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The light curves of Type IIn supernovae are dominated by the radiative energyreleased through the interaction of the supernova shockwaves with their densecircumstellar medium (CSM). The ultraluminous Type IIn supernova SN 2010jlexhibits an infrared emission component that is in excess of the extrapolatedUV-optical spectrum as early as a few weeks post-explosion. This emission hasbeen attributed by some as evidence for rapid formation of dust in the coolingpostshock CSM. We investigate the physical processes that may inhibit orfacilitate the formation of dust in the CSM. When only radiative cooling isconsidered, the temperature of the dense shocked gas rapidly drops below thedust condensation temperature. However, by accounting for the heating of thepostshock gas by the downstream radiation from the shock, we show that dustformation is inhibited until the radiation from the shock weakens, as the shockpropagates into the less dense outer regions of the CSM. In SN 2010jl dustformation can therefore only commence after day 380. Only the IR emission sincethat epoch can be attributed to the newly formed CSM dust. Observations on day460 and later show that the IR luminosity exceeds the UV-optical luminosity.The post-shock dust cannot extinct the radiation emitted by the expanding SNshock. Therefore, its IR emission must be powered by an interior source, whichwe identify with the reverse shock propagating through the SN ejecta. IRemission before day 380 must therefore be an IR echo from preexisting CSM dust.

Delayed Shock-induced Dust Formation in the Dense Circumstellar Shell Surrounding the Type IIn Supernova SN 2010jl