are based on a single-zone chemo-dynamical model. It is shown that the first episode of star formation was characterized by an initial mass function shifted toward massive stars (M ≥ 8M ⊙). We argue that the transition to a star formation with a normal (Salpeter) initial mass function was due to more efficient radiative cooling of the proto-globular cluster gas after its enrichment to a metallicity of Z ∼ 0.02 Z ⊙ in agreement with those observed in globular clusters.
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Translated from Astronomicheski\(\overset{\lower0.5em\hbox{$\smash{\scriptscriptstyle\smile}$}}{l}\) Zhurnal, Vol. 82, No. 11, 2005, pp. 967–975.
Original Russian Text Copyright © 2005 by Kas’yanova, Shchekinov.
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Kas’yanova, M.V., Shchekinov, Y.A. The chemical evolution of globular clusters. Astron. Rep. 49, 863–870 (2005). https://doi.org/10.1134/1.2127990
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DOI: https://doi.org/10.1134/1.2127990