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Pulsational Pair-instability Model for Superluminous Supernova PTF12dam : Interaction and Radioactive Decay. / Tolstov, Alexey; Nomoto, Ken'Ichi; Blinnikov, Sergei et al.

In: Astrophysical Journal, Vol. 835, No. 2, 266, 01.02.2017.

Research output: Contribution to journal › Article › peer-review

Harvard

Tolstov, A, Nomoto, KI, Blinnikov, S, Sorokina, E, Quimby, R & Baklanov, P 2017, 'Pulsational Pair-instability Model for Superluminous Supernova PTF12dam: Interaction and Radioactive Decay', Astrophysical Journal, vol. 835, no. 2, 266. https://doi.org/10.3847/1538-4357/835/2/266

APA

Tolstov, A., Nomoto, KI., Blinnikov, S., Sorokina, E., Quimby, R., & Baklanov, P. (2017). Pulsational Pair-instability Model for Superluminous Supernova PTF12dam: Interaction and Radioactive Decay. Astrophysical Journal, 835(2), [266]. https://doi.org/10.3847/1538-4357/835/2/266

Vancouver

Tolstov A, Nomoto KI, Blinnikov S, Sorokina E, Quimby R, Baklanov P. Pulsational Pair-instability Model for Superluminous Supernova PTF12dam: Interaction and Radioactive Decay. Astrophysical Journal. 2017 Feb 1;835(2):266. doi: 10.3847/1538-4357/835/2/266

Author

Tolstov, Alexey ; Nomoto, Ken'Ichi ; Blinnikov, Sergei et al. / Pulsational Pair-instability Model for Superluminous Supernova PTF12dam : Interaction and Radioactive Decay. In: Astrophysical Journal. 2017 ; Vol. 835, No. 2.

BibTeX

@article{6ed68866a78e482299dda2a963a93c25,
title = "Pulsational Pair-instability Model for Superluminous Supernova PTF12dam: Interaction and Radioactive Decay",
abstract = "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.",
keywords = "circumstellar matter, supernovae: general, supernovae: individual (PTF12dam), 2007BI, ANALYTIC FITS, LIGHT CURVES, RADIATION, PHOTOIONIZATION CROSS-SECTIONS, HYDROGEN, EXPLOSIONS, EVOLUTION, LUMINOUS SUPERNOVAE, STARS",
author = "Alexey Tolstov and Ken'Ichi Nomoto and Sergei Blinnikov and Elena Sorokina and Robert Quimby and Petr Baklanov",
year = "2017",
month = feb,
day = "1",
doi = "10.3847/1538-4357/835/2/266",
language = "English",
volume = "835",
journal = "Astrophysical Journal",
issn = "0004-637X",
publisher = "IOP Publishing Ltd.",
number = "2",

}

RIS

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 -

ID: 10311489