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The ex-nova RR Pic presents a periodic hump in its light curve which isconsidered to refer to its orbital period. Analyzing all available epochs ofthese hump maxima in the literature, and combining them with those from newlight curves obtained in 2013 and 2014, we establish an unique cycle countscheme valid during the past 50 years, and derive an ephemeris with the orbitalperiod 0.145025959(15) days. The O - C diagram of this linear ephemeris revealssystematic deviations which could have different causes. One of them could be alight-travel-time effect caused by the presence of a hypothetical third bodynear the star/brown dwarf mass limit, with an orbital period of the order of 70years. We also examine the difficulty of the problematic of detectingsub-stellar or planetary companions of close red-dwarf white-dwarf binaries(including cataclysmic variables), and discuss other possible mechanismsresponsible for the observed deviations in O - C. For RR Pic, we proposestrategies in order to solve this question by new observations.

The orbital ephemeris of the classical nova RR Pictoris: presence of a third body?