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dc.title The type IIB supernova 2011DH from a supergiant progenitor en
dc.type Artículo es
dcterms.abstract A set of hydrodynamical models based on stellar evolutionary progenitors is used to study the nature of SN 2011dh. Our modeling suggests that a large progenitor star —with R 200 R⊙—, is needed to reproduce the early light curve of SN 2011dh. This is consistent with the suggestion that the yellow super-giant star detected at the location of the SN in deep pre-explosion images is the progenitor star. From the main peak of the bolometric light curve and expansion velocities we constrain the mass of the ejecta to be 2 M⊙, the explosion energy to be E = 6 − 10 × 1050 erg, and the 56Ni mass to be approximately 0.06 M⊙. The progenitor star was composed of a helium core of 3 to 4 M⊙ and a thin hydrogen-rich envelope of 0.1 M⊙ with a main sequence mass estimated to be in the range of 12–15 M⊙. Our models rule out progenitors with helium-core masses larger than 8 M⊙, which correspond to MZAMS & 25 M⊙. This suggests that a single star evolutionary scenario for SN 2011dh is unlikely. en
dcterms.extent 20 p. es
dcterms.issued 2012
dcterms.language Inglés es
dcterms.license Attribution 4.0 International (BY 4.0) es
dcterms.publisher IOPscience es
dcterms.subject hydrodynamics en
dcterms.subject SN 2011dh en
dcterms.subject supernova es
cic.version info:eu-repo/semantics/submittedVersion es Bersten, Melina es Benvenuto, Omar Gustavo es Nomoto, Ken'ichi es Ergon, Mattias es Folatelli, Gastón es Sollerman, Jesper es Benetti, Stefano es Botticella, María Teresa es Fraser, Morgan es Kotak, Rubina es
cic.lugarDesarrollo Universidad Nacional de La Plata es
dcterms.subject.materia Astronomía es
dcterms.identifier.url Documento completo es
dcterms.identifier.other DOI:10.1088/0004-637X/757/1/31 es
dcterms.isPartOf.issue vol. 757, nº 1 es
dcterms.isPartOf.series Astrophysical Journal es
cic.isPeerReviewed true es
cic.isFulltext true es


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