Stellar Turbulent Convection. I. Theory

Canuto, V.; Dubovikov, M. S.

doi:10.1086/305141

Cited by 109 publications

(195 citation statements)

References 49 publications

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“…We fix two of the TCM parameters as C s = 0.08 and C k = 2.5, in agreement with the turbulence model of Canuto & Dubovikob (1998). The parameter α TCM is determined by calibrating the models to the solar parameters.…”

Section: Input Physics Of Solar Modelsmentioning

confidence: 99%

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Turbulent Convection Model in the Overshooting Region. I. Effects of the Convective Mixing in the Solar Overshooting Region

Zhang

2012

ApJ

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The overshooting in the framework of the turbulent convection model is investigated in the solar overshooting region. The overshooting mixing is treated as a diffusive process. It is found that the sound speed profile can be improved to be in good agreement with helioseismic inversions. The bump in the sound speed differences between solar models and the helioseismical inversions below the base of the solar convective envelope is almost eliminated by the overshooting mixing. The overshooting mixing leads to a significant depletion of Li in the main-sequence stage. Li abundance in the solar surface can be reduced to about 1% of its initial abundance in the solar models with the overshooting mixing. The solar model with the overshooting shows a smooth profile of the temperature gradient, which is also favored by the helioseismology.

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Section: Input Physics Of Solar Modelsmentioning

confidence: 99%

“…TCMs have been developed for the stellar convection in the past 30 years (Xiong 1981(Xiong , 1985Canuto 1993;Canuto & Dubovikob 1998;Xiong & Deng 2001;Deng & Xiong 2006, 2008Li & Yang 2007). Applying TCMs to model turbulent movements is physically more reliable (Hinze 1975) than the standard MLT.…”

Section: Introductionmentioning

confidence: 99%

Turbulent Convection Model in the Overshooting Region. I. Effects of the Convective Mixing in the Solar Overshooting Region

Zhang

2012

ApJ

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“…However, in a stellar context, one must include a Peclet number dependence because radiative losses by the eddies weaken the strength of turbulence. Adopting the treatment developed elsewhere (Canuto & Dubovikov 1998;Canuto et al 2008a,b), we now have:…”

Section: The Dissipation-relaxation Time Scales π Smentioning

confidence: 99%

Stellar mixing

Canuto

2011

A&A

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In this paper we use the Reynolds stress models (RSM) to derive algebraic expressions for the following variables: a) heat fluxes; b) μ fluxes; and c) momentum fluxes. These relations, which are fully 3D, include: 1) stable and unstable stratification, represented by the Brunt-Väisäla frequency,; 2) double diffusion, salt-fingers, and semi-convection, represented by the density ratio R μ = ∇ μ (∇ − ∇ ad ) −1 ; 3) shear (differential rotation), represented by the mean squared shear Σ 2 or by the Richardson number, Ri = N 2 Σ −2 ; 4) radiative losses represented by a Peclet number, Pe; 5) a complete analytical solution of the 1D version of the model. In general, the model requires the solution of two differential equations for the eddy kinetic energy K and its rate of dissipation, ε. In the local and stationary cases, when production equals dissipation, the model equations are all algebraic.

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“…Following the model of Canuto and Dubovikov (1998) and the approach of Kupka & Montgomery (2002), we solved the equations for the turbulent quantities on a weighted mass grid. Other quantities are computed on the same weighted mass grid in the envelope and on a log(τ ross ) grid in the stellar atmosphere.…”

Section: Discussionmentioning

confidence: 99%

Modelling convection in A star atmospheres

Stütz¹

2009

A&A

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Context. We present a code, VeDyn, for modelling envelopes and atmospheres of A to F stars focusing on accurate treatment of convective processes. Aims. VeDyn implements a highly sophisticated non-local convection model but is fast and can be used in practical astrophysical applications. Methods. We developed the HME envelope solver for this convection model to consistently model the envelope together with the stellar atmosphere. The synthesis code SynthV was extended to account for the resulting velocity structure. Finally, we tested our approach on atomic line bisectors. Results. It is shown that our synthetic line bisectors of HD 108642 bend towards the blue and are of a magnitude comparable to the observed ones. Conclusions. Even though this approach of modelling convection requires the solution of a coupled system of nonlinear differential equations, it is fast enough to be applicable to many of the investigation techniques relying on model atmospheres.

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Stellar Turbulent Convection. I. Theory

Cited by 109 publications

References 49 publications

Turbulent Convection Model in the Overshooting Region. I. Effects of the Convective Mixing in the Solar Overshooting Region

Turbulent Convection Model in the Overshooting Region. I. Effects of the Convective Mixing in the Solar Overshooting Region

Stellar mixing

Modelling convection in A star atmospheres

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