Helium Abundance of the Sun: A Spectroscopic Analysis

TL;DR

This paper presents a spectroscopic method to determine the helium abundance in the Sun by analyzing various atomic and molecular lines, providing a crucial reference for understanding helium content in cool stars.

Contribution

It introduces a novel spectroscopic approach combining multiple lines and model atmospheres to accurately estimate the Sun's helium abundance, addressing a key gap in stellar astrophysics.

Findings

Helium abundance in the Sun is estimated as He/H = 0.091 (+0.019/-0.014).

Derived solar mass fractions are X=0.7232, Y=0.2633, Z=0.0135.

The method provides a reference point for helium ratios in cool stars.

Abstract

Determining the He/H ratio in cool stars presents a fundamental astrophysical challenge. While this ratio is established for hot O and B stars, its extrapolation to cool stars remains uncertain due to the absence of helium lines in their observed spectra. We address this knowledge gap by focusing on the Sun as a representative cool star. We conduct spectroscopic analyses of the observed solar photospheric lines by utilizing a combination of MgH molecular lines and neutral Mg atomic lines including yet another combination of CH and C_2 molecular lines with neutral C atomic lines. Our spectroscopic analyses were further exploited by adopting solar model atmospheres constructed for distinct He/H ratios to determine the solar photospheric helium abundance. The helium abundance is determined by enforcing the fact that for an adopted model atmosphere with an appropriate He/H ratio, the derived Mg abundance from the neutral Mg atomic lines and that from the MgH molecular lines must be the same. Ditto holds for the C abundance derived from neutral C atomic lines and that from CH lines of the CH molecular band and C_2 lines from the C_2 Swan band. The estimated He/H ratio for the Sun is discussed based on the one-dimensional local thermodynamic equilibrium (1D LTE) model atmosphere. The helium abundance (He/H = 0.091(+0.019/+0.014)) obtained for the Sun serves as a critical reference point to characterize the He/H ratio of cool stars across the range in their effective temperature. Using this derived He/H ratio, the solar mass fractions are determined to be X_sun=0.7232(+0.0305/-0.0377), Y_sun=0.2633(+0.0384/-0.0311), and Z_sun=0.0135(+0.0006/-0.0007).