5 Conclusions

• From spectroscopy obtained during superoutburst, we have found the most likely orbital period of the dwarf nova V 592 Her, viz  $85.5 \pm 0.4$ min. The $91.2 \pm 0.5$ min alias cannot be completely ruled out.

• We show that both periods, when combined with the reported superhump period and theoretical relationships, give support for the view that V 592 Her harbours a brown dwarf like secondary star.

• The detection of He II 4686 emission, makes V 592 Her a good candidate to look for spiral shocks during superoutburst.

Acknowledgements

We thanks the referee, Dr. Paula Szkody, for useful comments that helped to improve a first version of this paper. This work was supported by Grant Fondecyt 1000324 and DI UdeC 202.011.030-1.0. We are grateful to the VSNET observers and the administrators of the VSNET database for making their data available through the WEB.