On the orbital period of the cataclysmic variable V 592 Herculis

We present a spectroscopic study of the long-recurrence-time dwarf nova V 592 Herculis based on observations obtained during its August 1998 superoutburst. From the analysis of the radial velocities of the H emission line we fi nd am ost likely orbital period of 85:5 0:4 min, but the 91:2 0:6 min alias cannot be completely discarded. Both periods imply a very small period excess and supports the brown-dwarf like nature of the secondary star.