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

Kondratyeva, L. N.; Denissyuk, E. K.; Reva, I.; Krugov, M.; Aimanova, G. K.; Kusakin, A.; Omar, Banaz

doi:10.1007/s10511-020-09642-3

Cited by 1 publication

(8 citation statements)

References 9 publications

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“…Furthermore, Camero-Arranz et al (2012) and Yan et al (2012) found that the optical V-band light curve of 1A 0535+262 indicated that each giant X-ray outburst occurred during a phase of decreased optical brightness, while the Hα lines showed a strong emission. Kondratyeva et al (2020) observd the same phenomenon as Camero-Arranz et al (2012) and Yan et al (2012), and predicted the occurrence of the X-ray giant outburst in 2020. Taranova & Shenavrin (2017) found that the IR brightness and color minima of 1A 0535+262/V725 Tau in 2003-2011 coincided with episodes of activity of the X-ray component of the binary.…”

Section: Introductionmentioning

confidence: 62%

“…For 1A 0535+262, the long-term variabilities of optical/infrared photometry and optical spectral can be found in previous publications from 2010 to 2020 (Yan et al 2012;Camero-Arranz et al 2012;Moritani et al 2013;Taranova & Shenavrin 2017;Kondratyeva et al 2020). Camero-Arranz et al (2012) and Yan et al (2012) found an anti-correlation between the equivalent widths of the Hα lines (hereafter EW(Hα)) and the V magnitudes around the giant outburst.…”

Section: Introductionmentioning

confidence: 77%

“…1. The spectrum datum on February 20, 2020, plotted with our label is from Kondratyeva et al (2020).…”

Section: Optical Spectroscopymentioning

confidence: 99%

“…The data from AAVSO, ASAS-SN, INTEGRAL-OMC, and this work are separately labeled with cyan upward-pointing triangles, blue leftward-pointing triangles, black pixels, and red points, respectively. In addition, the optical photometric data from Kondratyeva et al (2020), Camero-Arranz et al (2012 are labeled with green crosses and purple crosses, respectively. Fifth panel: long-term light curves of NEOWISE infrared magnitudes at 3.4 µm and 4.6 µm.…”

Section: Optical Photometrymentioning

confidence: 99%

“…Our data are labeled with red points. The data from Kondratyeva et al (2020), Stoyanov & Zamanov (2016), Moritani et al (2013), Camero-Arranz et al (2012 are labeled with green crosses, blue crosses, cyan stars, and purple downward-pointing triangles, respectively. Seventh panel: evolution of (B − V) color index.…”

Section: Optical Photometrymentioning

confidence: 99%

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Multiwavelength observation of 1A 0535+262=HD 245770 from 2010 to 2021

Liu,

Yan,

Xiao

et al. 2023

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Context. 1A 0535+262 is a high-mass X-ray binary that went into a giant X-ray outburst in 2020. During this event, the X-ray luminosity reached the highest value measured over the last 30 years. Aims. Our aim is to study the long-term variability of 1A 0535+262 before and after the 2020 major X-ray outburst and to uncover the mechanism that led to the X-ray outburst. Methods. We used the long-term photometric light curve and the equivalent widths of the Hα and He I λ6678 lines to monitor the state of the Be star’s circumstellar disk. The Hα line profiles show evidence for V/R variability, which we revealed by fitting the Hα spectral line profiles with two Gaussian functions. In addition, we divided our data into four periods according to the intensity of the X-ray, optical, and infrared emission. Results. The Hα line profiles show single-peaked profiles in most cases. This is consistent with the previously reported orbital inclination of i = 37° ±2°. Unlike the Hα lines, the He I λ6678 lines show a maximal intensity in October 2020, which is one month before the giant X-ray outburst in 2020. Based on the behavior of the equivalent widths of the Hα and He I λ6678 lines, and the V-band magnitude, we find two mass ejection processes from the Be star to the Be disk on MJD 55820 and MJD 56600. The V/R quasi-period is about two years during 2011–2015, which is different from 1994 to 1995. Furthermore, the periods I → II → III → IV in the (B − V) color index versus V-band magnitude diagram constitute a cycle. From the behavior of the V/R ratio of Hα lines, and the variability of the V band, we believe that the precession of the density perturbation inside the disk is retrograde.

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