Volume 622, February 2019
|Number of page(s)||9|
|Section||Stellar structure and evolution|
|Published online||15 February 2019|
Spectral observations of X Persei: Connection between Hα and X-ray emission
Institute of Astronomy and National Astronomical Observatory, Bulgarian Academy of Sciences, Tsarigradsko Shose 72, 1784 Sofia, Bulgaria
e-mail: email@example.com, firstname.lastname@example.org
2 Hamburger Sternwarte, Universität Hamburg, Gojenbergsweg 112, 21029 Hamburg, Germany
3 Department of Physics and Astronomy, Shumen University, 115 Universitetska Str., 9700 Shumen, Bulgaria
Accepted: 10 January 2019
We present spectroscopic observations of the Be/X-ray binary X Per obtained during the period 1999–2018. Using new and published data, we found that during “disc-rise” the expansion velocity of the circumstellar disc is 0.4–0.7 km s−1. Our results suggest that the disc radius in recent decades show evidence of resonant truncation of the disc by resonances 10:1, 3:1, and 2:1, while the maximum disc size is larger than the Roche lobe of the primary and smaller than the closest approach of the neutron star. We find correlation between equivalent width of Hα emission line (Wα) and the X-ray flux, which is visible when 15 Å < Wα ≤ 40 Å. The correlation is probably due to wind Roche lobe overflow.
Key words: stars: emission-line, Be / stars: winds, outflows / X-rays: binaries / accretion, accretion disks / stars: individual: X Per
© ESO 2019
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