On the orbital period of the cataclysmic variable V592 Herculis
Astrophysics
2009-11-07 v1
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.
Cite
@article{arxiv.astro-ph/0209038,
title = {On the orbital period of the cataclysmic variable V592 Herculis},
author = {R. E. Mennickent and C. Tappert and R. Gallardo and H. W. Duerbeck and T. Augusteijn},
journal= {arXiv preprint arXiv:astro-ph/0209038},
year = {2009}
}
Comments
4 pages, 5 figures, accepted for publication in Astronomy and Astrophysics