A supergiant progenitor for SN 2011dh

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 pro...

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Detalles Bibliográficos
Autores principales: Bersten, Melina Cecilia, Benvenuto, Omar Gustavo, Nomoto, Ken
Formato: Articulo Comunicacion
Lenguaje:Inglés
Publicado: 2011
Materias:
Ciencias Astronómicas
hydrodynamics
SN 2011dh
stellar evolution
supernovae
Hidrodinámica
Acceso en línea:http://sedici.unlp.edu.ar/handle/10915/84223
Aporte de:
SEDICI (UNLP) de Universidad Nacional de La Plata
id I19-R120-10915-84223
record_format dspace
institution Universidad Nacional de La Plata
institution_str I-19
repository_str R-120
collection SEDICI (UNLP)
language Inglés
topic Ciencias Astronómicas
hydrodynamics
SN 2011dh
stellar evolution
supernovae
Hidrodinámica
spellingShingle Ciencias Astronómicas
hydrodynamics
SN 2011dh
stellar evolution
supernovae
Hidrodinámica
Bersten, Melina Cecilia
Benvenuto, Omar Gustavo
Nomoto, Ken
A supergiant progenitor for SN 2011dh
topic_facet Ciencias Astronómicas
hydrodynamics
SN 2011dh
stellar evolution
supernovae
Hidrodinámica
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.
format Articulo
Comunicacion
author Bersten, Melina Cecilia
Benvenuto, Omar Gustavo
Nomoto, Ken
author_facet Bersten, Melina Cecilia
Benvenuto, Omar Gustavo
Nomoto, Ken
author_sort Bersten, Melina Cecilia
title A supergiant progenitor for SN 2011dh
title_short A supergiant progenitor for SN 2011dh
title_full A supergiant progenitor for SN 2011dh
title_fullStr A supergiant progenitor for SN 2011dh
title_full_unstemmed A supergiant progenitor for SN 2011dh
title_sort supergiant progenitor for sn 2011dh
publishDate 2011
url http://sedici.unlp.edu.ar/handle/10915/84223
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