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Bufano, F.; Pignata, G.; Bersten, M.; Mazzali, P. A.; Ryder, S. D.; Margutti, R.; Milisavljevic, D.; Morelli, L.; Benetti, S.; Cappellaro, E.; Gonzalez-Gaitan, S.; Romero-Cañizales, C.; Stritzinger, M.; Walker, E. S.; Anderson, J. P.; Contreras, C.; de Jaeger, T.; Förster, F.; Gutierrez, C.; Hamuy, M.; Hsiao, E.; Morrell, N.; Olivares E., F.; Paillas, E.; Parker, S.; Pian, E.; Pickering, T. E.; Sanders, N.; Stockdale, C.; Turatto, M.; Valenti, S.; Fesen, R. A.; Maza, J.; Nomoto, K.; Phillips, M. M.; Soderberg, A.
Monthly Notices of the Royal Astronomical Society, 04/2014, Letnik: 439, Številka: 2Journal Article
Observations spanning a large wavelength range, from X-ray to radio, of the Type IIb supernova (SN) 2011hs are presented, covering its evolution during the first year after explosion. The optical light curve presents a narrower shape and a fainter luminosity at peak than previously observed for Type IIb SNe. High expansion velocities are measured from the broad absorption H i and He i lines. From the comparison of the bolometric light curve and the time evolution of the photospheric velocities with hydrodynamical models, we found that SN 2011hs is consistent with the explosion of a 3-4 M He-core progenitor star, corresponding to a main-sequence mass of 12-15 M, that ejected a mass of 56Ni of about 0.04 M, with an energy of E = 8.5 × 1050 ERG. Such a low-mass progenitor scenario is in full agreement with the modelling of the nebular spectrum taken at ∼215 d from maximum. From the modelling of the adiabatic cooling phase, we infer a progenitor radius of 500-600 R, clearly pointing to an extended progenitor star. The radio light curve of SN 2011hs yields a peak luminosity similar to that of SN 1993J, but with a higher mass-loss rate and a wind density possibly more similar to that of SN 2001ig. Although no significant deviations from a smooth decline have been found in the radio light curves, we cannot rule out the presence of a binary companion star.
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Leto | Faktor vpliva | Izdaja | Kategorija | Razvrstitev | ||||
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JCR | SNIP | JCR | SNIP | JCR | SNIP | JCR | SNIP |
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in: SICRIS
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