The Type IIb Supernova 2011dh from a Supergiant Progenitor

Melina C. Bersten, Omar G. Benvenuto, Ken'ichi Nomoto, Mattias Ergon, Gastón Folatelli, Jesper Sollerman, Stefano Benetti, Maria Teresa Botticella, Morgan Fraser, Rubina Kotak, Keiichi Maeda, Paolo Ochner, Lina Tomasella

Research output: Contribution to journalArticlepeer-review

143 Citations (Scopus)


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 Rsun---, 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 Msun, the explosion energy to be E= 6-10 x 10^50 erg, and the 56Ni mass to be approximately 0.06 Msun. The progenitor star was composed of a helium core of 3 to 4 Msun and a thin hydrogen-rich envelope of ~0.1 M_sun with a main sequence mass estimated to be in the range of 12--15 Msun. Our models rule out progenitors with helium-core masses larger than 8 Msun, which correspond to M_ZAMS > 25 Msun. This suggests that a single star evolutionary scenario for SN 2011dh is unlikely.
Original languageUndefined/Unknown
Article number31
JournalAstrophysical Journal
Issue number31
Publication statusPublished - 25 Jul 2012

Bibliographical note

20 pages with 12 figures. Submitted to The Astrophysical Journal on 24 May 2012 and accepted on 17 July 2012


  • astro-ph.HE
  • astro-ph.SR

ASJC Scopus subject areas

  • Space and Planetary Science
  • Astronomy and Astrophysics

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