Three-dimensional Hydrodynamics Simulations of Precollapse Shell Burning in the Si- and O-rich Layers. (arXiv:2012.13261v2 [astro-ph.SR] UPDATED)
<a href="http://arxiv.org/find/astro-ph/1/au:+Yoshida_T/0/1/0/all/0/1">Takashi Yoshida</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Takiwaki_T/0/1/0/all/0/1">Tomoya Takiwaki</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kotake_K/0/1/0/all/0/1">Kei Kotake</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Takahashi_K/0/1/0/all/0/1">Koh Takahashi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Nakamura_K/0/1/0/all/0/1">Ko Nakamura</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Umeda_H/0/1/0/all/0/1">Hideyuki Umeda</a>
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.
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.
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