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Single Star Progenitors for Type Ia Supernovae

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dc.contributor.authorTout, Christopher A
dc.contributor.authorWickramasinghe, Dayal
dc.contributor.authorLattanzio, John
dc.coverage.spatialPerugia Italy
dc.date.accessioned2015-12-07T22:43:13Z
dc.date.createdOctober 22-26 2007
dc.date.issued2008
dc.date.updated2016-02-24T10:35:11Z
dc.description.abstractType 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.
dc.identifier.isbn9780735405202
dc.identifier.urihttp://hdl.handle.net/1885/24909
dc.publisherAmerican Institute of Physics (AIP)
dc.relation.ispartofseriesTorino Workshop on Evolution and Nucleosynthesis in AGB Stars 2007
dc.sourceAIP Conference Proceedings
dc.source.urihttp://proceedings.aip.org/proceedings/
dc.subjectKeywords: AGB and Post-AGB; General; Mass-Loss; Stars; Supernovae; White Dwarfs
dc.titleSingle Star Progenitors for Type Ia Supernovae
dc.typeConference paper
local.bibliographicCitation.lastpage32
local.bibliographicCitation.startpage25
local.contributor.affiliationTout, Christopher A, University of Cambridge
local.contributor.affiliationWickramasinghe, Dayal, College of Physical and Mathematical Sciences, ANU
local.contributor.affiliationLattanzio, John, Monash University
local.contributor.authoruidWickramasinghe, Dayal, u7600909
local.description.embargo2037-12-31
local.description.notesImported from ARIES
local.description.refereedYes
local.identifier.absfor020110 - Stellar Astronomy and Planetary Systems
local.identifier.ariespublicationu4085724xPUB35
local.identifier.doi10.1063/1.2916973
local.identifier.scopusID2-s2.0-84861766865
local.type.statusPublished Version

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