New Solar Composition: The Problem With Solar Models Revisited

TL;DR

The paper investigates the solar abundance problem by constructing standard solar models using three abundance sets—GS98, AGS05, and AGSS09—with updated physics and assessing their consistency with helioseismic constraints and solar neutrino fluxes. It finds that AGSS09 partially alleviates, but does not eliminate, the discrepancies with helioseismology (e.g., $R_{ m CZ}=0.724\,R_\odot$ and $Y_{ m surf}=0.231$ versus $0.713\pm0.001\,R_\odot$ and $0.2485\pm0.0035$), and quantifies that an opacity increase of about $12$–$15\%$ at the base of the convective zone would be needed to restore agreement, tapering toward the core. Neutrino fluxes are affected, with notable increases in the $^{13}$N and $^{15}$O channels due to higher C and N abundances. The results underscore a persistent solar abundance problem and provide quantitative guidance for opacity studies and interior solar physics.

Abstract

We construct updated solar models with different sets of solar abundances, including the most recent determinations by Asplund et al. (2009). The latter work predicts a larger ($\sim 10%$) solar metallicity compared to previous measurements by the same authors but significantly lower ($\sim 25%$) than the recommended value from a decade ago by Grevesse & Sauval (1998). We compare the results of our models with determinations of the solar structure inferred through helioseismology measurements. The model that uses the most recent solar abundance determinations predicts the base of the solar convective envelope to be located at $R_{\rm CZ}= 0.724{\rm R_\odot}$ and a surface helium mass fraction of $Y_{\rm surf}=0.231$. These results are in conflict with helioseismology data ($R_{\rm CZ}= 0.713\pm0.001{\rm R_\odot}$ and $Y_{\rm surf}=0.2485\pm0.0035$) at 5$-σ$ and 11$-σ$ levels respectively. Using the new solar abundances, we calculate the magnitude by which radiative opacities should be modified in order to restore agreement with helioseismology. We find that a maximum change of $\sim 15%$ at the base of the convective zone is required with a smooth decrease towards the core, where the change needed is $\sim 5%$. The required change at the base of the convective envelope is about half the value estimated previously. We also present the solar neutrino fluxes predicted by the new models. The most important changes brought about by the new solar abundances are the increase by $\sim 10%$ in the predicted $^{13}$N and $^{15}$O fluxes that arise mostly due to the increase in the C and N abundances in the newly determined solar composition.

Figures (2)

• Figure 1: Relative sound speed $\delta c/c$ and density $\delta \rho / \rho$ differences, in the sense (Sun - Model)/Model, between solar models and helioseismological results. Details on the inversion procedure and data used, as well as the reference sound speeds and densities are given in bisoniii.
• Figure 2: Separation ratios. Comparison between values determined from BiSON data and the solar models presented in this work.