Time delay between the optical and X-ray outbursts in the high-mass X-ray transient A0535+26/HDE245770

Author： Giovannelli F. Bisnovatyi-Kogan G. S. Klepnev A. S.

E-ISSN： 1432-0746|560|issue|A1-A1

ISSN： 0004-6361

Source： Astronomy & Astrophysics, Vol.560, Iss.issue, 2013-11, pp. : A1-A1

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Abstract

The optical behavior of the Be star in the high-mass X-ray transient A0535+26/HDE245770 shows that at periastron the luminosity is typically enhanced by 0.02 to a few tenths mag, and the X-ray outburst occurs eight days after the periastron. We constructed a quantitative model for this event based on a nonstationary accretion disk behavior, connected with a high ellipticity of the orbital motion. We explain the observed time delay between the peaks of the optical and X-ray outbursts in this system by the time of radial motion of the matter in the accretion disk, after an increase of the mass flux in the vicinity of a periastral point in the binary. This time is determined by the turbulent viscosity with a parameter of α = 0.1−0.3. The increase of the mass flux is a sort of flush that reaches the external part of the accretion disk around the neutron star, which enhances the optical luminosity. The subsequent X-ray flare occurs when the matter reaches the hot central parts of the accretion disk and the neutron star’s surface.