X-ray and optical periodicities in X-ray binaries. I.A0535+26

Abstract

A homogeneous set of UBV photometry (354 data points obtained between 1983 and 1998) for the Be/X-ray binary A0535+26 = V725Tau is analysed, aiming to look for possible periodic component(s). After subtraction of the long-term variation it was found that only a 103-day periodic component remains in the power spectra in both the V and B colour bands. The probability of chance occurrence of such a peak is less than 0.1%. There are no signs of optical variability at the X-ray period (111 d). We discuss possible reasons for a 103-day modulation and suggest that it corresponds to a beat frequency of the orbital period of the neutron star and the precession period (~1400 d) either of an accretion disc around the neutron star or a warped decretion disc around the Be star.

LaTeX, 6 pages, 5 figures, uses psfig.sty

References in corpus (2)

• The Be/X-ray transient 4U 0115+63/V635 Cas I. A consistent model
• The Be/X-ray transient 4U 0115+63/V635 Cas: II. Outburst mechanisms

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• Cyclical behaviour and disc truncation in the Be/X-ray binary A0535+26
• X-ray properties of the transient pulsar 3A 0535+262 in quiescence
• Long-term variability of high-mass X-ray binaries. I.Photometry
• Studies of the Be star X Persei during a bright infrared phase
• High-dispersion spectroscopic monitoring of the Be/X-ray binary A0535+26/V725 Tau I: The long-term profile variability