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dc.contributor.authorYamaguchi, H
dc.contributor.authorBadenes, Carles
dc.contributor.authorFoster, Adam
dc.contributor.authorBravo Guil, Eduardo
dc.contributor.authorWilliams, Brian
dc.contributor.authorMaeda, Keichi
dc.contributor.authorNobukawa, Masayoshi
dc.contributor.authorEriksen, Kristoffer
dc.contributor.authorBrickhouse, Nancy
dc.contributor.authorPetre, Robert
dc.contributor.authorKoyama, Katsuyi
dc.contributor.otherUniversitat Politècnica de Catalunya. Departament de Física i Enginyeria Nuclear
dc.date.accessioned2015-06-08T13:05:55Z
dc.date.created2015-03-12
dc.date.issued2015-03-12
dc.identifier.citationYamaguchi, H. [et al.]. A Chandrasekhar mass progenitor for the type Ia supernova remnant 3C 397 from the enhanced abundances of nickel and manganese. "Astrophysical journal", 12 Març 2015, vol. 801, núm. 2, p. L31-L35.
dc.identifier.issn0004-637X
dc.identifier.urihttp://hdl.handle.net/2117/28214
dc.description.abstractDespite decades of intense efforts, many fundamental aspects of Type Ia supernovae (SNe Ia) remain elusive. One of the major open questions is whether the mass of an exploding white dwarf (WD) is close to the Chandrasekhar limit. Here, we report the detection of strong K-shell emission from stable Fe-peak elements in the Suzaku X-ray spectrum of the Type Ia supernova remnant (SNR) 3C 397. The high Ni/Fe and Mn/Fe mass ratios (0.11–0.24 and 0.018–0.033, respectively) in the hot plasma component that dominates the K-shell emission lines indicate a degree of neutronization in the supernova ejecta that can only be achieved by electron capture in the dense cores of exploding WDs with a near-Chandrasekhar mass. This suggests a single-degenerate origin for 3C 397, since Chandrasekhar mass progenitors are expected naturally if the WD accretes mass slowly from a companion. Together with other results supporting the double-degenerate scenario, our work adds to the mounting evidence that both progenitor channels make a significant contribution to the SN Ia rate in star-forming galaxies.
dc.language.isoeng
dc.subjectÀrees temàtiques de la UPC::Física::Astronomia i astrofísica
dc.subject.lcshSupernovae
dc.subject.otheratomic data—infrared: ISM—ISM: individual objects (3C397
dc.subject.otherG41.1–0.3)— ISM: supernova remnants — nuclear reactions
dc.subject.othernucleosynthesis
dc.subject.otherabundances — X-rays: ISM
dc.titleA Chandrasekhar mass progenitor for the type Ia supernova remnant 3C 397 from the enhanced abundances of nickel and manganese
dc.typeArticle
dc.subject.lemacSupernoves
dc.contributor.groupUniversitat Politècnica de Catalunya. GRPFM - Grup de Recerca en Propietats Físiques dels Materials
dc.identifier.doi10.1088/2041-8205/801/2/L31
dc.description.peerreviewedPeer Reviewed
dc.relation.publisherversionarxiv.org/pdf/1502.04255
dc.rights.accessRestricted access - publisher's policy
drac.iddocument15539818
dc.description.versionPostprint (author’s final draft)
dc.date.lift10000-01-01
upcommons.citation.authorYamaguchi, H.; Badenes, C.; Foster, A.; Bravo, E.; Williams, B.; Maeda, K.; Nobukawa, M.; Eriksen, K.; Brickhouse, N.; Petre, R.; Koyama, K.
upcommons.citation.publishedtrue
upcommons.citation.publicationNameAstrophysical journal
upcommons.citation.volume801
upcommons.citation.number2
upcommons.citation.startingPageL31
upcommons.citation.endingPageL35


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