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

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 )...

Full description

Saved in:
Bibliographic Details
Published in:The Astrophysical journal 2024-07, Vol.970 (1), p.38
Main Authors: Yang, Wuming, Tian, Zhijia
Format: Article
Language:English
Subjects:
Abundance
Astronomical models
Convection
Density
Diffusion rate
Enhanced diffusion
Fluxes
Helioseismology
Helium
Neutrinos
Nuclear reaction cross sections
Nuclear reactions
Photosphere
Solar abundances
Solar interior
Solar models
Solar neutrinos
Solar rotation
Citations: Items that this one cites
Online Access:Get full text
Tags: Add Tag
No Tags, Be the first to tag this record!
Description
Summary: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 under 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 the 1 σ level. Furthermore, the calculated neutrino fluxes from these models agree with detected ones at the level of 1 σ . 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.
ISSN:0004-637X
1538-4357
DOI:10.3847/1538-4357/ad4d87