  16 Cyg A and B are among the brightest stars observed by Kepler. What makes
these stars more interesting is that they are solar analogs. 16 Cyg A and B
exhibit solar-like oscillations. In this work we use oscillation frequencies
obtained using 2.5 years of Kepler data to determine the current helium
abundance of these stars. For this we use the fact that the helium ionization
zone leaves a signature on the oscillation frequencies and that this signature
can be calibrated to determine the helium abundance of that layer. By
calibrating the signature of the helium ionization zone against models of known
helium abundance, the helium abundance in the envelope of 16 Cyg A is found to
lie in the range 0.231 to 0.251 and that of 16 Cyg B lies in the range 0.218 to
0.266.
