Forum Springer Astron. Astrophys.
Forum Whats New Search Orders

Astron. Astrophys. 357, 677-680 (2000)

Table of Contents
Available formats: HTML | PDF | (gzipped) PostScript

AM Herculis star EV UMa (RE 1307+535) in a high accretion state

S. Katajainen  *  1, H.J. Lehto 1,2, V. Piirola 1, H. Karttunen 1 and J. Piironen 3

1 Tuorla Observatory, Väisäläntie 20, 21500 Piikkiö, Finland
2 Department of Physics, 21400, Turku University, Finland
3 Observatory, P.O. Box 14, 00014 University of Helsinki, Finland

Received 10 March 2000 / Accepted 14 March 2000


We present results of the first simultaneous UBVRI-photopolarimetry of the AM Herculis system EV UMa (RE 1307+535), carried out in February 1999. EV UMa is known to have a large variation in circular polarization (-20% to +50%) in the R-band. It has an orbital period close to the theoretical lower limit for magnetic CVs. During our observations EV UMa was in a very high accretion state, (15.7 [FORMULA] V [FORMULA] 17.2), which was about two magnitudes brighter than during our earlier (1994) high state observations (17.8 [FORMULA] V [FORMULA] 18.8). Dramatic changes have occured in the circular polarization curves compared to earlier observations, in particular the positive circular polarization is now reduced almost by factor of ten. Circular polarization varied during our observations from -23% to +5% in the U-band, from -15% to +6% in the B-, V-, and I-bands, and from -12% to 7% in the R-band. An eclipse-like feature is seen in the optical light curves between the orbital phases [FORMULA] and [FORMULA]. The presence of an eclipse and the reduction in the positive circular polarization during the same phase interval could be due to effects caused by the accretion stream. Our observations show that the accretion rate has increased and the accretion geometry has changed in EV UMa since our previous observations. We have calculated an improved ephemeris for EV UMa, based on the negative circular polarization maxima observed in 1994 and 1999. The new value for the white dwarf spin period is 0.05533887(2) days.

Key words: stars: magnetic fields – stars: novae, cataclysmic variables – accretion, accretion disks – stars: binaries: close – polarization

* Based on observations made with the Nordic Optical Telescope, operated on the island of La Palma jointly by Denmark, Finland, Iceland, Norway, and Sweden, in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofísica de Canarias.

Send offprint requests to: S. Katajainen (sekataja@astro.utu.fi)

© European Southern Observatory (ESO) 2000

Online publication: June 5, 2000