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A supergiant progenitor for SN 2011dh

Published online by Cambridge University Press:  05 September 2012

Melina C. Bersten ,
Omar Benvenuto  and
Ken Nomoto
Melina C. Bersten
Affiliation:
Kavli Institute for the Physics and Mathematics of the Universe, Todai Institutes for Advanced Study, the University of Tokyo, Kashiwa, Japan 277-8583 (Kavli IPMU, WPI) email: melina.bersten@ipmu.jp
Omar Benvenuto
Affiliation:
Facultad de Ciencias Astronómicas y Geofísicas, Universidad Nacional de La Plata, Paseo del Bosque S/N, B1900FWA La Plata, Argentina email: obenvenu@fcaglp.unlp.edu.ar
Ken Nomoto
Affiliation:
Kavli Institute for the Physics and Mathematics of the Universe, Todai Institutes for Advanced Study, the University of Tokyo, Kashiwa, Japan 277-8583 (Kavli IPMU, WPI) email: melina.bersten@ipmu.jp
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Abstract

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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.

Keywords

hydrodynamicsstellar evolutionsupernovaeSN 2011dh
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 7 , Symposium S279: Death of Massive Stars: Supernovae and Gamma-Ray Bursts , April 2011 , pp. 18 - 21
Copyright
Copyright © International Astronomical Union 2012

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