Be Components in X-Ray Binaries

Loore, C. De; Burger, M.; Dessel, E. L. van; Mouchet, M.

doi:10.1007/978-94-009-8565-0_55

Cited by 18 publications

(30 citation statements)

References 6 publications

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“…The orbital eccentricity of the system is 0.47 (Finger et al 1994). The terminal velocity of the stellar wind from the star with significant optical output is ∼630 km s −1 (Giovannelli et al 1982), and its mass loss rate is ∼10 −8 M yr −1 de Loore et al 1984). The X-ray pulsar is close to its equilibrium state (Bisnovatyi-Kogan 1991;Li & van den Heuvel 1996), which could be a reason why some of the expected X-ray outbursts have failed to occur.…”

Section: Introductionmentioning

confidence: 99%

“…This was noted at the end of the eighties, as discussed by Giovannelli & Ziółkowski (1990, and references therein), or in the mid-nineties, as found by the RXTE satellite (see http:// space.mit.edu/XTE). The O9.7 IIIe companion does not normally fill its Roche lobe (de Loore et al 1984), although a temporary accretion disc can be formed around the neutron star when it is close to periastron (Giovannelli & Ziółkowski 1990). …”

Section: Introductionmentioning

confidence: 99%

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HeI doubled emission lines from A0535+26 ≡ HDE 245770

Giovannelli

Bernabei

Rossi

et al. 2007

A&A

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We report results of the spectroscopy for V725 Tau (HDE 245770, BD +26• 883), commonly known as Flavia's star, which is the optical counterpart of the X-ray pulsar A0535+26, carried out at the 1.5 m Loiano telescope during one run of observations of this star spread over a period of years. The HeI emission lines clearly show doubling, which is good evidence for the presence of a disc. In this paper we critically discuss the possibility that this disc is a temporary accretion disc around the neutron star, a view that contrasts to the usual interpretation, which considers that this sort of doubling in the HeI emission lines is due to a disc formed by gas expelled from the Be star. In the former case the outer radius of the accretion disc could range from 5.9 × 10 10 cm to 2.1 × 10 11 cm, taking the most probable range into account for the orbital inclination of the binary system, from 35• to 39• . The presence of such a temporary accretion disc around the neutron star was predicted by Giovannelli & Ziółkowski (1990).

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Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

HeI doubled emission lines from A0535+26 ≡ HDE 245770

Giovannelli

Bernabei

Rossi

et al. 2007

A&A

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“…12 middle and lower panels, respectively). The maximum and minimum values ofṀ 0 were derived from Persi et al (1979) and de Loore et al (1984), respectively. The mass of the gas falling onto the neutron star during the flare was found from Eq.…”

Section: Resultsmentioning

confidence: 99%

“…We took, for the most intensive outburst,Ṁ 0 = 10 −7 M /year as the maximum value ofṀ (Persi et al 1979), M 0 = 3 × 10 −8 M /year andṀ 0 = 10 −8 M /year for weaker outbursts (de Loore et al 1984). The disk is formed at radius r 0 , at which the velocity, v flow , of the matter flowing out from the star is of the order of the Keplerian velocity v K = √ GM/r 0 .…”

Section: Time-delay Modelmentioning

confidence: 99%

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

Giovannelli¹,

Бисноватый-Коган²,

Klepnev³

2013

A&A

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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.

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The Origin of X-Ray Pulsars in Binary Systems

Giovannelli

Sabau-Graziati²

2000

The Evolution of the Milky Way

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Be Components in X-Ray Binaries

Cited by 18 publications

References 6 publications

HeI doubled emission lines from A0535+26 ≡ HDE 245770

HeI doubled emission lines from A0535+26 ≡ HDE 245770

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

The Origin of X-Ray Pulsars in Binary Systems

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