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We model dust formation in the core collapse supernova explosion SN 1987A bytreating the gas-phase formation of dust grain nuclei as a chemical process. Tocompute the synthesis of fourteen species of grains we integrate anon-equilibrium network of nucleating and related chemical reactions and followthe growth of the nuclei into grains via accretion and coagulation. The effectsof the radioactive cobalt, titanium, and sodium on the thermodynamics andchemistry of the ejecta are taken into account. The grain temperature, which weallow to differ from the gas temperature, affects the surface-tension-correctedevaporation rate. We also account for He$^+$, Ne$^+$, Ar$^+$, and O weathering.We combine our dust synthesis model with a crude prescription for anisotropicradioactive nickel dredge-up into the core ejecta, the so-called `nickelbubbles', to compute the total dust mass and molecular-species-specific grainsize distribution. The total mass varies between $0.41\,M_\odot$ and$0.73\,M_\odot$, depending on the bubble shell density contrast. In thedecreasing order of abundance, the grain species produced are: magnesia,silicon, forsterite, iron sulfide, carbon, silicon dioxide, alumina, and iron.The combined grain size distribution is a power law $dN/da\propto a^{-4.39}$.Early ejecta compaction by expanding radioactive nickel bubbles stronglyenhances dust synthesis. This underscores the need for improved understandingof hydrodynamic transport and mixing over the entire pre-homologous expansion.

Molecular nucleation theory of dust formation in core-collapse supernovae applied to SN 1987A