Abstract
Helioseismology and solar modelling have enjoyed a golden era thanks to decades-long surveys from ground-based networks such as for example GONG, BiSON, IRIS and the SOHO and SDO space missions which have provided high-quality helioseismic observations that supplemented photometric, gravitational, size and shape, limb-darkening and spectroscopic constraints as well as measurements of neutrino fluxes. However, the success of solar models is also deeply rooted in progress in fundamental physics (equation of state of the solar plasma, high-quality atomic physics computations and opacities, description of convection and the role of macroscopic transport processes of angular momentum and chemicals, such as for example meridional circulation, internal gravity waves, shear-induced turbulence or even convection. In this paper, we briefly outline some key areas of research that deserve particular attention in solar modelling. We discuss the current uncertainties that need to be addressed, how these limit our predictions from solar models and their impact on stellar evolution in general. We outline potential strategies to mitigate them and how multidisciplinary approaches will be needed in the future to tackle them.
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References
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Acknowledgements
We thank the referee for their careful reading of the manuscript and their constructive suggestions. We thank D. Chari for providing Figure 2. We thank Dr. A.M. Amarsi for the fruitful discussions associated with the spectroscopic determinations of the solar abundances. We acknowledge support by the ISSI team “Probing the core of the Sun and the stars” (ID 423) led by Thierry Appourchaux.
Funding
GB acknowledges fundings from the Fonds National de la Recherche Scientifique (FNRS) as a postdoctoral researcher. GC acknowledges funds from the Knut and Alice Wallenberg Foundation. RT acknowledges support from NASA grants 80NSSC20K0543 and 80NSSC-22K0829. The study by V.A.B., A.V.O , and S.V.A. is conducted under the state assignment of Lomonosov Moscow State University. R.A.G. acknowledges the support from the GOLF and PLATO Centre National D’Études Spatiales grants. J.B. acknowledges funding from the SNF Postdoc.Mobility grant no. P\(\rm 500PT\_222217\) (Impact of magnetic activity on the characterization of FGKM main-sequence host-stars). M.K. was supported by the JSPS KAKENHI (grant nos. 24K00654 and 24K07099). AP acknowledges partial support from US National Science Foundation (Astronomy). Los Alamos National Laboratory is operated by Triad National Security, LLC, for the National Nuclear Security Administration of US Department of Energy (Contract No. 89233218NCA000001). This research has made use of the Astrophysics Data System, funded by NASA under Cooperative Agreement 80NSSC21M00561.
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G.B. initiated, designed and coordinated the project and took care of most of the writing. G.C., V.A.B, R.T., A.L.S, A.P., J.C.P., A.O.V., M.K., T.A., R.A.G., M.D., N.G. took part in the writing of their respective section of expertise. J.C.D., A.N., T.G.,D.N., J.B., C.B., J.C., P.C., C.J.F., L.P. and C.P. provided comments on the content of the manuscript.
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Buldgen, G., Canocchi, G., Le Saux, A. et al. The Future of Solar Modelling: Requirements for a New Generation of Solar Models. Sol Phys 300, 97 (2025). https://doi.org/10.1007/s11207-025-02508-x
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DOI: https://doi.org/10.1007/s11207-025-02508-x