Abstract
We present the first three-dimensional study of the asymptotic ejecta distributions for a suite of theoretical Type IIp supernovae originating from red supergiant (RSG) progenitors. We simulate using the radiation hydrodynamic code FORNAX from the core bounce through to the first seconds of the neutrino-driven explosion and then follow using a hydrodynamic variant of the code FLASH until the shock breakout of the star and through to homologous expansion of the ejecta into the circumstellar environment. Our studied progenitor models range from 9 to 25 M⊙, with explosion energies spanning ∼0.1−1 Bethe. The shock breakout times span the range of ∼1−4 days, with a breakout time spread by direction ranging from hours to over a day. We find that the dipole orientation of the 56Ni ejecta is well preserved from the first seconds out to the shock breakout. The 56Ni ejecta penetrates through the initially outer oxygen shell, and its global structure is imprinted with small-scale clumping as the ejecta evolve through the stellar envelope. For the majority of our models, the neutron star kick is anti-aligned with the 56Ni ejecta. Models with strongly dipolar ejecta morphology and a massive hydrogen/helium envelope with an inner boundary located deep see as much as ∼70% of the 56Ni ejecta mixed into that outer envelope, reaching asymptotic velocities ranging from ∼350 to 3200 km s−1. Supernovae arising from RSG progenitors and exhibiting prominent nickel features generally display significant 56Ni mixing into the stellar envelope.