TY - JOUR

T1 - Pulsational Pair-instability Model for Superluminous Supernova PTF12dam

T2 - Interaction and Radioactive Decay

AU - Tolstov, Alexey

AU - Nomoto, Ken'Ichi

AU - Blinnikov, Sergei

AU - Sorokina, Elena

AU - Quimby, Robert

AU - Baklanov, Petr

PY - 2017/2/1

Y1 - 2017/2/1

N2 - Being a superluminous supernova, PTF12dam can be explained by a 56Ni-powered model, a magnetar-powered model, or an interaction model. We propose that PTF12dam is a pulsational pair-instability supernova, where the outer envelope of a progenitor is ejected during the pulsations. Thus, it is powered by a double energy source: radioactive decay of 56Ni and a radiative shock in a dense circumstellar medium. To describe multicolor light curves and spectra, we use radiation-hydrodynamics calculations of the STELLA code. We found that light curves are well described in the model with 40 Mo ejecta and 20-40 Mo circumstellar medium. The ejected 56Ni mass is about 6 Mo, which results from explosive nucleosynthesis with large explosion energy (2-3) × 1052 erg. In comparison with alternative scenarios of pair-instability supernova and magnetar-powered supernova, in the interaction model, all the observed main photometric characteristics are well reproduced: multicolor light curves, color temperatures, and photospheric velocities.

AB - Being a superluminous supernova, PTF12dam can be explained by a 56Ni-powered model, a magnetar-powered model, or an interaction model. We propose that PTF12dam is a pulsational pair-instability supernova, where the outer envelope of a progenitor is ejected during the pulsations. Thus, it is powered by a double energy source: radioactive decay of 56Ni and a radiative shock in a dense circumstellar medium. To describe multicolor light curves and spectra, we use radiation-hydrodynamics calculations of the STELLA code. We found that light curves are well described in the model with 40 Mo ejecta and 20-40 Mo circumstellar medium. The ejected 56Ni mass is about 6 Mo, which results from explosive nucleosynthesis with large explosion energy (2-3) × 1052 erg. In comparison with alternative scenarios of pair-instability supernova and magnetar-powered supernova, in the interaction model, all the observed main photometric characteristics are well reproduced: multicolor light curves, color temperatures, and photospheric velocities.

KW - circumstellar matter

KW - supernovae: general

KW - supernovae: individual (PTF12dam)

KW - 2007BI

KW - ANALYTIC FITS

KW - LIGHT CURVES

KW - RADIATION

KW - PHOTOIONIZATION CROSS-SECTIONS

KW - HYDROGEN

KW - EXPLOSIONS

KW - EVOLUTION

KW - LUMINOUS SUPERNOVAE

KW - STARS

UR - http://www.scopus.com/inward/record.url?scp=85012004965&partnerID=8YFLogxK

U2 - 10.3847/1538-4357/835/2/266

DO - 10.3847/1538-4357/835/2/266

M3 - Article

AN - SCOPUS:85012004965

VL - 835

JO - Astrophysical Journal

JF - Astrophysical Journal

SN - 0004-637X

IS - 2

M1 - 266

ER -