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Conventionally, the helium-to-hydrogen ratio for the stars are adopted to be0.1, as standard, unless, the stars are severely deficient in hydrogen like inRCB-class, or the stars' helium abundance is accurately measured using He Itransitions in warm/hotter stars. In our study, the small change inhelium-to-hydrogen ratio (from standard value, 0.1) in normal giants weredetected from the large difference (> 0.3 dex) in the Mg-abundance measuredfrom Mg I lines and the subordinate lines of (0,0) MgH band. These are thestars that are mildly hydrogen-deficient/He-enhanced. Such stars werespectroscopically discovered for the first time among giants of the globularcluster Omega Centauri. The sample selection, observations, methodology andresults are discussed in detail.

Measuring Hydrogen-to-Helium Ratio in Cool Stars