2020/12/31 by Takashi Yoshida, Tomoya Takiwaki, Kei Kotake +3 · 26 citations
Physics and Astronomy · #Adiabatic process #Convection #Gamma-ray bursts and supernovae #Mach number #Mixing (physics) #Neutrino Physics Research #Pulsars and Gravitational Waves Research #Spherical shell #Stars #Supernova #Turbulence #astro-ph.HE #astro-ph.SR
paper · pdf · doi:10.3847/1538-4357/abd3a3
published in The Astrophysical Journal 908(1), 44 (IOP Publishing) · 23 pages, 26 figures, 5 tables. Accepted for publication in Astrophys. J
openalex created_date 2021/01/05 · arxiv created 2021/01/25 · openalex publication_date 2021/02/01 · arxiv updated 2021/02/17 · openalex updated_date 2026/08/05
Abstract We present 3D hydrodynamics simulations of shell burning in two progenitors with zero-age main-sequence masses of 22 and 27 M ⊙ for ∼65 and 200 s up to the onset of gravitational collapse, respectively. The 22 and 27 M ⊙ stars are selected from a suite of 1D progenitors. The former and the latter have an extended Si- and O-rich layer with a width of ∼10 9 cm and ∼5 × 10 9 cm, respectively. Our 3D results show that turbulent mixing occurs in both of the progenitors with the angle-averaged turbulent Mach number exceeding ∼0.1 at the maximum. We observe that an episodic burning of O and Ne, which takes place underneath the convection bases, enhances the turbulent mixing in the 22 and 27 M ⊙ models, respectively. The distribution of nucleosynthetic yields is significantly different from that in 1D simulations, namely, in 3D more homogeneous and inhomogeneous in the radial and angular direction, respectively. By performing a spectrum analysis, we investigate the growth of turbulence and its role of material mixing in the convective layers. We also present a scalar spherical harmonics mode analysis of the turbulent Mach number. This analytical formula would be helpful for supernova modelers to implement the precollapse perturbations in core-collapse supernova simulations. Based on the results, we discuss implications for the possible onset of the perturbation-aided neutrino-driven supernova explosion.