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THE TYPE IIb SUPERNOVA 2011dh FROM A SUPERGIANT PROGENITOR
Stockholm University, Faculty of Science, Department of Astronomy. Stockholm University, Faculty of Science, The Oskar Klein Centre for Cosmo Particle Physics (OKC).
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2012 (English)In: Astrophysical Journal, ISSN 0004-637X, E-ISSN 1538-4357, Vol. 757, no 1, 31Article in journal (Refereed) Published
Abstract [en]

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 similar to 200 R-circle dot-is needed to reproduce the early light curve (LC) of SN 2011dh. This is consistent with the suggestion that the yellow super-giant star detected at the location of the supernova (SN) in deep pre-explosion images is the progenitor star. From the main peak of the bolometric LC and expansion velocities, we constrain the mass of the ejecta to be approximate to 2 M-circle dot, the explosion energy to be E = (6-10) x 10(50) erg, and the Ni-56 mass to be approximately 0.06 M-circle dot. The progenitor star was composed of a helium core of 3-4 M-circle dot and a thin hydrogen-rich envelope of approximate to 0.1M(circle dot) with a main-sequence mass estimated to be in the range of 12-15 M-circle dot. Our models rule out progenitors with helium-core masses larger than 8 M-circle dot, which correspond to M-ZAMS greater than or similar to 25M(circle dot). This suggests that a single star evolutionary scenario for SN 2011dh is unlikely.

Place, publisher, year, edition, pages
2012. Vol. 757, no 1, 31
Keyword [en]
hydrodynamics, supernovae: general, supernovae: individual (SN 2011dh)
National Category
Astronomy, Astrophysics and Cosmology
Research subject
Astronomy
Identifiers
URN: urn:nbn:se:su:diva-81845DOI: 10.1088/0004-637X/757/1/31ISI: 000309052800031OAI: oai:DiVA.org:su-81845DiVA: diva2:564077
Note

AuthorCount:13;

Available from: 2012-11-01 Created: 2012-11-01 Last updated: 2017-12-07Bibliographically approved

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Ergon, MattiasSollerman, Jesper
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