  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).
