Formation, distribution, and IR emission of dust in the clumpy ejecta of Type II-P core-collapse supernovae, in isotropic and anisotropic scenarios

Large discrepancies are found between observational estimates and theoretical predictions when exploring the characteristics of dust formed in ejecta core-collapse supernovae. We revisit scenario production typical supernova first 3000 days after explosion, with an improved understanding evolving physical conditions distribution clumps. The generic, nonuniform within was determined using that, relevant opacities fluxes were calculated. dependence emerging on viewing angle estimated for anisotropic, ellipsoidal geometry that imitate SN 1987A. model He-core from center to its outer edge as 450 stratified, clumpy, annular shells, uniquely identified by their distinct velocities characterized variations abundances, densities, gas temperatures. find formation starts day 550 post-explosion, it continues until about 2800, although 1600 most productive. total mass evolves 10^-5 Msun at 500 10^-3 800, finally saturating 0.06 Msun. masses O-rich (silicates, alumina) dominates C-rich (amorphous carbon, silicon carbide) all times; carbon is delayed beyond 2000 post-explosion. show largest 800 1600, characteristic spectral features species suppressed those times. along smallest axes be obscured, while a 16 21 degrees axis appears best agreement 1987A 615 775.