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We study the formation of molecules and dust clusters in the ejecta of solarmetallicity, Type II-P supernovae using a chemical kinetic approach. We followthe evolution of molecules and small dust cluster masses from day 100 to day1500 after explosion. We consider stellar progenitors with initial mass of 12,15, 19 and 25 Msun that explode as supernovae with stratified ejecta. Themolecular precursors to dust grains comprise molecular chains, rings and smallclusters of silica, silicates, metal oxides, sulphides and carbides, puremetals, and carbon, where the nucleation of silicate clusters is described by atwo-step process of metal and oxygen addition. We study the impact of the 56Nimass on the type and amount of synthesised dust. We predict that large massesof molecules including CO, SiO, SiS, O2, and SO form in the ejecta. We showthat the discrepancy between the small dust masses detected at infraredwavelengths some 500 days post-explosion and the larger amounts of dustrecently detected with Herschel in supernova remnants can be explained by thenon-equilibrium chemistry linked to the formation of molecules and dustclusters in the ejected material. Dust gradually builds up from small (~10^{-5}Msun) to large masses (~5x 10^{-2} Msun) over a 5 yr period after explosion.Subsequent dust formation and/or growth is hampered by the shortage of chemicalagents participating in the dust nucleation and the long time scale foraccretion. The results highlight the dependence of the dust chemicalcomposition and mass on the amount of 56Ni synthesised during the explosion.This dependence may partly explain the diversity of epochs at which dust formsin supernovae. More generally, our results indicate that type II-P supernovaeare efficient but moderate dust producers with an upper limit on the mass ofsynthesised dust ranging from ~ 0.03 to 0.09 Msun.

The chemically controlled synthesis of dust in type II-P supernovae