Photometric and Spectral Study of the Be/X-Ray Binary Object V725 Tau=A0535+262

• Published in: Astrophysics 2020-09, Vol.63 (3), p.367-375
• Main Authors: Kondratyeva, L. N., Denissyuk, E. K., Reva, I. V., Krugov, M. A., Aimanova, G. K., Kusakin, A. V., Omar, B. K.
• Format: Article
• Language: English
• Subjects: Analysis; Astronomical photometry; Astronomical research; Astronomical spectroscopy; Astronomy; Astrophysics; Astrophysics and Astroparticles; Astrophysics and Cosmology; Brightness; Emission; Emission lines; Emissions; Fluxes; Giant stars; H alpha line; Methods; Observations; Observations and Techniques; Outbursts; Photometric observations; Photometry; Physics; Physics and Astronomy; Pulsars; Space Exploration and Astronautics; Space Sciences (including Extraterrestrial Physics; Spectra; Spectral classification; Stars, Double; Stellar oscillations; X ray binaries; X ray stars; X-ray astronomy
• ISSN: 0571-7256; 1573-8191
• DOI: 10.1007/s10511-020-09642-3

This is a study of spectral and photometric observations of the binary system with an X-ray component V725 Tauri=A0535+262. It consists of a giant star HDE 245770 of spectral class O9.7 and the pulsar A0535+26 with a pulsation period of ~103 s. Active stages of this object, accompanied by “giant” X-ray outbursts, have been observed repeatedly. The last events occurred during 2009-2011. Our studies in 2017-2020 yielded the following data: over the last three years the B and V band brightness of the object has remained at a high level and began to decrease at the end of 2019. Here, beginning in 2016 a gradual increase in the radiative fluxes in the Hβ and Hα emission lines has been observed. At present the equivalent widths of these lines exceed the values recorded during the time of the gigan X-ray outburst of 2011. Previous studies have shown that a similar combination of the characteristics of this object, specifically an increase in emission line fluxes as the brightness decreases. is detected just before the onset of an active stage.