SIMBAD references

2014MNRAS.438..318K - Mon. Not. R. Astron. Soc., 438, 318-328 (2014/February-2)

Rapidly fading supernovae from massive star explosions.


Abstract (from CDS):

Transient surveys have recently discovered a class of supernovae (SNe) with extremely rapidly declining light curves. These events are also often relatively faint, especially compared to Type Ia SNe. The common explanation for these events involves a weak explosion, producing a radioactive outflow with small ejected mass and kinetic energy (M ∼ 0.1M and E ∼ 0.1 B, respectively), perhaps from the detonation of a helium shell on a white dwarf. We argue, in contrast, that these events may be Type Ib/c SNe with typical masses and energies (M ∼ 3M, E ∼ 1 B), but which ejected very little radioactive material. In our picture, the light curve is powered by the diffusion of thermal energy deposited by the explosion shock wave, and the rapid evolution is due to recombination, which reduces the opacity and results in an `oxygen-plateau' light curve. Using a radiative transfer code and simple 1D ejecta profiles, we generate synthetic spectra and light curves and demonstrate that this model can reasonably fit the observations of one event, SN 2010X. Similar models may explain the features of other rapidly evolving SNe such as SN 2002bj and SN 2005ek. SNe such as these may require stripped-envelope progenitors with rather large radii (R ∼ 20R), which may originate from a mass-loss episode occurring just prior to explosion.

Abstract Copyright: © 2013 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society (2013)

Journal keyword(s): radiative transfer - supernovae: general - supernovae: individual: SN 2010X - supernovae: individual: SN 2002bj - supernovae: individual: SN 2005ek - supernovae: individual: SN 1994I

Simbad objects: 8

goto Full paper

goto View the references in ADS

To bookmark this query, right click on this link: simbad:2014MNRAS.438..318K and select 'bookmark this link' or equivalent in the popup menu


© Université de Strasbourg/CNRS

    • Contact