On the orbital period of the magnetic cataclysmic variable HS 0922+1333
Observatorio Astrónomico Nacional SPM, Instituto de Astronomía, Universidad Nacional Autónoma de México, Ensenada, BC, México (PO Box 439027, San Diego, CA, 92143-9024, USA.) e-mail: [gag;zhar]@astrosen.unam.mx
Accepted: 18 March 2007
Context.The object HS 0922+1333 was visited briefly in 2002 in a mini survey of low accretion rate polars (LARPs) in order to test if they undergo high luminosity states similar to ordinary polars. On the basis of that short observation the suspicion arose that the object might be an asynchronous polar (Tovmassian et al. 2004). The disparity between the presumed orbital and spin period appeared to be quite unusual.
Aims.We performed follow-up observations of the object to resolve the problem.
Methods.New simultaneous spectroscopic and photometric observations spanning several years allowed measurements of radial velocities of emission and absorption lines from the secondary star and brightness variations due to synchrotron emission from the primary.
Results.New observations show that the object is actually synchronous and its orbital and spin period are equal to 4.04 h.
Conclusions. We identify the source of confusion of previous observations to be a high velocity component of emission line arousing from the stream of matter leaving L1 point.
Key words: binaries: close / binaries: spectroscopic / novae, cataclysmic variables / white dwarfs / magnetic fields / stars: individual: HS 0922+1333
© ESO, 2007