We present the optical spectroscopic study of two Classical Be stars , 59 Cyg and OT Gem obtained over a period of few months in 2009 .
We detected a rare triple-peak H \alpha emission phase in 59 Cyg and a rapid decrease in the emission strength of H \alpha in OT Gem , which are used to understand their circumstellar disks .
We find that 59 Cyg is likely to be rapid rotator , rotating at a fractional critical rotation of \sim 0.80 .
The radius of the H \alpha emission region for 59 Cyg is estimated to be R _ { d } / R _ { * } \sim 10.0 , assuming a Keplerian disk , suggesting that it has a large disk .
We classify stars which have shown triple-peaks into two groups and find that the triple-peak emission in 59 Cyg is similar to \zeta Tau .
OT Gem is found to have a fractional critical rotation of \sim 0.30 , suggesting that it is either a slow rotator or viewed in low inclination .
In OT Gem , we observed a large reduction in the radius of the H \alpha emission region from \sim 6.9 to \sim 1.7 in a period of three months , along with the reduction in the emission strength .
Our observations suggest that the disk is lost from outside to inside during this disk loss phase in OT Gem .