2018MNRAS.480.5580S

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 14 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 ⁵⁶Co, ⁵⁷Co, ⁴⁴Ti, and ²²Na 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 ⁵⁶Ni 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 and 0.73 M_☉, 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 ∝ a^–4.39. Early ejecta compaction by expanding radioactive ⁵⁶Ni bubbles strongly enhances dust synthesis. This underscores the need for improved understanding of hydrodynamic transport and mixing over the entire pre-homologous expansion.