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In supernovae (SNe), where the light curves show evidence of strong and earlyinteraction between the ejecta and the circumstellar matter (CSM), theformation of new dust is estimated to take place in a dense shell of gasbetween the forward (FS) and the reverse shock (RS). For the first time, inthis study, the mechanism of dust formation in this dense shell is modeled. Aset of 9 cases, considering variations of the ejecta mass, and thepre-explosion mass-loss rates is considered, accounting for the diverse natureof interactions reported in such SNe. For a single main sequence mass, thevariation of ejecta mass was manifested as a variation of the H-shell mass ofthe star, lost due to pre-explosion mass-loss. We find that the dust masses inthe dense shell range between 10$^{-3}$ M$_{\odot}$ and 0.8 M$_{\odot}$,composed of O-rich and C-rich grains, whose relative proportions are determinedby the nature of interaction. Dust formation in the post-shock gas ischaracterized by a gradual production rate, mostly ranging from 10$^{-6}$ to10$^{-3}$ M$_{\odot}$ day$^{-1}$, which may continue for a decade,post-explosion. A higher mass-loss rate leads to a larger mass of dust, while asmaller ejecta mass (smaller left-over H-shell) increases the efficiency ofdust production in such SNe. Dust formed behind the RS, as in our calculations,is not subject to destruction by either the FS or RS and is thus likely tosurvive in larger proportion than dust formed in the ejecta.

Dust Production in a Thin Dense Shell in Supernovae with Early Circumstellar Interactions