The pre-SN activity as a possible explanation of the peculiar properties of Type IIP Supernova 2009kf

Abstract

SN 2009kf is an exceptionally bright Type IIP Supernova (SN IIP) discovered by the Pan-STARRS 1 survey. The $V$-band magnitude at the plateau phase is $M_V=-18.4$ mag, which is much brighter than typical SNe IIP. We propose that its unusual properties can be naturally explained, if we assume that there was an super-Eddington energy injection into the envelope in the last few years of the evolution before the SN explosion. Using a progenitor model with such an pre-SN energy injection, we can fit the observational data of SN 2009kf with the reasonable explosion energy of $E_{\exp }=2.8\times 10^{51}$ erg and the ${}^{56}$Ni mass of $0.25M_{\odot }$. Specifically, we injected the energy into the envelope at a constant rate of $3.0\times 10^{39}$ erg s${}^{-1}$ in the last 3.0 years of evolution before the core collapse. We propose that some of the unusually bright SNe IIP might result from the pre-SN energy injection to the envelope.

arXiv commentComments: 6 pages, 5 figures, accepted for publication in MNRAS

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