On the orbital period of the cataclysmic variable V592 Herculis
arXiv:astro-ph/0209038 · doi:10.1051/0004-6361:20021278
Abstract
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.
4 pages, 5 figures, accepted for publication in Astronomy and Astrophysics
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