3D hydrodynamic simulations of carbon burning in massive stars

Cristini, Andréa; Meakin, Casey; Hirschi, Raphaël; Arnett, David; Georgy, Cyril; Viallet, Maxime; Walkington, Ian

doi:10.1093/mnras/stx1535

Cited by 87 publications

(126 citation statements)

References 69 publications

(130 reference statements)

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“…This is confirmed by movies of (1) the evolution in time ("Very high resolution movie of the C-shell"), and of (2) a fly-through of the computations at a given instant in time Figure 1. Vertical slice of a 3D, 1024 3 simulation of a carbon burning shell (Cristini, et al 2017). Velocity magnitudes are shown (red is high; white is medium; blue is low).…”

Section: Simulation Methodsmentioning

confidence: 99%

“…The simulations extend in resolution from above the integral scale of turbulence, down to well inside the inertial range of the cascade (Cristini, et al 2017). The full cascade is represented because the method used (PPM, Colella & Woodward (1984)) solves the Riemann problem for nonlinear flow at the individual zone level.…”

Section: Methods: Iles and Ramentioning

confidence: 99%

“…Fig. 2, top pane, shows the evolution in time of specific turbulent kinetic energy (TKE) in the carbon-burning simulations (Cristini, et al 2017(Cristini, et al , 2018, for resolutions of 128 3 , 256 3 , and 512 3 . Multi-mode behavior, like that seen in Meakin & Arnett (2007b) (Fig 4) and Arnett, Meakin & Young (2009) (Fig.…”

Section: Evolution Of Turbulent Kinetic Energymentioning

confidence: 99%

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3D Simulations and MLT. I. Renzini’s Critique

Arnett

Hirschi

Cristini

et al. 2019

ApJ

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Renzini (1987) wrote an influential critique of mixing-length theory (Böhm-Vitense 1958, MLT) as used in stellar evolution codes, and concluded that three-dimensional (3D) fluid dynamical simulations were needed to clarify several important issues. We have critically explored the limitations of the numerical methods and conclude that they are approaching the required accuracy Woodward et al. 2015). Implicit large eddy simulations (ILES) automatically connect large scale turbulence to a Kolmogorov cascade below the grid scale, allowing turbulent boundary layers to remove singularities that appear in the theory. Interactions between coherent structures give multi-modal behavior, driving intermittency and fluctuations. Reynolds averaging (RA) allows us to abstract the essential features of this dynamical behavior of boundaries which are appropriate to stellar evolution, and consider how they relate static boundary conditions (Richardson, Schwarzschild or Ledoux). We clarify several questions concerning when and why MLT works, and does not work, using both analytical theory and 3D high resolution numerical simulations. The composition gradients and boundary layer structure which are produced by our simulations suggest a self-consistent approach to boundary layers, removing the need for ad hoc procedures for 'convective overshooting' and 'semi-convection'. In a companion paper we quantify the adequacy of our numerical resolution, determine of the length scale of dissipation (the 'mixing length') without astronomical calibration, quantify agreement with the four-fifths law of Kolmogorov for weak stratification, and extend MLT to deal with strong stratification.

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Section: Simulation Methodsmentioning

confidence: 99%

Section: Methods: Iles and Ramentioning

confidence: 99%

Section: Evolution Of Turbulent Kinetic Energymentioning

confidence: 99%

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3D Simulations and MLT. I. Renzini’s Critique

Arnett

Hirschi

Cristini

et al. 2019

ApJ

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“…Then, it is impossible to cover the whole evolution of a star by multi-dimensional hydrodynamical simulations (for compressible fluids) in which the time step is limited by the maximum fluid velocity or the maximum sound speed inside the computational domain from the Courant-Friedrichs-Lewy (CFL) condition. Nevertheless, there have been attempts at such multi-dimensional hydrodynamical simulations of the evolution of massive stars which cover one or a few burning shells (for up to a few convection turnover times in the case of 3D simulations) (Bazan & Arnett 1994;Bazán & Arnett 1998;Meakin & Arnett 2006, 2007aArnett et al 2009;Arnett & Meakin 2011a;Viallet et al 2013;Couch et al 2015;Chatzopoulos et al 2016;Müller et al 2016;Cristini et al 2017;Mocák et al 2018;Yoshida et al 2019). As seen in e.g., Figures 3 and 4 in Müller et al (2016), the distributions of 28 Si and radial velocities are very fluctuating with large-scale anisotropies.…”

Section: Issues In Stellar Evolution Models and Impacts Of Possible Lmentioning

confidence: 99%

Matter Mixing in Aspherical Core-collapse Supernovae: Three-dimensional Simulations with Single-star and Binary Merger Progenitor Models for SN 1987A

Ono

Nagataki

Ferrand

et al. 2020

ApJ

104

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We perform three-dimensional hydrodynamic simulations of aspherical core-collapse supernovae focusing on the matter mixing in SN 1987A. The impacts of four progenitor (pre-supernova) models and parameterized aspherical explosions are investigated. The four pre-supernova models include a blue supergiant (BSG) model based on a slow merger scenario developed recently for the progenitor of SN 1987A (Urushibata et al. 2018. The others are a BSG model based on a single star evolution and two red supergiant (RSG) models. Among the investigated explosion (simulation) models, a model with the binary merger progenitor model and with an asymmetric bipolar-like explosion, which invokes a jetlike explosion, best reproduces constraints on the mass of high velocity 56 Ni, as inferred from the observed [Fe II] line profiles. The advantage of the binary merger progenitor model for the matter mixing is the flat and less extended ρ r 3 profile of the C+O core and the helium layer, which may be characterized by the small helium core mass. From the best explosion model, the direction of the bipolar explosion axis (the strongest explosion direction), the neutron star (NS) kick velocity, and its direction are predicted. Other related implications and future prospects are also given.

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“…fig. 6 of Cristini et al 2017). The magnitude and direction of the arrows represent the speed and direction of the and velocity fields within the xy plane.…”

Section: General Flow Propertiesmentioning

confidence: 99%

Dependence of convective boundary mixing on boundary properties and turbulence strength

Cristini

Hirschi

Meakin

et al. 2019

Monthly Notices of the Royal Astronomical Society

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Convective boundary mixing is one of the major uncertainties in stellar evolution. In order to study its dependence on boundary properties and turbulence strength in a controlled way, we computed a series of 3D hydrodynamical simulations of stellar convection during carbon burning with a varying boosting factor of the driving luminosity. Our 3D implicit large eddy simulations were computed with the prompi code. We performed a mean field analysis of the simulations within the Reynolds-averaged Navier-Stokes framework. Both the vertical RMS velocity within the convective region and the bulk Richardson number of the boundaries are found to scale with the driving luminosity as expected from theory: ∝ 1/3 and Ri B ∝ −2/3 , respectively. The positions of the convective boundaries were estimated through the composition profiles across them, and the strength of convective boundary mixing was determined by analysing the boundaries within the framework of the entrainment law. We find that the entrainment is approximately inversely proportional to the bulk Richardson number, Ri B (∝ Ri − B , ∼ 0.75). Although the entrainment law does not encompass all the processes occurring at boundaries, our results support the use of the entrainment law to describe convective boundary mixing in 1D models, at least for the advanced phases. The next steps and challenges ahead are also discussed.

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3D hydrodynamic simulations of carbon burning in massive stars

Cited by 87 publications

References 69 publications

3D Simulations and MLT. I. Renzini’s Critique

3D Simulations and MLT. I. Renzini’s Critique

Matter Mixing in Aspherical Core-collapse Supernovae: Three-dimensional Simulations with Single-star and Binary Merger Progenitor Models for SN 1987A

Dependence of convective boundary mixing on boundary properties and turbulence strength

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