  We present a spectroscopic study of the long-recurrence-time dwarf nova V592
Herculis based on observations obtained during its August 1998 superoutburst.
  From the analysis of the radial velocities of the Halpha emission line we
find a most likely orbital period of 85.5 +- 0.4 minutes, but the 91.2 +- 0.6
minutes alias cannot be completely discarded. Both periods imply a very small
period excess and supports the brown-dwarf like nature of the secondary star.
