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 progenitors. We simulate using the radiation-hydrodynamic code Fornax from core bounce through the first seconds of the neutrino-driven explosion and then follow using a hydrodynamic variant of the code FLASH until 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 $_{\odot}$ , with explosion energies spanning$\sim$ 0.1 $-$ 1 Bethe. The shock breakout times span the range$\sim$ 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$^{56}$ Ni ejecta is well-preserved from the first seconds out to shock breakout. The$^{56}$ Ni 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$^{56}$ Ni ejecta. Models with strongly dipolar ejecta morphology and a massive hydrogen/helium envelope with an inner boundary located deep see as much as$\sim$ 70\% of the$^{56}$ Ni ejecta mixed into that outer envelope, reaching asymptotic velocities ranging from$\sim$ 350 to 3200 km s $^{-1}$ . Supernovae arising from red supergiant progenitors and exhibiting prominent nickel features generally display significant$^{56}$ Ni mixing into the stellar envelope.