Investigating the properties of stripped-envelope supernovae, what are the implications for their progenitors?
S. J. Prentice,S. J. Prentice,Chris Ashall,Chris Ashall,Phil A. James,L. Short,Paolo A. Mazzali,Paolo A. Mazzali,D. Bersier,Paul A. Crowther,Cristina Barbarino,Ting-Wan Chen,Chris M. Copperwheat,M. J. Darnley,L. Denneau,Nancy Elias-Rosa,Morgan Fraser,Lluís Galbany,Avishay Gal-Yam,Jussi Harmanen,D. A. Howell,D. A. Howell,Griffin Hosseinzadeh,Griffin Hosseinzadeh,Griffin Hosseinzadeh,Cosimo Inserra,Erkki Kankare,Emir Karamehmetoglu,Gavin P. Lamb,Gavin P. Lamb,Marco Limongi,Kate Maguire,Curtis McCully,Curtis McCully,A. S. Piascik,Giuliano Pignata,Giuliano Pignata,Daniel E. Reichart,Armin Rest,Armin Rest,T. M. Reynolds,Ósmar Rodríguez,Ósmar Rodríguez,J. Saario,Steve Schulze,Stephen J. Smartt,K. W. Smith,Jesper Sollerman,B. Stalder,Mark Sullivan,Francesco Taddia,Stefano Valenti,S. D. Vergani,Steven Williams,D. R. Young +54 more
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In this article, the peak luminosity and characteristic time-scales of the bolometric light curves are calculated, and the light curves modelled to derive 56Ni and ejecta masses (MNi and Mej).Abstract:
We present observations and analysis of 18 stripped-envelope supernovae observed during 2013–2018. This sample consists of five H/He-rich SNe, six H-poor/He-rich SNe, three narrow lined SNe Ic, and four broad lined SNe Ic. The peak luminosity and characteristic time-scales of the bolometric light curves are calculated, and the light curves modelled to derive 56Ni and ejecta masses (MNi and Mej). Additionally, the temperature evolution and spectral line velocity curves of each SN are examined. Analysis of the [O I] line in the nebular phase of eight SNe suggests their progenitors had initial masses = 2.8 ± 1.5 M⊙ which further strengthens the evidence that SE–SNe arise from low-mass progenitors which are typically and lack of clear bimodality in the distribution implies <30 M⊙ progenitors and that envelope stripping via binary interaction is the dominant evolutionary pathway of these SNe.read more
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Journal ArticleDOI
The Explosion of Helium Stars Evolved with Mass Loss
Journal ArticleDOI
Models for the Type Ic Hypernova SN 2003lw associated with GRB 031203
Paolo A. Mazzali,Jinsong Deng,Elena Pian,D. Malesani,Nozomu Tominaga,Keiichi Maeda,Ken'ichi Nomoto,Guido Chincarini,Stefano Covino,Massimo Della Valle,Dino Fugazza,Gianpiero Tagliaferri,Avishay Gal-Yam +12 more
TL;DR: The Gamma-Ray Burst 20031203 at a redshift z = 0.1055 revealed a highly reddened Type Ic Supernova, SN 2003lw, in its afterglow light as discussed by the authors.
Journal ArticleDOI
The Explosion of Helium Stars Evolved With Mass Loss
TL;DR: In this paper, light curves, explosion energies, and remnant masses for a grid of supernovae resulting from massive helium stars that have been evolved including mass loss are calculated for a set of stars in interacting systems.
Journal ArticleDOI
A meta-analysis of core-collapse supernova 56 Ni masses
TL;DR: In this paper, a meta-analysis of all published 56 Ni masses for core-collapse supernovae (CC SNe) is provided, and a median 56 Ni mass of 0.032 M ⊙ for SNe II (N ǫ= 115), 0.102 M ⌉ for SNE IIb (Nǫ = 27, 0.163 M ⎉ for SE-SNeIb, SNEI Ib (N ë = ‚=‚33), and 0.155 M
Journal ArticleDOI
Why binary interaction does not necessarily dominate the formation of Wolf-Rayet stars at low metallicity
TL;DR: In this paper, the importance of the binary channel in the formation of Wolf-Rayet stars was investigated in the Magellanic Clouds and the Galaxy, and it was shown that the contribution of binary interactions is a non-trivial and model-dependent function of Z that cannot be conclusively claimed to be monotonically increasing with decreasing Z.
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