Registro completo de metadatos
| Campo DC | Valor | Lengua/Idioma |
|---|---|---|
| dc.provenance | Comisión de Investigaciones Científicas | - |
| dc.contributor | Bersten, Melina | - |
| dc.contributor | Benvenuto, Omar Gustavo | - |
| dc.contributor | Nomoto, Ken'ichi | - |
| dc.contributor | Ergon, Mattias | - |
| dc.contributor | Folatelli, Gastón | - |
| dc.contributor | Sollerman, Jesper | - |
| dc.contributor | Benetti, Stefano | - |
| dc.contributor | Botticella, María Teresa | - |
| dc.contributor | Fraser, Morgan | - |
| dc.contributor | Kotak, Rubina | - |
| dc.creator | Bersten, Melina | - |
| dc.creator | Benvenuto, Omar Gustavo | - |
| dc.creator | Nomoto, Ken'ichi | - |
| dc.creator | Ergon, Mattias | - |
| dc.creator | Folatelli, Gastón | - |
| dc.creator | Sollerman, Jesper | - |
| dc.creator | Benetti, Stefano | - |
| dc.creator | Botticella, María Teresa | - |
| dc.creator | Fraser, Morgan | - |
| dc.creator | Kotak, Rubina | - |
| dc.date | 2012 | - |
| dc.date.accessioned | 2019-04-29T16:05:21Z | - |
| dc.date.available | 2019-04-29T16:05:21Z | - |
| dc.date.issued | 2012 | - |
| dc.identifier | http://digital.cic.gba.gob.ar/handle/11746/4220 | - |
| dc.identifier | Documento completo | - |
| dc.identifier.uri | http://rodna.bn.gov.ar:8080/jspui/handle/bnmm/308895 | - |
| dc.description | 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. | - |
| dc.format | application/pdf | - |
| dc.format | 20 p. | - |
| dc.language | eng | - |
| dc.publisher | IOPscience | - |
| dc.rights | info:eu-repo/semantics/openAccess | - |
| dc.rights | Attribution 4.0 International (BY 4.0) | - |
| dc.source | reponame:CIC Digital (CICBA) | - |
| dc.source | instname:Comisión de Investigaciones Científicas de la Provincia de Buenos Aires | - |
| dc.source | instacron:CICBA | - |
| dc.source.uri | http://digital.cic.gba.gob.ar/handle/11746/4220 | - |
| dc.source.uri | Documento completo | - |
| dc.subject | Astronomía | - |
| dc.title | The type IIB supernova 2011DH from a supergiant progenitor | - |
| dc.type | info:eu-repo/semantics/article | - |
| dc.type | info:eu-repo/semantics/submittedVersion | - |
| dc.type | info:ar-repo/semantics/articulo | - |
| Aparece en las colecciones: | Comisión de Investigaciones Científicas de la Prov. de Buenos Aires | |
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