2025/09/19 by David Vartanyan, Vartanyan, David, Adam Burrows +11
Physics and Astronomy · #Astronomy and Astrophysical Research #FOS: Physical sciences #Gamma-ray bursts and supernovae #High Energy Astrophysical Phenomena (astro-ph.HE) #Solar and Stellar Astrophysics (astro-ph.SR)
paper · pdf · doi:10.48550/arxiv.2509.16314
openalex publication_date 2025/09/19 · openalex created_date 2025/10/16 · openalex updated_date 2026/07/28
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 F\scornax 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 ∼0.1-1 Bethe. The shock breakout times span the range ∼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 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 red supergiant progenitors and exhibiting prominent nickel features generally display significant 56Ni mixing into the stellar envelope.