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#### Three-dimensional Hydrodynamics Simulations of Precollapse Shell Burning in the Si- and O-rich Layers

##### Fulltext (public)

2012.13261.pdf

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##### Supplementary Material (public)

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##### Citation

Yoshida, T., Takiwaki, T., Kotake, K., Takahashi, K., Nakamura, K., & Umeda, H. (2021).
Three-dimensional Hydrodynamics Simulations of Precollapse Shell Burning in the Si- and O-rich Layers.*
The Astrophysical Journal,* *908*(1): 44. doi:10.3847/1538-4357/abd3a3.

Cite as: http://hdl.handle.net/21.11116/0000-0008-16F6-A

##### Abstract

We present 3D hydrodynamics simulations of shell burning in two progenitors
with zero-age main-sequence masses of 22 and 27 $M_{\odot}$ for $\sim$65 and
200 s up to the onset of gravitational collapse, respectively. The 22 and 27
$M_{\odot}$ 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 $\sim$10$^9$
cm and $\sim$5$\times 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 $\sim$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 $M_\odot$ 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.