One-, Two-, and Three-dimensional Simulations of Oxygen-shell Burning Just before the Core Collapse of Massive Stars
Astrophysical Journal, ISSN: 1538-4357, Vol: 881, Issue: 1
2019
- 67Citations
- 30Captures
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Article Description
We perform two- (2D) and three-dimensional (3D) hydrodynamics simulations of convective oxygen-shell burning that takes place deep inside a massive progenitor star of a core-collapse supernova. Using a one-dimensional (1D) stellar evolution code, we first calculate the evolution of massive stars with an initial mass of 9-40 M . Four different overshoot parameters are applied, and a CO-core mass trend similar to previous works is obtained in the 1D models. Selecting eleven 1D models that have a coexisting silicon and oxygen layer, we perform 2D hydrodynamics simulations of the evolution for ∼100 s until the onset of core collapse. We find that convection with large-scale eddies and the turbulent Mach number of ∼0.1 is obtained in the models having a Si/O layer with a scale of 10 cm, whereas most models that have an extended O/Si layer up to a few ×10 cm exhibit lower turbulent velocity. Our results indicate that the supernova progenitors that possess a thick Si/O layer could provide the preferred condition for perturbation-aided explosions. We perform the 3D simulation of a 25 M model, which exhibits large-scale convection in the 2D models. The 3D model develops large-scale (ℓ = 2) convection similar to the 2D model; however, the turbulent velocity is lower. By estimating the neutrino emission properties of the 3D model, we point out that a time modulation of the event rates, if observed in KamLAND and Hyper-Kamiokande, could provide important information about structural changes in the presupernova convective layer.
Bibliographic Details
http://www.scopus.com/inward/record.url?partnerID=HzOxMe3b&scp=85072050075&origin=inward; http://dx.doi.org/10.3847/1538-4357/ab2b9d; https://iopscience.iop.org/article/10.3847/1538-4357/ab2b9d; https://iopscience.iop.org/article/10.3847/1538-4357/ab2b9d/pdf; https://dx.doi.org/10.3847/1538-4357/ab2b9d; https://validate.perfdrive.com/fb803c746e9148689b3984a31fccd902/captcha?ssa=https%3A%2F%2Fiopscience.iop.org%2Farticle%2F10.3847%2F1538-4357%2Fab2b9d&ssb=eb53d929a062e67903d73d569bcfbc7137d0a8c8&ssc=MDI3MDQ5ZTAzYjcxLTcyNDgtZjNlNC03NDRiLWRhYzdkOTUy
American Astronomical Society
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