The type IIB supernova 2011DH from a supergiant progenitor
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 sup...
| Autores: | , , , , , , , , , |
|---|---|
| Tipo de recurso: | artículo |
| Estado: | Versión enviada para evaluación y publicación |
| Fecha de publicación: | 2012 |
| País: | Argentina |
| Institución: | Comisión de Investigaciones Científicas de la Provincia de Buenos Aires |
| Repositorio: | CIC Digital (CICBA) |
| Idioma: | inglés |
| OAI Identifier: | oai:digital.cic.gba.gob.ar:11746/4220 |
| Acceso en línea: | https://digital.cic.gba.gob.ar/handle/11746/4220 |
| Access Level: | acceso abierto |
| Palabra clave: | Astronomía hydrodynamics SN 2011dh supernova |
| Sumario: | 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. |
|---|