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Three-dimensional Hydrodynamics Simulations of Precollapse Shell Burning in the Si- and O-rich Layers
Solar and Stellar Astrophysics · Submitted 24 Dec 2020
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim Based on the results, we discuss implications for the possible onset of the perturbation-aided neutrino-driven supernova explosion.
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The abstract, sentence by sentence
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.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | 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. | contribution 0.97 | 0.97 | 0.08 | asserted 0.99 |
| s1 | The 22 and 27 $M_{\odot}$ stars are selected from a suite of 1D progenitors. | method 0.92 | 0.53 | 0.02 | asserted 1.00 |
| s2 | 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. | method 0.60 | 0.45 | 0.03 | asserted 1.00 |
| s3 | 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. | result 1.00 | 0.97 | 0.24 | asserted 1.00 |
| s4 | 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. | result 0.99 | 0.94 | 0.13 | asserted 1.00 |
| s5 | 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. | result 1.00 | 0.93 | 0.35 | asserted 1.00 |
| s6 | By performing a spectrum analysis, we investigate the growth of turbulence and its role of material mixing in the convective layers. | method 0.89 | 0.95 | 0.04 | asserted 0.84 |
| s7 | We also present a scalar spherical harmonics mode analysis of the turbulent Mach number. | method 0.76 | 0.94 | 0.04 | asserted 0.93 |
| s8 | This analytical formula would be helpful for supernova modelers to implement the precollapse perturbations in core-collapse supernova simulations. | future work 0.42 | 0.39 | 0.10 | hedged possibility 0.73 |
| s9 | Based on the results, we discuss implications for the possible onset of the perturbation-aided neutrino-driven supernova explosion. | interpretation 1.00 | 0.62 | 0.25 | hedged possibility 0.70 |
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Original 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.
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