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The Impact of the Transport of Chemicals and Electronic Screening on Helioseismic and Neutrino Observations in Solar Models

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Abstract

The transport of chemical elements in stellar interiors is one of the greatest sources of uncertainties of solar and stellar modelling. The Sun, with its exquisite spectroscopic, helioseismic and neutrino observations, offers a prime environment to test the prescriptions used for both microscopic and macroscopic transport processes. We study in detail the impact of various formalisms for atomic diffusion on helioseismic constraints in both CLES (Scuflaire et al. 2008a) and Cesam2k20 (Morel and Lebreton 2008; Marques et al. 2013; Deal et al. 2018) models and compare both codes in detail. Moreover, due to the inability of standard models using microscopic diffusion to reproduce light element depletion in the Sun (Li, Be), another efficient process must be included to reproduce these constraints (rotation-induced: Eggenberger et al. 2022, overshooting -or penetrative convection- below the convective envelope: Thévenin et al. 2017, or ad hoc turbulence: Lebreton and Maeder 1987; Richer, Michaud, and Turcotte 2000). However, introducing such an extra mixing leads to issues with the CNO neutrino fluxes (see Buldgen et al. 2023), which seem to be systematically lower than the Borexino observations (Appel et al. 2022). Another key aspect to consider when reconciling models with neutrino fluxes is the impact of electronic screening (Mussack and Däppen 2011).

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Data Availability

All observational data are public and accessible from the references mentioned in the text.

Code Availability

The Cesam2k20 stellar evolution code and OSM code are publicly available and can be accessed from this website: https://www.ias.u-psud.fr/cesam2k20/home.html.

Notes

  1. https://www.ias.u-psud.fr/cesam2k20/.

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Acknowledgments

We gratefully thank our anonymous referee whose comprehensive readings and remarks helped to improve the content of the manuscript.

Funding

M. D. acknowledges support from CNES, focused on PLATO. G. B. acknowledges fundings from the Fonds National de la Recherche Scientifique (FNRS) as a postdoctoral researcher. L. M. acknowledges support from the Agence Nationale de la Recherche (ANR) grant ANR-21-CE31-0018.

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Authors and Affiliations

  1. LUPM, Université de Montpellier, CNRS, Place Eugène Bataillon, 34095, Montpellier, France

    Morgan Deal

  2. STAR Institute, Université de Liège, Liège, Belgium

    Gaël Buldgen, Arlette Noels & Richard Scuflaire

  3. LIRA, Observatoire de Paris, Université PSL, Sorbonne Université, Université Paris Cité, CY Cergy Paris Université, CNRS, 92190, Meudon, France

    Louis Manchon & Yveline Lebreton

  4. IPR (Institut de Physique de Rennes) – UMR 6251, Université de Rennes, CNRS, 35000, Rennes, France

    Yveline Lebreton

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  1. Morgan Deal
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  2. Gaël Buldgen
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  3. Louis Manchon
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  4. Yveline Lebreton
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  5. Arlette Noels
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  6. Richard Scuflaire
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Contributions

M. D. proposed the idea of testing different micro- and macroscopic transport of chemical element formalisms on solar models, and G. B. proposed the idea of testing the impact of electronic screening on solar models and neutrino fluxes. The idea of comparing CLES and Cesam2k20 in this context was decided by all co-authors. CLES models were computed by G. B., A. N., and R. S., and Cesam2k20 models were computed by M. D., L. M., and Y. L. The comparison of internal structures and evolution of surface abundances was performed by M. D. and inversions were performed by G. B. All co-authors contributed to the interpretation of the results and were involved in the discussions.

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Correspondence to Morgan Deal.

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Deal, M., Buldgen, G., Manchon, L. et al. The Impact of the Transport of Chemicals and Electronic Screening on Helioseismic and Neutrino Observations in Solar Models. Sol Phys 300, 96 (2025). https://doi.org/10.1007/s11207-025-02512-1

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