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dc.contributor.authorAznar Siguan, Gabriela
dc.contributor.authorGarcía-Berro Montilla, Enrique
dc.contributor.authorLorén Aguilar, Pablo
dc.contributor.authorSoker, Noam
dc.contributor.authorKashi, Amit
dc.contributor.otherUniversitat Politècnica de Catalunya. Departament de Física
dc.date.accessioned2016-01-13T13:50:35Z
dc.date.available2016-01-13T13:50:35Z
dc.date.issued2015-07-01
dc.identifier.citationAznar, G., Garcia-berro, E., Loren, P., Soker, N., Kashi, A. Smoothed particle hydrodynamics simulations of the core-degenerate scenario for Type Ia supernovae. "Monthly notices of the Royal Astronomical Society", 01 Juliol 2015, vol. 450, núm. 3, p. 2948-2962.
dc.identifier.issn0035-8711
dc.identifier.urihttp://hdl.handle.net/2117/81353
dc.description.abstractThe core-degenerate scenario for Type Ia supernovae involves the merger of the hot core of an asymptotic giant branch star and a white dwarf, and might contribute a non-negligible fraction of all thermonuclear supernovae. Despite its potential interest, very few studies, and based on only crude simplifications, have been devoted to investigate this possible scenario, compared with the large efforts invested to study some other scenarios. Here we perform the first three-dimensional simulations of the merger phase, and find that this process can lead to the formation of a massive white dwarf, as required by this scenario. We consider two situations, according to the mass of the circumbinary disc formed around the system during the final stages of the common envelope phase. If the disc is massive enough, the stars merge on a highly eccentric orbit. Otherwise, the merger occurs after the circumbinary disc has been ejected and gravitational wave radiation has brought the stars close enough for the secondary to overflow its Roche lobe radius. Not surprisingly, the overall characteristics of the merger remnants are similar to those found for the double-degenerate scenario, independently of the very different core temperature and of the orbits of the merging stars. They consist of a central massive white dwarf, surrounded by a hot, rapidly rotating corona and a thick debris region.
dc.format.extent15 p.
dc.language.isoeng
dc.rights.urihttp://creativecommons.org/licenses/by-nc-nd/3.0/es/
dc.subjectÀrees temàtiques de la UPC::Física::Astronomia i astrofísica
dc.subject.lcshWhite dwarf stars
dc.subject.lcshSupernovae
dc.subject.otherhydrodynamics
dc.subject.otherstars: AGB and post-AGB
dc.subject.otherbinaries: close
dc.subject.othersupernovae: general
dc.subject.otherwhite dwarfs
dc.subject.otherACCRETING WHITE-DWARFS
dc.subject.otherDYNAMICAL INTERACTIONS
dc.subject.otherSURFACE DETONATIONS
dc.subject.otherHELIUM DETONATIONS
dc.subject.otherCARBON IGNITION
dc.subject.otherMERGER REMNANTS
dc.subject.otherTRIPLE-SYSTEMS
dc.subject.otherRAY-BURSTS
dc.subject.otherEVOLUTION
dc.subject.otherPROGENITORS
dc.titleSmoothed particle hydrodynamics simulations of the core-degenerate scenario for Type Ia supernovae
dc.typeArticle
dc.subject.lemacEstels nans
dc.subject.lemacSupernoves
dc.contributor.groupUniversitat Politècnica de Catalunya. CTE-CRAE - Grup de Recerca en Ciències i Tecnologies de l'Espai
dc.contributor.groupUniversitat Politècnica de Catalunya. GAA - Grup d'Astronomia i Astrofísica
dc.identifier.doi10.1093/mnras/stv824
dc.description.peerreviewedPeer Reviewed
dc.rights.accessOpen Access
local.identifier.drac16674463
dc.description.versionPostprint (published version)
local.citation.authorAznar, G.; Garcia-berro, E.; Loren, P.; Soker, N.; Kashi, A.
local.citation.publicationNameMonthly notices of the Royal Astronomical Society
local.citation.volume450
local.citation.number3
local.citation.startingPage2948
local.citation.endingPage2962


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