  The helium-enriched (He-enriched) metal-rich red giants of Omega Centauri,
discovered by Hema and Pandey using the low-resolution spectra from the Vainu
Bappu Telescope (VBT) and confirmed by the analyses of the high-resolution
spectra obtained from the HRS-South African Large Telescope (SALT) for LEID
34225 and LEID 39048, are reanalysed here to determine their degree of
He-enhancement/hydrogen-deficiency (H-deficiency). The observed MgH band
combined with model atmospheres with differing He/H ratios are used for the
analyses. The He/H ratios of these two giants are determined by enforcing the
fact that the derived Mg abundances from the MgI lines and from the subordinate
lines of the MgH band must be same for the adopted model atmosphere. The
estimated He/H ratios for LEID 34225 and LEID 39048 are 0.15+/-0.04 and
0.20+/-0.04, respectively, whereas the normal He/H ratio is 0.10. Following the
same criteria for the analyses of the other two comparison stars (LEID 61067
and LEID 32169), a normal He/H ratio of 0.10 is obtained. The He/H ratio of
0.15-0.20 corresponds to a mass fraction of helium (Z(He)=Y) of about
0.375-0.445. The range of helium enhancement and the derived metallicity of the
program stars are in line with those determined for Omega Cen blue
main-sequence stars. Hence, our study provides the missing link for the
evolutionary track of the metal-rich helium-enhanced population of Omega
Centuari. This research work is the very first spectroscopic determination of
the amount of He-enhancement in the metal-rich red giants of Omega Centauri
using the MgI and MgH lines.
