Abstract:
Long period light variations of the cataclysmic variables PG 1711+336 (V795 Her) were first noticed by Mironov et al. (1983 a,b) who reported a photometric period of 0.115883 day for the system. Baidak et al., (1985) improved the ephemer is and refined the period to 0.114488 day (2.75 hour). If this period is interpreted as the orbital period, then the system is unique in that its orbital period falls within the period gap in the distribution of cataclysmic variables versus their orbital periods.
