Long-term variability of the Be/X-ray binary A0535+26. I - Optical and UV spectroscopy

Details Long-term variability of the Be/X-ray binary A0535+26. I - Optical and UV spectroscopy Long-term variability of the Be/X-ray binary A0535+26. I - Optical and UV spectroscopy

Feb 1998

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998mnras.294..165c&link_type=abstract

Monthly Notices of the Royal Astronomical Society, vol. 294, p. 165

Astronomy and Astrophysics

Astronomy

31

Ultraviolet Spectroscopy, X Ray Binaries, Optical Measurement, Astronomical Spectroscopy, Variable Stars, Variability, Time Dependence, H Alpha Line, Stellar Oscillations, Astronomical Photometry

Scientific paper

The results of a seven-yr optical and UV spectroscopic study of the high-mass X-ray binary A0535+26 are presented. It was found that throughout the period of the observations the line profile of H-alpha showed considerable variability. A correlation between the equivalent width of H-alpha and both V-band magnitude and (B-V) color excess was observed, albeit with considerable scatter present in the data set. A giant X-ray flare in early 1994 was accompanied by a fading in optical and infrared photometric bands, and a reduction in the equivalent width of H-alpha. When the star was observed in 1994 September, it was found to have developed a double-peaked H-alpha profile, and further observations saw the V/R peak ratio vary cyclically, with a period of about one yr. If this is identified as a global one-armed oscillation, it becomes the shortest period ever observed in a Be star. The accompanying photometric and spectroscopic observations provide a test of any theory seeking to describe the onset and behavior of such a density wave.

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