Modelling the composition of a young star cluster ejecta

Abstract

We have computed with a fine time grid the evolution of the elemental abundances of He, C, N and O ejected by a young (t < 20 Myr) and massive (M$=10^6$\,\Msun) 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 Msun) 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 over-abundant in N for all initial abundances and in He, C and O for initial abundances higher than 1/5th Solar. The C and O abundance in the cluster ejecta can reach over 50 times the solar value with important consequences for the chemical and hydrodynamical evolution of the surrounding ISM.

13 pages, 10 figures, 7 tables, accepted by MNRAS

References in corpus (5)

• The chemical composition of the Sun
• Galactic chemical evolution: Carbon through Zinc
• Very low metallicity massive star models: Pre-SN evolution and primary nitrogen production
• Massive star formation in Wolf-Rayet galaxies. IV: Colours, chemical composition analysis and metallicity-luminosity relations
• Rotating massive stars: Pre-SN models and stellar yields at solar metallicity

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• A massive bubble of extremely metal poor gas around a collapsing Ly-alpha blob at z=2.54
• Are Wolf-Rayet stars able to pollute the interstellar medium of galaxies? Results from the integral field spectroscopy
• Discovery of new N-emitters over a wide redshift range