Spectral observations of X Persei : connection between X-ray and H-alpha emission. (arXiv:1811.09162v1 [astro-ph.SR])
<a href="http://arxiv.org/find/astro-ph/1/au:+Zamanov_R/0/1/0/all/0/1">R. Zamanov</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Stoyanov_K/0/1/0/all/0/1">K. A. Stoyanov</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wolter_U/0/1/0/all/0/1">U. Wolter</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Marchev_D/0/1/0/all/0/1">D. Marchev</a>
We present spectroscopic observations of the Be/X-ray binary X Per obtained
during the period 1999 – 2018. Using our as well as published data, we found
that during the disc-rise the expansion velocity of the circumstellar disc is
0.4 – 0.7 km/s. We suggest that the disc radius during the last decades show
evidences of resonant truncation of the disc by resonances 10:1, 3:1, 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 H-alpha emission line ($Walpha$) and the X-ray
flux, which is visible when 15 AA $< Walpha le 40$ AA. The correlation is
probably due to wind Roche lobe overflow.
We present spectroscopic observations of the Be/X-ray binary X Per obtained
during the period 1999 – 2018. Using our as well as published data, we found
that during the disc-rise the expansion velocity of the circumstellar disc is
0.4 – 0.7 km/s. We suggest that the disc radius during the last decades show
evidences of resonant truncation of the disc by resonances 10:1, 3:1, 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 H-alpha emission line ($Walpha$) and the X-ray
flux, which is visible when 15 AA $< Walpha le 40$ AA. The correlation is
probably due to wind Roche lobe overflow.
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