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Title:
Single Star Progenitors for Type Ia Supernovae
Authors:
Tout, Christopher A.; Wickramasinghe, Dayal T.; Lattanzio, John C.
Affiliation:
AA(Institute of Astronomy, The Observatories, Madingley Road, Cambridge CB3 0HA, England), AB(Department of Mathematics, The Australian National University, Canberra, ACT 0200, Australia), AC(Centre for Stellar and Planetary Astrophysics, School of Mathematics, Monash University, Clayton, Victoria 3800, Australia)
Publication:
IXTH TORINO WORKSHOP ON EVOLUTION AND NUCLEOSYNTHESIS IN AGB STARS AND THE IIND PERUGIA WORKSHOP ON NUCLEAR ASTROPHYSICS. AIP Conference Proceedings, Volume 1001, pp. 25-32 (2008). (AIPC Homepage)
Publication Date:
04/2008
Origin:
AIP
PACS Keywords:
Supernovae, Abundances, chemical composition, Faint blue stars , white dwarfs, degenerate stars, nuclei of planetary nebulae, Stellar structure, interiors, evolution, nucleosynthesis, ages, Mass loss and stellar winds
DOI:
10.1063/1.2916973
Bibliographic Code:
2008AIPC.1001...25T

Abstract

Type Ia supernovae are identified as exploding degenerate stars. Their luminosity is due to the radioactive decay of about a solar mass of 56Ni through 56Co to 56Fe. Although it is generally accepted that a degenerate carbon/oxygen white dwarf explodes as it accretes material from a binary companion, the progenitors of type Ia supernovae have not been categorically identified. The cores of intermediate mass asymptotic giant branch stars are composed of carbon and oxygen in a degenerate state. We discuss conditions under which carbon can ignite at the centre of such a core and when the ensuing explosion would appear as a type Ia supernova.
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