We report on a three year spectroscopic monitoring program of the H \alpha emission in the massive X-ray binary LS I +65 010 = 2S 0114+650 , which consists of a B-supergiant and a slowly rotating X-ray pulsar .
We present revised orbital elements that yield a period of P = 11.5983 \pm 0.0006 d and confirm that the orbit has a non-zero eccentricity e = 0.18 \pm 0.05 .
The H \alpha emission profile is formed in the base of the wind of the B-supergiant primary , and we show how this spectral feature varies on timescales that are probably related to the rotational period of the B-supergiant .
We also examine the X-ray fluxes from the Rossi X-ray Timing Explorer All-Sky Monitor instrument , and we show that the X-ray orbital light curve has a maximum at periastron and a minimum at the inferior conjunction of the B-supergiant .
We also show that the wind emission strength and the high energy X-ray flux appear to vary in tandem on timescales of approximately a year .