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Title:
The Peculiar Type Ib Supernova 2006jc: A WCO Wolf-Rayet Star Explosion
Authors:
Tominaga, N.; Limongi, M.; Suzuki, T.; Tanaka, M.; Nomoto, K.; Maeda, K.; Chieffi, A.; Tornambe, A.; Minezaki, T.; Yoshii, Y.; Sakon, I.; Wada, T.; Ohyama, Y.; Tanabé, T.; Kaneda, H.; Onaka, T.; Nozawa, T.; Kozasa, T.; Kawabata, K. S.; Anupama, G. C.; Sahu, D. K.; Gurugubelli, U. K.; Prabhu, T. P.; Deng, J.
Affiliation:
AA(Optical and Infrared Astronomy Division, National Astronomical Observatory, 2-21-1 Osawa, Mitaka, Tokyo, Japan; .; Department of Astronomy, School of Science, University of Tokyo, 7-3-1 Hongo, Bunkyo-ku, Tokyo, Japan.), AB(Department of Astronomy, School of Science, University of Tokyo, 7-3-1 Hongo, Bunkyo-ku, Tokyo, Japan.; Istituto Nazionale di Astrofisica-Osservatorio Astronomico di Roma, Via Frascati 33, I-00040, Monteporzio Catone, Italy.; Center for Stellar and Planetary Astrophysics, School of Mathematical Sciences, P.O. Box, 28M, Monash University, Victoria 3800, Australia.), AC(Department of Astronomy, School of Science, University of Tokyo, 7-3-1 Hongo, Bunkyo-ku, Tokyo, Japan.), AD(Department of Astronomy, School of Science, University of Tokyo, 7-3-1 Hongo, Bunkyo-ku, Tokyo, Japan.), AE(Department of Astronomy, School of Science, University of Tokyo, 7-3-1 Hongo, Bunkyo-ku, Tokyo, Japan.; Institute for the Physics and Mathematics of the Universe, University of Tokyo, 5-1-5 Kashiwa, Chiba, Japan.), AF(Institute for the Physics and Mathematics of the Universe, University of Tokyo, 5-1-5 Kashiwa, Chiba, Japan.; Max-Planck-Institut für Astrophysik, Karl-Schwarzschild Strasse 1, 85741 Garching, Germany.), AG(Istituto Nazionale di Astrofisica-Istituto di Astrofisica Spaziale e Fisica Cosmica, Via Fosso del Cavaliere 100, Roma, Italy.), AH(Istituto Nazionale di Astrofisica-Osservatorio Astronomico di Roma, Via Frascati 33, I-00040, Monteporzio Catone, Italy.), AI(Institute of Astronomy, School of Science, University of Tokyo, 2-21-1 Osawa, Mitaka, Tokyo, Japan.), AJ(Institute of Astronomy, School of Science, University of Tokyo, 2-21-1 Osawa, Mitaka, Tokyo, Japan.), AK(Department of Astronomy, School of Science, University of Tokyo, 7-3-1 Hongo, Bunkyo-ku, Tokyo, Japan.), AL(Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, 3-1-1 Yoshinodai, Sagamihara, Kanagawa, Japan.), AM(Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, 3-1-1 Yoshinodai, Sagamihara, Kanagawa, Japan.), AN(Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, 3-1-1 Yoshinodai, Sagamihara, Kanagawa, Japan.), AO(Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, 3-1-1 Yoshinodai, Sagamihara, Kanagawa, Japan.), AP(Department of Astronomy, School of Science, University of Tokyo, 7-3-1 Hongo, Bunkyo-ku, Tokyo, Japan.), AQ(Department of Cosmosciences, Graduate School of Science, Hokkaido University, Sapporo, Japan.), AR(Department of Cosmosciences, Graduate School of Science, Hokkaido University, Sapporo, Japan.), AS(Hiroshima Astrophysical Science Center, Hiroshima University, Hiroshima, Japan.), AT(Indian Institute of Astrophysics, Bangalore 560 034, India.), AU(Indian Institute of Astrophysics, Bangalore 560 034, India.), AV(Indian Institute of Astrophysics, Bangalore 560 034, India.), AW(Indian Institute of Astrophysics, Bangalore 560 034, India.), AX(National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012, China.)
Publication:
The Astrophysical Journal, Volume 687, Issue 2, pp. 1208-1219. (ApJ Homepage)
Publication Date:
11/2008
Origin:
UCP
ApJ Keywords:
ISM: Dust, Extinction, Infrared: ISM, Nuclear Reactions, Nucleosynthesis, Abundances, Stars: Supernovae: General, supernovae: individual (SN 2006jc), Stars: Wolf-Rayet
DOI:
10.1086/591782
Bibliographic Code:
2008ApJ...687.1208T

Abstract

We present a theoretical model for Type Ib supernova (SN) 2006jc. We calculate the evolution of the progenitor star, hydrodynamics and nucleosynthesis of the SN explosion, and the SN bolometric light curve (LC). The synthetic bolometric LC is compared with the observed bolometric LC constructed by integrating the UV, optical, near-infrared (NIR), and mid-infrared (MIR) fluxes. The progenitor is assumed to be as massive as 40 Msolar on the zero-age main sequence. The star undergoes extensive mass loss to reduce its mass down to as small as 6.9 Msolar, thus becoming a WCO Wolf-Rayet star. The WCO star model has a thick carbon-rich layer, in which amorphous carbon grains can be formed. This could explain the NIR brightening and the dust feature seen in the MIR spectrum. We suggest that the progenitor of SN 2006jc is a WCO Wolf-Rayet star having undergone strong mass loss, and such massive stars are important sites of dust formation. We derive the parameters of the explosion model in order to reproduce the bolometric LC of SN 2006jc by the radioactive decays: the ejecta mass 4.9 Msolar, hypernova-like explosion energy 1052 ergs, and ejected 56Ni mass 0.22 Msolar. We also calculate the circumstellar interaction and find that a CSM with a flat density structure is required to reproduce the X-ray LC of SN 2006jc. This suggests a drastic change of the mass-loss rate and/or the wind velocity that is consistent with the past luminous blue variable (LBV)-like event.
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