Time delay between the optical and X-ray outbursts in the high-mass X-ray transient A0535 26/HDE245770. Astronomy and Astrophysics Volume 560, 2013, Article number A1

14 сентября 2018
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Контактные данные автора публикации Giovannelli, F.a , Bisnovatyi-Kogan, G.S.bc, Klepnev, A.S.bc a INAF-Istituto di Astrofisica e Planetologia Spaziali, Area di Ricerca di Tor Vergata, via del Fosso del Cavaliere 100, 00133 Roma, Italy b Space Research Institute, Profsoyuznaya 84/32,
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Аннотация

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 stars surface.
Indexed keywords
Accretion accretion disks; Stars: emission-line be; Stars: individual; Stars: neutrons; X-rays: Binaries; X-rays: individual
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