31 UV spectra obtained with tne LWR camera of the lUE satellite in the period 1978-83 were analysed. Changes of Mg II h and k emissions are evident but there is no evident correlation between emission intensity of Mg II and orbital or photometric phase. Using three various methods of analysis of possible periodicity in variation of Mg II h and k emission intensities we have found reál chanes in
h + k fluxes with period equal to the half of the orbital one, 0.5 Porb = 10.2606. We interpret this effect as evidence of direct influence of tidal inxeraction of secondary component on the chromospheric structure of the primary. Evident minimum of the Mg II h and k intensity is observed when the tides are on the line of sight and maximum when both tidal bulges are visible. Difference between maximum and minimum of total flux of k line is equal to about 20%, while the shape of the profile is practically unchanged.