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Infrared (IR) observations of core collapse supernovae (CCSNe) have been usedto infer the mass of dust that has formed in their ejecta. A plot of inferreddust masses versus supernova (SN) ages shows a trend of increasing dust masswith time, spanning a few decades of observations. This trend has beeninterpreted as evidence for the slow and gradual formation of dust in CCSNe.Observationally, the trend exhibits a $ t^2$ behavior, exactly what is expectedfrom an expanding optically thick ejecta. In this case, the observed dustresides in the infrared (IR)-thin "photosphere" of the ejecta, and constitutesonly a fraction of the total dust mass. We therefore propose that dustformation proceeds very rapidly, condensing most available refractory elementswithin two years after the explosion. At early epochs, only a fraction of thedust emission escapes the ejecta accounting for the low observed dust mass. Theejecta's entire dust content is unveiled only a few decades after theexplosion, with the gradual decrease in its IR opacity. Corroborating evidencefor this picture includes the early depletions of refractory elements in theejecta of SN1987A and the appearance of a silicate emission band around day 300in SN~2004et.

The Evolution of Dust Opacity in Core Collapse Supernovae and the Rapid Formation of Dust in Their Ejecta