Abstract

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 find a most 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.