Issue |
A&A
Volume 433, Number 3, April III 2005
|
|
---|---|---|
Page(s) | 1037 - 1046 | |
Section | Stellar structure and evolution | |
DOI | https://doi.org/10.1051/0004-6361:20041755 | |
Published online | 29 March 2005 |
Carbon burning in intermediate-mass primordial stars
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;garcia]@fa.upc.es
2
Department of Physics, Hokkaido University, Sapporo, Hokkaido 060–0810, Japan
3
Meme Media Laboratory, Hokkaido University, Sapporo, Hokkaido 060–0813, Japan
4
Institute for Space Studies of Catalonia, c/Gran Capità 2–4, Edif. Nexus 104, 08034 Barcelona, Spain
Received:
29
July
2004
Accepted:
2
December
2004
The evolution of a zero metallicity star is
computed, analyzed and compared with that of a solar metallicity star
of identical ZAMS mass. Our computations range from the main sequence
until the formation of a massive oxygen-neon white dwarf. Special
attention has been payed to carbon burning in conditions of partial
degeneracy as well as to the subsequent thermally pulsing Super-AGB
phase. The latter develops in a fashion very similar to that of a
solar metallicity
star, as a consequence of the
significant enrichment in metals of the stellar envelope that ensues
due to the so-called third dredge-up episode. The abundances in
mass of the main isotopes in the final ONe core resulting from the
evolution are
O
,
Ne
and
Mg
. This core is surrounded by a
buffer mainly composed of carbon and oxygen, and on top of
it a He envelope of mass ∼
.
Key words: stars: evolution / stars: abundances / stars: AGB and post-AGB / stars: interiors
© ESO, 2005
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