The late stages of the evolution of intermediate-mass primordial stars: the effects of overshooting

Free access article

Issue		A&A Volume 464, Number 2, March III 2007


Page(s)		667 - 682
Section		Stellar structure and evolution
DOI		http://dx.doi.org/10.1051/0004-6361:20065641

A&A 464, 667-682 (2007)
DOI: 10.1051/0004-6361:20065641

The late stages of the evolution of intermediate-mass primordial stars: the effects of overshooting

P. Gil-Pons¹, J. Gutiérrez¹, and E. García-Berro^{1, 2}

¹ Departament de Física Aplicada, Escola Politécnica Superior de Castelldefels, Universitat Politècnica de Catalunya, Avda. del Canal Olímpic s/n, 08860 Castelldefels, Spain
e-mail: [pilar;jordi;garcia]@fa.upc.edu
² Institute for Space Studies of Catalonia, c/Gran Capità 2-4, Edif. Nexus 104, 08034 Barcelona, Spain

(Received 19 May 2006 / Accepted 6 December 2006)

Abstract
Aims.We compute and analyze the evolution of primordial stars of masses at the ZAMS between $5 \, M_{\odot}$ and $10 \, M_{\odot}$ , with and without overshooting. Our main goals are to determine the nature of the remnants of massive intermediate-mass primordial stars and to check the influence of overshooting in their evolution.
Methods.Our calculations cover stellar evolution from the main sequence phase until the formation of the degenerate cores and the thermally pulsing phase.
Results.We have obtained the values for the limiting masses of Population III progenitor stars leading to carbon-oxygen and oxygen-neon compact cores. Moreover, we have also obtained the limiting mass for which isolated primordial stars would lead to core-collapse supernovae after the end of the main central burning phases. Considering a moderate amount of overshooting, the mass thresholds at the ZAMS for the formation of carbon-oxygen and oxygen-neon degenerate cores shift to smaller values by about $2\, M_{\odot}$ . As a by-product of our calculations, we have also obtained the structure and composition profiles of the resulting compact remnants.
Conclusions.As opposed to what happens with solar metallicity objects, the final fate of primordial stars is not straightforwardly determined from the mass of the compact cores at the end of carbon burning. Instead, the small mass-loss rates typically associated with stellar winds of low metallicity stars might allow the growth of the resulting degenerate cores up to the Chandrasekhar mass, on time scales one or two orders of magnitude shorter than the time required to lose the envelope. This would lead to the formation of supernovae for initial masses as small as ~ $5 \, M_{\odot}$ .

Key words: stars: evolution -- stars: AGB and post-AGB -- stars: white dwarfs -- stars: supernovae: general

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