Volume 435, Number 1, May III 2005
|Page(s)||231 - 237|
|Section||Stellar structure and evolution|
|Published online||25 April 2005|
The gravitational collapse of ONe electron-degenerate cores and white dwarfs: The role of Mg and C revisited
Departament de Física Aplicada, Escola Politécnica Superior de Castelldefels, Universitat Politècnica de Catalunya, Avda. del Canal Olímpic s/n, 08860 Castelldefels, Spain e-mail: firstname.lastname@example.org
2 Departament d'Astronomia i Meteorologia, Universitat de Barcelona, Facultat de Física, Martí i Franquès 1, 08028 Barcelona, Spain
3 Institute for Space Studies of Catalonia, c/Gran Capità 2–4, Edif. Nexus 104, 08034 Barcelona, Spain
4 Special Research Center in Astrophysics, Particle Physics and Cosmology, University of Barcelona, Martí i Franquès 1, 08028 Barcelona, Spain
Accepted: 23 January 2005
The final stages of the evolution of electron-degenerate ONe cores, resulting from carbon burning in “heavy weight” intermediate-mass stars () and growing in mass, either from carbon burning in a shell or from accretion of matter in a close binary system, are examined in the light of their detailed chemical composition. In particular, we have modelled the evolution taking into account the abundances of the following minor nuclear species, which result from the previous evolutionary history: 12C, 23Na, 24Mg, and 25Mg. Both 23Na and 25Mg give rise to Urca processes, which are found to be unimportant for the final outcome of the evolution. 24Mg was formerly considered a major component of ONe cores (hence called ONeMg cores), but updated evolutionary calculations in this mass range have severely reduced its abundance. Nevertheless, we have parameterized it and we have found that the minimum amount of 24Mg required to produce NeO burning at moderate densities is 23%, a value exceedingly high in the light of recent evolutionary models. Finally, we have determined that models with relatively small abundances of unburnt carbon () could be a channel to explosion at low to moderate density (∼ g cm-3). This is clearly below the current estimate for the explosion/collapse threshold and would have interesting consequences.
Key words: nuclear reactions, nucleosynthesis, abundances / stars: evolution / stars: interiors / white dwarfs / supernovae: general
© ESO, 2005
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