A recent study by the Indian Institute of Astrophysics has made significant progress in estimating the abundance of Helium in the Sun's photosphere. Traditionally, estimating Helium levels in stars like the Sun has been challenging due to the absence of observable spectral lines from the photosphere. Using a novel technique, the researchers at IIA analyzed Magnesium and Carbon features in the Sun's spectrum to accurately calculate the Helium abundance. By modeling the lines of neutral Magnesium and Carbon atoms along with hydrogenated molecules, they were able to determine the relative abundance of Helium. This breakthrough challenges previous indirect estimation methods and provides a more reliable measurement of solar composition. The study confirmed a Helium to Hydrogen ratio of 0.1, aligning with established helioseismological studies and enhancing our understanding of the Sun's opacity. The findings offer insights into stellar composition analysis and could have implications for advancing research in solar physics and astronomy.