Please use this identifier to cite or link to this item: http://hdl.handle.net/2248/1094
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
Keywords: Dust, extinction — infrared;ISM—nuclear reactions;Nucleosynthesis;Abundances—supernovae;General—supernovae: individual (SN 2006jc)—stars;Wolf-Rayet
Issue Date: Nov-2008
Publisher: The American Astronomical Society
Citation: The Astrophysical Journal, Vol. 687, No. 2, pp. 1208 – 1219
Abstract: ISM: Dust, Extinction, Infrared: ISM, Nuclear Reactions, Nucleosynthesis, Abundances, Stars: Supernovae: General, supernovae: individual (SN 2006jc), Stars: Wolf-Rayet 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
URI: http://hdl.handle.net/2248/1094
ISSN: 0004-637X
???metadata.dc.rights???: © The American Astronomical Society. All rights reserved
???metadata.dc.relation.uri???: http://www.journals.uchicago.edu/doi/abs/10.1086/591782
http://adsabs.harvard.edu/abs/2008ApJ...687.1208T
http://arxiv.org/abs/0711.4782
Appears in Collections:Publications based on data from IAO, Hanle
IIAP Publications

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