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The Sun is the most studied and well-known star, and as such, solarfundamental parameters are often used to bridge gaps in the knowledge of otherstars, when these are required for modelling. However, the two most powerfuland precise independent methodologies currently available to infer the internalsolar structure are in disagreement. We aim to show the potential impact ofcomposition choices in the overall evolution of a star, using the Sun as anexample. To this effect, we create two Standard Solar Models and a comparisonmodel using different combinations of metallicity and relative elementabundances and compare evolutionary, helioseismic, and neutrino-relatedproperties for each. We report differences in age for models calibrated to thesame point in the HR diagram, in the red giant branch, of more than 1 Gyr, andfound that the current precision level of asteroseismic measurements is enoughto differentiate these models, which would exhibit differences in priod spacingof 1.30-2.58 per cent. Additionally, we show that the measurement of neutrinofluxes from the carbon-nitrogen-oxygen cycle with a precision of around 17 percent, which could be achieved by the next generation of solar neutrinoexperiments, could help resolve the stellar abundance problem.

The impact of composition choices on solar evolution: age, helio- and asteroseismology, and neutrinos