Rotating Solar Models in Agreement with Helioseismic Results and Updated Neutrino Fluxes

TL;DR

This study develops rotating solar models incorporating new low-metal abundances, enhanced diffusion, and convection overshoot, achieving better agreement with helioseismic data and neutrino flux measurements than previous models.

Contribution

It introduces rotating solar models with updated low-metal abundances that align well with helioseismic and neutrino observational constraints, improving upon prior non-rotating models.

Findings

Rotating models match observed sound-speed and density profiles.

Models reproduce the depth and helium abundance of the convection zone within 1σ.

Neutrino flux predictions agree with Borexino measurements within 1σ.

Abstract

Standard solar models (SSMs) constructed in accordance with old solar abundances are in reasonable agreement with seismically inferred results, but SSMs with new low-metal abundances disagree with the seismically inferred results. The constraints of neutrino fluxes on solar models exist in parallel with those of helioseismic results. The solar neutrino fluxes were updated by Borexino Collaboration. We constructed rotating solar models with new low-metal abundances where the effects of enhanced diffusion and convection overshoot were included. A rotating model using OPAL opacities and the Caffau abundance scale has better sound-speed and density profiles than the SSM with the old solar abundances and reproduces the observed $p$-mode frequency ratios $r_{02}$ and $r_{13}$. The depth and helium abundance of the convection zone of the model agree with the seismically inferred ones at the level of $1\sigma$. The updated neutrino fluxes are also reproduced by the model at the level of $1\sigma$. The effects of rotation and enhanced diffusion not only improve the model's sound-speed and density profiles but bring the neutrino fluxes predicted by the model into agreement with the detected ones. Moreover, the calculations show that OP may underestimate opacities for the regions of the Sun with $T\gtrsim5\times10^{6}$ K by around $1.5\%$, while OPAL may underestimate opacities for the regions of the Sun with $2\times10^{6}$ K $\lesssim T \lesssim 5\times10^{6}$ K by about $1-2\%$.