Solar Models and Astrophysical S-factors Constrained by Helioseismic Results and Updated Neutrino Fluxes

TL;DR

This study uses helioseismic data and neutrino flux measurements to refine solar models, constraining astrophysical S-factors and addressing the solar abundance problem with improved accuracy.

Contribution

It introduces rotating solar models with various abundance scales, demonstrating that models based on Magg's abundance scale better match helioseismic and neutrino observations, and proposes a diagnostic method for S-factors.

Findings

Models with Magg's abundance scale outperform others in sound-speed profiles.

Neutrino fluxes from the models agree within 1σ with observations.

The diagnostic approach suggests S11 may be underestimated by 2%, S33 overestimated by 3%.

Abstract

The ratio of metal abundance to hydrogen abundance of the solar photosphere, $(Z/X)_{s}$, has been revised several times. Standard solar models, based on these revised solar abundances, are in disagreement with seismically inferred results. Recently, Magg et al. introduced a new value for $(Z/X)_{s}$, which is still in debate in the community. The solar abundance problem or solar modeling problem remains a topic of ongoing debate. We constructed rotating solar models in accordance with various abundance scales where the effects of convection overshoot and enhanced diffusion were included. Among these models, those utilizing Magg's abundance scale exhibit superior sound-speed and density profiles compared to models using other abundance scales. Additionally, they reproduce the observed frequency separation ratios $r_{02}$ and $r_{13}$. These models also match the seismically inferred surface helium abundance and convection zone depth within $1\sigma$ level. Furthermore, the calculated neutrino fluxes from these models agree with detected ones at the level of $1\sigma$. We found that neutrino fluxes and density profile are influenced by nuclear reactions, allowing us to use the combination of detected neutrino fluxes and seismically inferred density for diagnosing astrophysical $S$-factors. This diagnostic approach shows that $S_{11}$ may be underestimated by $2\%$, while $S_{33}$ may be overestimated by about $3\%$ in previous determinations. The $S$-factors favored by updated neutrino fluxes and helioseismic results can lead to significant improvements in solar models.