Volume 445, Number 3, January III 2006
|Page(s)||1037 - 1040|
|Section||Stellar structure and evolution|
|Published online||03 January 2006|
RX J2133.7+5107: identification of a new long period Intermediate Polar
Service d'Astrophysique, DSM/DAPNIA/SAp, CE Saclay, 91191 Gif-sur-Yvette Cedex, France e-mail: firstname.lastname@example.org
2 LUTH (CNRS-UMR 8102), Observatoire de Paris, Section de Meudon, 92195 Meudon Cedex, France
3 APC (CNRS-UMR 7164), Université Denis Diderot, 2 place Jussieu, 75005 Paris, France e-mail: email@example.com
4 INAF - Osservatorio Astronomico di Capodimonte, Via Moiariello 16, 80131 Napoli, Italy e-mail: firstname.lastname@example.org
5 Observatoire Astronomique de Strasbourg, 67000 Strasbourg, France e-mail: email@example.com
Accepted: 20 July 2005
We report the first time-resolved photometric and spectroscopic optical observations of the X-ray source RX J2133.7+5107, identified in the ROSAT survey. A clear persistent optical light pulsation is discovered with fast photometry at a period of s which we associate with the spin period of an accreting white dwarf. Radial velocity curves of the strong emission lines show modulation with a period of h, identified as the orbital period. These observations establish that the source is a member of the intermediate polar class (IPs) of magnetic cataclysmic variables. With only 4 IPs with longer orbital periods, RX J2133.7+5107 is among the widest systems. It is a unique IP with an orbital period in the middle of the so-called (6-10) h IP gap and it shows a significant degree of asynchronism with a ratio / of 0.02. When attributed to the motion of the white dwarf, the emission lines orbital modulation yields a mass function of which, for a probable inclination and a white dwarf mass , corresponds to a secondary mass .
Key words: stars: binaries: general / stars: individual: RX J2133.7+5107 / stars: novae, cataclysmic variables / accretion, accretion disks / stars: variables: general / white dwarfs
© ESO, 2006
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