| dc.creator | Bersten, Melina Cecilia | |
| dc.creator | Benvenuto, Omar Gustavo | |
| dc.creator | Nomoto, Ken | |
| dc.date | 2011-04 | |
| dc.date | 2019-10-28T15:52:00Z | |
| dc.identifier | http://sedici.unlp.edu.ar/handle/10915/84223 | |
| dc.identifier | issn:1743-9213 | |
| 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 (LC) of SN 2011dh. This is consistent with the suggestion that the progenitor is a yellow super-giant star detected at the location of the SN in deep pre-explosion images. From the main peak of the bolometric light curve (LC) and expansion velocities we constrain the mass of the ejecta to be ≈2 M⊙, the explosion energy to be E = 8 × 1050 erg, and the 56Ni mass to be 0.063 M⊙. The progenitor star is composed of a helium core of ≈4 M⊙ and a thin hydrogen envelope, and it had a main-sequence mass of ≈13 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 evolutionary scenario for SN 2011dh is highly unlikely. | |
| dc.description | Facultad de Ciencias Astronómicas y Geofísicas | |
| dc.format | application/pdf | |
| dc.format | 18-21 | |
| dc.language | en | |
| dc.rights | http://creativecommons.org/licenses/by-nc-sa/4.0/ | |
| dc.rights | Creative Commons Attribution-NonCommercial-ShareAlike 4.0 International (CC BY-NC-SA 4.0) | |
| dc.subject | Ciencias Astronómicas | |
| dc.subject | hydrodynamics | |
| dc.subject | SN 2011dh | |
| dc.subject | stellar evolution | |
| dc.subject | supernovae | |
| dc.subject | Hidrodinámica | |
| dc.title | A supergiant progenitor for SN 2011dh | |
| dc.type | Articulo | |
| dc.type | Comunicacion | |
