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A comparative study of Type II-P and II-L supernova rise times as exemplified by the case of LSQ13cuw
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Number of Authors: 20
2015 (English)In: Astronomy and Astrophysics, ISSN 0004-6361, E-ISSN 1432-0746, Vol. 582, A3Article in journal (Refereed) Published
Abstract [en]

We report on our findings based on the analysis of observations of the Type II-L supernova LSQ13cuw within the framework of currently accepted physical predictions of core-collapse supernova explosions. LSQ13cuw was discovered within a day of explosion, hitherto unprecedented for Type II-L supernovae. This motivated a comparative study of Type II-P and II-L supernovae with relatively well-constrained explosion epochs and rise times to maximum (optical) light. From our sample of twenty such events, we find evidence of a positive correlation between the duration of the rise and the peak brightness. On average, SNe II-L tend to have brighter peak magnitudes and longer rise times than SNe II-P. However, this difference is clearest only at the extreme ends of the rise time versus peak brightness relation. Using two different analytical models, we performed a parameter study to investigate the physical parameters that control the rise time behaviour. In general, the models qualitatively reproduce aspects of the observed trends. We find that the brightness of the optical peak increases for larger progenitor radii and explosion energies, and decreases for larger masses. The dependence of the rise time on mass and explosion energy is smaller than the dependence on the progenitor radius. We find no evidence that the progenitors of SNe II-L have significantly smaller radii than those of SNe II-P.

Place, publisher, year, edition, pages
2015. Vol. 582, A3
Keyword [en]
supernovae: general, supernovae: individual: LSQ13cuw, methods: analytical
National Category
Physical Sciences
URN: urn:nbn:se:su:diva-123801DOI: 10.1051/0004-6361/201525868ISI: 000363538500003OAI: diva2:881935
Available from: 2015-12-11 Created: 2015-12-07 Last updated: 2015-12-11Bibliographically approved

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Sollerman, Jesper
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Department of AstronomyThe Oskar Klein Centre for Cosmo Particle Physics (OKC)
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