• Limongi, M.
• Kozasa, T.
• Gurugubelli, U. K.
• Kaneda, H.
• Minezaki, T.
• Sahu, D. K.
• Yoshii, Y.
• Deng, J.
• Wada, T.
• Nomoto, K.
• Chieffi, Alessandro
• Tanabé, T.
• Tominaga, N.
• Nozawa, T.
• Ohyama, Y.
• Anupama, G. C.
• Tanaka, M.
• Kawabata, K. S.
• Onaka, T.
• Sakon, I.
• Maeda, K.
• Suzuki, T.
• Prabhu, T. P.
• Tornambe, A.

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 M<SUB>solar</SUB> on the zero-age main sequence. The star undergoes extensive mass loss to reduce its mass down to as small as 6.9 M<SUB>solar</SUB>, 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 M<SUB>solar</SUB>, hypernova-like explosion energy 10<SUP>52</SUP> ergs, and ejected <SUP>56</SUP>Ni mass 0.22 M<SUB>solar</SUB>. 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.

Topics

• density
• impedance spectroscopy
• amorphous
• Carbon
• grain
• liquid chromatography