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PROGENITORS OF TYPE IIb SUPERNOVAE IN THE LIGHT OF RADIO AND X-RAYS FROM SN 2013df
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Number of Authors: 10
2016 (English)In: Astrophysical Journal, ISSN 0004-637X, E-ISSN 1538-4357, Vol. 818, no 2, 111Article in journal (Refereed) Published
Abstract [en]

We present radio and X-ray observations of the nearby SN IIb 2013df in NGC 4414 from 10 to 250 days after the explosion. The radio emission showed a peculiar steep-to-shallow spectral evolution. We present a model in which inverse Compton cooling of synchrotron emitting electrons can account for the observed spectral and light curve evolution. A significant mass-loss rate, (M) over dot approximate to 8 x 10(-5) M-circle dot yr(-1) for a wind velocity of 10 km s(-1), is estimated from the detailed modeling of radio and X-ray emission, which are primarily due to synchrotron and bremsstrahlung, respectively. We show that SN 2013df is similar to SN 1993J in various ways. The shock wave speed of SN 2013df was found to be average among the radio supernovae; v(sh)/c similar to 0.07. We did not find any significant deviation from smooth decline in the light curve of SN 2013df. One of the main results of our self-consistent multiband modeling is the significant deviation from energy equipartition between magnetic fields and relativistic electrons behind the shock. We estimate epsilon(e) = 200 epsilon(B). In general for SNe IIb, we find that the presence of bright optical cooling envelope emission is linked with free-free radio absorption and bright thermal X-ray emission. This finding suggests that more extended progenitors, similar to that of SN 2013df, suffer from substantial mass loss in the years before the supernova.

Place, publisher, year, edition, pages
2016. Vol. 818, no 2, 111
Keyword [en]
radiation mechanisms: non-thermal, radio continuum: general, supernovae: general, supernovae: individual (SN 2013df, SN 1993J)
National Category
Astronomy, Astrophysics and Cosmology
Identifiers
URN: urn:nbn:se:su:diva-129643DOI: 10.3847/0004-637X/818/2/111ISI: 000372302800010OAI: oai:DiVA.org:su-129643DiVA: diva2:924581
Available from: 2016-04-28 Created: 2016-04-26 Last updated: 2016-04-28Bibliographically approved

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Fransson, Claes
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Department of AstronomyThe Oskar Klein Centre for Cosmo Particle Physics (OKC)
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