Early Formation of Dust in the Ejecta of Type Ib SN 2006jc and Temperature and Mass of the Dust

SN 2006jc is a peculiar supernova (SN), in which the formation of dust has been confirmed at an early epoch of ∼50 days after the explosion. We investigate the possibility of such an earlier formation of dust grains in the expanding ejecta of SN 2006jc, applying the Type Ib SN model that is developed to reproduce the observed light curve. We find that the rapid decrease of the gas temperature in SN 2006jc enables the condensation of C grains in the C-rich layer at 40–60 days after the explosion, which is followed by the condensation of silicate and oxide grains until ∼200 days. The average radius of each grain species is confined to be less than 0.01 μm due to the low gas density at the condensation time. The calculated total dust mass reaches to ≃1.5 M⊙, of which C dust shares 0.7 M⊙. On the other hand, based on the calculated dust temperature, we show that the dust species and mass evaluated to reproduce the spectral energy distribution Department of Cosmosciences, Graduate School of Science, Hokkaido University, Sapporo 060-0810, Japan; [email protected] Department of Astronomy, School of Science, University of Tokyo, Bunkyo-ku, Tokyo 113-0033, Japan Research Center for the Early Universe, School of Science, University of Tokyo, Bunkyo-ku, Tokyo 113-0033, Japan Institute for the Physics and Mathematics of the Universe, University of Tokyo, Kashiwa, Chiba 2778568, Japan Max-Planck-Institut für Astrophysik, Karl-Schwarzschild Strasse 1, 85741 Garching, Germany 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