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Modelling the composition of a young star cluster ejecta




We have computed with a fine time grid the evolution of the elemental abundances of He, C, N and O ejected by young (t < 20 Myr) and massive (M = 106 M) coeval stellar cluster with a Salpeter initial mass function (IMF) over a wide range of initial abundances. Our computations incorporate the mass loss from massive stars (M ≥ 30 M) during their wind phase including the Wolf–Rayet phase and the ejecta from the core-collapse supernovae. We find that during the Wolf–Rayet phase (t < 5 Myr) the cluster ejecta composition suddenly becomes vastly overabundant in N for all initial abundances and in He, C and O for initial abundances higher than one-fifth of the solar. The C and O abundances in the cluster ejecta can reach over 50 times the solar value with important consequences for the chemical and hydrodynamical evolution of the surrounding interstellar medium.

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