On the orbital period of the cataclysmic variable V 592 Herculis

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 Hα emission line we find a most likely orbital period of $85.5 \pm 0.4$ min, but the $91.2 \pm...

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Bibliographic Details
Published in:Astronomy and astrophysics (Berlin) 2002-11, Vol.395 (2), p.557-561
Main Authors: Mennickent, R. E., Tappert, C., Gallardo, R., Duerbeck, H. W., Augusteijn, T.
Format: Article
Language:English
Subjects:
binaries: general
cataclysmic variables
stars: evolution
stars: fundamental parameters
stars: individual: V 592 Her
stars: novae
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Summary: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 Hα emission line we find a most likely orbital period of $85.5 \pm 0.4$ min, but the $91.2 \pm 0.6$ 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.
ISSN:0004-6361
1432-0746
DOI:10.1051/0004-6361:20021278