1999/11/30 by K. Kifonidis, T. Plewa, Hans‐Thomas Janka +3 · 5 citations
Engineering · Physics and Astronomy · #Astrophysics #Gamma-ray bursts and supernovae #Inner core #Neutrino #Neutrino Physics Research #Nuclear physics #Nuclear reactor physics and engineering #Nucleosynthesis #Physics #Red giant #Red supergiant #Stars #Supergiant #Supernova #Type II supernova #astro-ph
paper · pdf · doi:10.1086/312541
8 pages, LaTeX, 2 postscript figures, 2 gif figures, shortened and slightly revised text and references, accepted by ApJ Letters
arxiv created 2000/01/12 · openalex publication_date 2000/03/10 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
High-resolution two-dimensional simulations were performed for the first 5 minutes of the evolution of a core-collapse supernova explosion in a 15 M middle dot in circle blue supergiant progenitor. The computations start shortly after bounce and include neutrino-matter interactions by using a lightbulb approximation for the neutrinos and a treatment of the nucleosynthesis due to explosive silicon and oxygen burning. We find that newly formed iron-group elements are distributed throughout the inner half of the helium core by Rayleigh-Taylor instabilities at the (Ni + Si)/O and (C + O)/He interfaces, seeded by convective overturn during the early stages of the explosion. Fast-moving nickel mushrooms with velocities up to approximately 4000 km s-1 are observed. This offers a natural explanation for the mixing required in light-curve and spectral synthesis studies of Type Ib explosions. A continuation of the calculations to later times, however, indicates that the iron velocities observed in SN 1987A cannot be reproduced because of a strong deceleration of the clumps in the dense shell left behind by the shock at the He/H interface.