Volume 439, Number 3, September I 2005
|Page(s)||1131 - 1134|
|Section||Stellar structure and evolution|
|Published online||12 August 2005|
X-ray outburst of 4U 0115+634 and ROTSE observations of its optical counterpart V635 Cas
Physics Department, Middle East Technical University, Ankara 06531, Turkey e-mail: firstname.lastname@example.org
2 Department of Electrical and Electronics Engineering, Başkent University, 06530 Ankara, Turkey e-mail: email@example.com
Accepted: 1 June 2005
ROTSE IIId (The Robotic Optical Transient Experiment) observations of the X-ray binary system 4U 0115+634/V635 Cas obtained during 2004 June and 2005 January make it possible, for the first time, to study the correlation between optical and type II X-ray outbursts. The X-ray outburst sharply enhanced after periastron passage where the optical brightness was reduced by 0.3 mag for a few days. We interpret the sharp reduction of optical brightness as a sign of mass ejection from the outer parts of the disc of the Be star. After this sharp decrease, the optical brightness rose again and reached the pre-X-ray outburst level. Afterwards, a gradual decrease of the optical brightness followed until a minimum then a gradual increase started again. Qualitatively, the change of the optical lightcurve suggests a precession of the Be star disc of around a few hundred days. We also investigate the periodic signatures from the archival RXTE-ASM (Rossi X-ray Timing Explorer – All Sky Monitor) light curve covering a time span of ∼9 years. We find significant orbital modulation in the ASM light curve during the type I X-ray outburst.
Key words: stars: binaries: close / stars: pulsars: general / stars: emission line, Be / stars: individual: 4U 0115+634, V635 Cas / X-rays: stars
© ESO, 2005
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