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SN 2006jc is a peculiar supernova (SN), in which the formation of dust hasbeen confirmed at an early epoch of ~50 days after the explosion. Weinvestigate the possibility of such an earlier formation of dust grains in theexpanding ejecta of SN 2006jc, applying the Type Ib SN model that is developedto reproduce the observed light curve. We find that the rapid decrease of thegas temperature in SN 2006jc enables the condensation of C grains in the C-richlayer at 40-60 days after the explosion, which is followed by the condensationof silicate and oxide grains until ~200 days. The average radius of each grainspecies is confined to be less than 0.01 micron due to the low gas density atthe condensation time. The calculated total dust mass reaches ~1.5 Msun, ofwhich C dust shares 0.7 Msun. On the other hand, based on the calculated dusttemperature, we show that the dust species and mass evaluated to reproduce thespectral energy distribution observed by AKARI and MAGNUM at day 200 aredifferent from those obtained by the dust formation calculations; the dustspecies contributing to the observed flux are hot C and FeS grains with massesof $5.6 \times 10^{-4}$ Msun and $2.0 \times 10^{-3}$ Msun, respectively,though we cannot defy the presence of a large amount of cold dust such assilicate and oxide grains up to 0.5 Msun. One of the physical processesresponsible for the difference between calculated and evaluated masses of C andFeS grains could be considered to be the destruction of small-sized clusters byenergetic photons and electrons prevailing within the ejecta at the earlierepoch.

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