Impact of radial truncation on global 2D hydrodynamic simulations for a Sun-like model

A. Le Saux; A. Morison; D. G. Vlaykov; I. Baraffe; J. Pratt; T. Constantino; T. Goffrey; T. Guillet

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Impact of radial truncation on global 2D hydrodynamic simulations for a Sun-like model

D. G. Vlaykov, I. Baraffe, T. Constantino, T. Goffrey, T. Guillet, A. Le Saux, A. Morison, J. Pratt

Solar and Stellar Astrophysics · Submitted 9 May 2022

abstract compiled · 2026-09-23 · no language-model review

The authors' main claim However, we find that extending the outer boundary by only a few percent of the stellar radius significantly increases the velocity and temperature perturbations in the convection zone, the overshooting depth, the power and the spectral slope of the IGWs.

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arXiv ID2205.04270 (version 1)

Pith IDFEUUNB26, Pith's permanent record of this paper and its review

CitationA. Le Saux, A. Morison, D. G. Vlaykov, I. Baraffe, J. Pratt, T. Constantino, T. Goffrey, T. Guillet. "Impact of radial truncation on global 2D hydrodynamic simulations for a Sun-like model." arXiv:2205.04270 (2022). https://pith.science/paper/FEUUNB26

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Stellar convection is a non-local process responsible for the transport of heat and chemical species. It can lead to enhanced mixing through convective overshooting and excitation of internal gravity waves (IGWs) at convective boundaries. The relationship between these processes is still not well understood and requires global hydrodynamic simulations to capture the important large-scale dynamics. The steep stratification in stellar interiors suggests that the radial extent of such simulations can affect the convection dynamics, the IGWs in the stably stratified radiative zone, and the depth of the overshooting layer. We investigate these effects using two-dimensional global simulations performed with the fully compressible stellar hydrodynamics code MUSIC. We compare eight different radial truncations of the same solar-like stellar model evolved over approximately 400 convective turnover times. We find that the location of the inner boundary has an insignificant effect on the convection dynamics, the convective overshooting and the travelling IGWs. We relate this to the background conditions at the lower convective boundary which are unaffected by the truncation, as long as a significantly deep radiative layer is included in the simulation domain. However, we find that extending the outer boundary by only a few percent of the stellar radius significantly increases the velocity and temperature perturbations in the convection zone, the overshooting depth, the power and the spectral slope of the IGWs. The effect is related to the background conditions at the outer boundary, which are determined in essence by the hydrostatic stratification and the given luminosity.

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What the classifier reports for each sentence. The number is the probability it gave the label.
#	sentence	role	the authors' own work	states the main conclusion	strength
s0	Stellar convection is a non-local process responsible for the transport of heat and chemical species.	background 1.00	0.04	0.02	asserted 1.00
s1	It can lead to enhanced mixing through convective overshooting and excitation of internal gravity waves (IGWs) at convective boundaries.	background 1.00	0.06	0.02	hedged possibility 0.96
s2	The relationship between these processes is still not well understood and requires global hydrodynamic simulations to capture the important large-scale dynamics.	gap 0.93	0.04	0.02	asserted 0.96
s3	The steep stratification in stellar interiors suggests that the radial extent of such simulations can affect the convection dynamics, the IGWs in the stably stratified radiative zone, and the depth of the overshooting layer.	background 0.88	0.09	0.04	hedged possibility 0.98
s4	We investigate these effects using two-dimensional global simulations performed with the fully compressible stellar hydrodynamics code MUSIC.	method 0.94	0.94	0.02	asserted 0.95
s5	We compare eight different radial truncations of the same solar-like stellar model evolved over approximately 400 convective turnover times.	method 0.94	0.97	0.02	asserted 0.96
s6	We find that the location of the inner boundary has an insignificant effect on the convection dynamics, the convective overshooting and the travelling IGWs.	result 1.00	0.97	0.31	asserted 1.00
s7	We relate this to the background conditions at the lower convective boundary which are unaffected by the truncation, as long as a significantly deep radiative layer is included in the simulation domain.	interpretation 1.00	0.82	0.17	asserted 0.99
s8	However, we find that extending the outer boundary by only a few percent of the stellar radius significantly increases the velocity and temperature perturbations in the convection zone, the overshooting depth, the power and the spectral slope of the IGWs.	result 1.00	0.98	0.62	asserted 1.00
s9	The effect is related to the background conditions at the outer boundary, which are determined in essence by the hydrostatic stratification and the given luminosity.	interpretation 1.00	0.76	0.14	asserted 0.99

What kind of paper the classifier reports this is: simulation study 1.00 · evidence from simulation or computation 1.00.

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Original abstract

Stellar convection is a non-local process responsible for the transport of heat and chemical species. It can lead to enhanced mixing through convective overshooting and excitation of internal gravity waves (IGWs) at convective boundaries. The relationship between these processes is still not well understood and requires global hydrodynamic simulations to capture the important large-scale dynamics. The steep stratification in stellar interiors suggests that the radial extent of such simulations can affect the convection dynamics, the IGWs in the stably stratified radiative zone, and the depth of the overshooting layer. We investigate these effects using two-dimensional global simulations performed with the fully compressible stellar hydrodynamics code MUSIC. We compare eight different radial truncations of the same solar-like stellar model evolved over approximately 400 convective turnover times. We find that the location of the inner boundary has an insignificant effect on the convection dynamics, the convective overshooting and the travelling IGWs. We relate this to the background conditions at the lower convective boundary which are unaffected by the truncation, as long as a significantly deep radiative layer is included in the simulation domain. However, we find that extending the outer boundary by only a few percent of the stellar radius significantly increases the velocity and temperature perturbations in the convection zone, the overshooting depth, the power and the spectral slope of the IGWs. The effect is related to the background conditions at the outer boundary, which are determined in essence by the hydrostatic stratification and the given luminosity.

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Each citing sentence is taken from the citing paper's LaTeX source and typed by Pith's classifier. A label appears at probability 0.8 or more (0.95 for support), a contest at 0.7 or more; the quoted words are the citing authors'. How each label was checked · JSON

What it cites · 8 sentences without a confident label

Uses the method or tool of 2 papers

Specifically, we characterise the overshooting in the same way as [ref] .

Two-dimensional simulations of solar-like models with artificially enhanced luminosity -- I. Impact on convective penetration · Characteristic overshooting depth · 1.00
The initial conditions are generated with the one-dimensional Lyon stellar evolution code [ref] , using the same opacities and equation of state as implemented in .

Evolutionary models for solar metallicity low-mass stars: mass-magnitude relationships and color-magnitude diagrams · Description of the simulations. · 1.00

Compares with 1 paper

This effect is qualitatively similar to the dependence we find on $$, especially considering that the stellar models used by [ref] and in this study have significantly different background stratification and luminosity.

Two-dimensional simulations of solar-like models with artificially enhanced luminosity -- I. Impact on convective penetration · Luminosity boosting analogy · 1.00

Cites as support 1 paper

However, as demonstrated by [ref] such boosting causes significant changes in the convection dynamics, the overshooting layer and the internal gravity waves in the radiative zone.

Two-dimensional simulations of solar-like models with artificially enhanced luminosity -- I. Impact on convective penetration · Description of the simulations. · 0.97

Cites as background 2 papers

A quantity that is also often used in the literature is $F_ΔT_t, θ = ρc_p ΔT _t, θ$ [ref] , where $ΔT$ is the temperature fluctuations with respect to a reference model.

Two-dimensional simulations of solar-like models with artificially enhanced luminosity -- I. Impact on convective penetration · Characteristic overshooting depth · 0.81
It has been proposed [ref] that stellar convection is primarily driven by the `rain' of radiatively cooled (low entropy) perturbations which originate at the top convective layers and buoyantly fall towards the lower convective boundary.

Entropy Rain: Dilution and Compression of Thermals in Stratified Domains · Results: convection zone · 0.91

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