  We model dust formation in the core collapse supernova explosion SN 1987A by
treating the gas-phase formation of dust grain nuclei as a chemical process. To
compute the synthesis of fourteen species of grains we integrate a
non-equilibrium network of nucleating and related chemical reactions and follow
the growth of the nuclei into grains via accretion and coagulation. The effects
of the radioactive cobalt, titanium, and sodium on the thermodynamics and
chemistry of the ejecta are taken into account. The grain temperature, which we
allow to differ from the gas temperature, affects the surface-tension-corrected
evaporation rate. We also account for He$^+$, Ne$^+$, Ar$^+$, and O weathering.
We combine our dust synthesis model with a crude prescription for anisotropic
radioactive nickel dredge-up into the core ejecta, the so-called `nickel
bubbles', to compute the total dust mass and molecular-species-specific grain
size distribution. The total mass varies between $0.41\,M_\odot$ and
$0.73\,M_\odot$, depending on the bubble shell density contrast. In the
decreasing 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 strongly
enhances dust synthesis. This underscores the need for improved understanding
of hydrodynamic transport and mixing over the entire pre-homologous expansion.
