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dc.contributor.authorCanals, Pere
dc.contributor.authorTorres Gil, Santiago
dc.contributor.authorSoker, Noam
dc.contributor.otherUniversitat Politècnica de Catalunya. Departament de Física
dc.date.accessioned2019-01-25T12:51:46Z
dc.date.available2019-01-25T12:51:46Z
dc.date.issued2018-11-01
dc.identifier.citationCanals, P.; Torres, S.; Soker, N. Oxygen-neon-rich merger during common envelope evolution. "Monthly notices of the Royal Astronomical Society", 1 Novembre 2018, vol. 480, núm. 4, p. 4519-4525.
dc.identifier.issn0035-8711
dc.identifier.urihttp://hdl.handle.net/2117/127601
dc.description.abstractWe conduct a population synthesis study of the common envelope evolution (CEE) of a white dwarf (WD) and an asymptotic giant branch (AGB) star and find that the potential number of type Ia supernovae (SNe Ia) from the core degenerate (CD) and from the double degenerate (DD) scenarios are of the same order of magnitude. For the CD scenario we consider cases where a carbon oxygen rich (CO) AGB core and a CO WD merge during the CEE and leave a WD remnant with a mass of >1.35Mo, and for the DD scenario we count surviving CO WD binary systems that merge within a time of 10 Gyr. When either the AGB core or the WD are oxygen neon rich (ONe) we assume that the outcome might be a peculiar SN Ia. We find that the number of potential peculiar SNe Ia in the channels we study, that do not include peculiar SNe Ia that involve helium WDs or helium donors, is non-negligible, but less than the number of normal SNe Ia. If a SN Ia or a peculiar SN Ia explosion takes place within about million year after CEE, whether in the CD scenario or in the DD scenario, a massive circumstellar matter is present at explosion time. Our results are compatible with the suggestion that Chandrasekhar-mass SNe Ia mostly come from the CD scenario, and sub-Chandrasekhar SNe Ia mostly come from the DD scenario.
dc.format.extent7 p.
dc.language.isoeng
dc.publisherOxford University Press
dc.rightsAttribution-NonCommercial-NoDerivs 3.0 Spain
dc.rights.urihttp://creativecommons.org/licenses/by-nc-nd/3.0/es/
dc.subjectÀrees temàtiques de la UPC::Física::Astronomia i astrofísica
dc.subject.lcshAsymptotic giant branch stars
dc.subject.lcshWhite dwarf stars
dc.subject.otherstars: AGB and post-AGB
dc.subject.otherbinaries: close
dc.subject.othersupernovae: general-white dwarfs
dc.titleOxygen-neon-rich merger during common envelope evolution
dc.typeArticle
dc.subject.lemacEstels nans
dc.contributor.groupUniversitat Politècnica de Catalunya. GAA - Grup d'Astronomia i Astrofísica
dc.identifier.doi10.1093/mnras/sty2121
dc.description.peerreviewedPeer Reviewed
dc.relation.publisherversionhttps://academic.oup.com/mnras/article-abstract/480/4/4519/5067319
dc.rights.accessOpen Access
local.identifier.drac23611901
dc.description.versionPreprint
dc.relation.projectidinfo:eu-repo/grantAgreement/AEI/Plan Estatal de Investigación Científica y Técnica y de Innovación 2013-2016/AYA2017-86274-P/ES/DEL ENFRIAMIENTO A LAS EXPLOSIONES: LA FISICA DE LOS OBJETOS COMPACTOS/
dc.relation.projectidinfo:eu-repo/grantAgreement/AGAUR/SGR2017-661
local.citation.authorCanals, P.; Torres, S.; Soker, N.
local.citation.publicationNameMonthly notices of the Royal Astronomical Society
local.citation.volume480
local.citation.number4
local.citation.startingPage4519
local.citation.endingPage4525


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