We present high resolution spectroscopic observations of the massive X-ray binary system LS I+65 010=2S 0114+650 in the optical wavelength region .
A correlation between equivalent width and radial velocity of photospheric absorption lines is found .
The systemic velocity , inferred from the weaker lines is v _ { helio } - 31 \pm 5 km s ^ { -1 } , which , if attributed solely to the Galactic rotation curve , implies that LS I + 65 010 lies within 3 kpc from the Sun .
The ISM Na I D lines display 2 resolved high velocity components at v _ { helio } - 70 , - 48 km s ^ { -1 } , possibly associated with gas surrounding the binary system , in addition to the - 24 - 8 km s ^ { -1 } ISM features due to the Orion and in the Perseus arm regions .
Strong photospheric line profile variability is present on a night to night timescale , with He I 5875 Å displaying an additional blue-shifted absorption in some of the spectra , similar to what is observed in the optical counterpart of Vela X-1 .
A connection between the extended blue wing and X-ray maximum is suggested .
Short timescale variations in line profiles are detected on only two nights , but the evidence that these variations occur on the 2.78 hour X-ray flaring period is marginal .