THE TYPE IIb SUPERNOVA 2011dh FROM A SUPERGIANT PROGENITOR

By M. Bersten, O. Benvenuto, Ken'ichi Nomoto, M. Ergon, G. Folatelli, J. Sollerman, S. Benetti, M. Botticella, Morgan Fraser, R. Kotak and 3 more. 2012

166 citations recorded by the source corpus.

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 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 ≈2 M☉, the explosion energy to be E = (6–10) × 1050 erg, and the 56Ni mass to be approximately 0.06 M☉. The progenitor star was composed of a helium core of 3–4 M☉ and a thin hydrogen-rich envelope of ≈0.1M☉ with a main-sequence mass estimated to be in the range of 12–15 M☉. Our models rule out progenitors with helium-core masses larger than 8 M☉, which correspond to MZAMS ≳ 25M☉. This suggests that a single star evolutionary scenario for SN 2011dh is unlikely.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/fc8ef93eab2b1d9fa6e366a1503a8cce5ada521e

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In Astronomy and Astrophysics

1. S. Smartt
2. E. Berger
3. A. Filippenko
4. A. Riess
5. N. Smith
6. Ryan Chornock
7. A. Gal-yam
8. R. Kirshner

In Nuclear and High Energy Physics

1. S. Smartt
2. A. Filippenko
3. A. Gal-yam
4. Ryan Chornock
5. E. Berger
6. R. Kirshner
7. J. C. Wheeler
8. A. Riess

Citations in the corpus

• The Carnegie Supernova Project I: analysis of stripped-envelope supernova light curves (2017, methodology): “…et al. 1993, 1994), SN 2008ax (Pastorello et al. 2008; Chornock et al. 2011; Taubenberger et al. 2011; Folatelli et al. 2015), SN 2011dh (Bersten et al. 2012; Ergon et al. 2014, 2015), SN 2011hs (Bufano et al. 2014), SN 2010as (Folatelli et al. 2014b), and PTF12os (Fremling et al. 2016).”
• DISCOVERY, PROGENITOR AND EARLY EVOLUTION OF A STRIPPED ENVELOPE SUPERNOVA iPTF13bvn (2013, background): “…a supernova, which is sensitive to the progenitor size, explosion energy and the composition of the outer layers (e.g., Nakar & Sari 2010; Rabinak & Waxman 2011; Bersten et al. 2012; Piro & Nakar 2013), and in some propitious cases can even diagnose the presence of a binary companion (Kasen 2010).”
• RAPIDLY EVOLVING AND LUMINOUS TRANSIENTS FROM PAN-STARRS1 (2014, background): “…2013; Kasliwal et al. 2012; Perets et al. 2010), type Ib/Ic (Drout et al. 2011; Valenti et al. 2008; Campana et al. 2006; Taubenberger et al. 2006; Bersten et al. 2012; Olivares et al. 2012; Cobb et al. 2010; Valenti et al. 2012), type IIP/IIL (Arcavi et al. 2012; Hamuy 2003; Andrews et al.…”
• Bolometric light curves and explosion parameters of 38 stripped-envelope core-collapse supernovae (2014, methodology): “For comparison, we use the parameters of Ergon et al. (2014), which revise those used in Bersten et al. (2012) where initial modelling of SN 2011dh was performed, in order to compare to their hydrodynamical modelling results.”
• CHARACTERIZING THE V-BAND LIGHT-CURVES OF HYDROGEN-RICH TYPE II SUPERNOVAE (2014, background): “The extent in time, post explosion of this cooling is predicted to be directly related to the radius of the pre-SN progenitor star (see Bersten et al. 2012, for recent application of this hypothesis to a SN IIb).”
• SUPER-LUMINOUS TYPE Ic SUPERNOVAE: CATCHING A MAGNETAR BY THE TAIL (2013, methodology): “In previous works, values ranging between 0.01 and 0.24 cm2 g−1 have been used (e.g., Herzig et al. 1990; Swartz et al. 1991; Young 2004; Bersten et al. 2011, 2012).”
• PTF12os and iPTF13bvn. Two stripped-envelope supernovae from low-mass progenitors in NGC 5806 (2016, background): “However, there is evidence that analytical shock-cooling models tend to predict unrealistically high temperatures when the radius becomes large (e.g., Bersten et al. 2012).”
• Early-time light curves of Type Ib/c supernovae from the SDSS-II Supernova Survey (2014, methodology): “(∼ 200 R ) yellow supergiant progenitors (Maund et al. 2011; Bersten et al. 2012; Ergon et al. 2014a,b).”