A0535+26 - A hard X-ray observation of the 1977 December flare-up with the Prognoz 6 Signe II experiment

Violes, F.; Niel, M.; Bui-van, A.; Védrenne, G.; Chambon, Guillaume; Estulin, I. V.; Rakhamimov, Sh. Iu.

doi:10.1086/160506

Cited by 4 publications

(9 citation statements)

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“…This maximum in the softer region occurred about a week earlier than in the harder region (28-40 keV). Figure 14 shows the spectral evolution of A 0535 + 26 during the December 1977 outburst (Violes et al, 1982). Figure 15 shows the combined energy spectrum of A 0535 + 26, derived …”

Section: Day Of Oecember Igt?mentioning

confidence: 99%

“…Usually, to improve the signal-to-noise ratio, the technique to compose two successive high-resolution SW spectra is used. (Violes et al, 1982).…”

Section: Uv Observationsmentioning

confidence: 99%

“…Prognoz 6 Signe III Prognoz 6 Signe III Signe III Ariel V Vela 5B SAS 3 SAS 3 Ariel V Ariel V Vela 5B Ariel V Ariel V Ariel V Vela 5B Vela 5B Ariel V Ariel V Ariel V Ariel V Vela 5B Balloon Hakucho Violes et aL, 1982Bouchacourt et al, 1981Bouchacourt et al, 1981Warwick et aL, 1981Priedhorsky et al, 1983Kaluzienski et al, 1978Kaluzienski et aL, 1978Priedhorsky et aL, 1983Kaluzienski et al, 1978Warwick et al, 1981Warwick et aL, 1981Priedhorsky et aL, 1983Priedhorsky et al, 1983Sims et al, 1979Warwick et al, 1981Sims et al, 1979Warwick et aL, 1981Priedhorsky et aL, 1983Hameury et al, 1983Nagase et al, 1982 Sembay et al, 1989 Sembay et al, 1989 Sembay et al, 1989 Sembay et al, 1989 Sembay et al, 1989 Sembay et al, 1989 Sembay et al, 1989 Sembay et al, 1989 Sembay et al, 1989 Sembay et aL, 1989 Sembay et al, 1989 Sembay et aL, 1989…”

Section: Signe IIIunclassified

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A 0535 + 26/HDE 245770: A typical X-ray/Be system

Giovannelli

Graziati

1992

Space Sci Rev

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Abstract. Among the X-ray/Be systems, A 0535 + 26/HDE 245770 has been noted, since its discovery, for its peculiar features in several respects, in a wide energy range. For this reason and for a series of concomitant favorable causes, this system has been one of the most studied among the massive X-ray binary systems. The most remarkable incident was that its optical identification with an early-type-emission-line star (O9.7IIie) has led to a deep studies on Be stars and their interactions with neutron stars, which have allowed to discover, without unbiguity, the presence of optical indicators of consequent X-ray flares, as well as that Be stars in X-ray/Be systems behave just as 'normal' Be stars. Overmore, thanks to the multifrequency coordinated observations of this system, the X-ray emissions from binary companion of the Be stars are best explained by assuming the presence of a thick equatorial disk with low expansion velocity and a thin polar region with high expansion velocity. This picture reconciled the strong discrepancy in mass loss rate evaluations coming from IR and from UV measurements, assuming that the observed regions are enterely distinct from each other, one being a high-density, low-velocity region, and the other being a low-density, very hot, rapidly-expanding disk-like zone.Since, this picture seems to be the best up-to-date frame to cuckold all the experimental panorama available on X-ray/Be systems, we would like to paint in this paper the multifrequency behaviour of A 0535 + 26/HDE 245770, which is the best studied among such systems, in order to stimulate future coordinated experimental-theoretical works on this very interesting class of objects.

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Section: Day Of Oecember Igt?mentioning

confidence: 99%

“…Usually, to improve the signal-to-noise ratio, the technique to compose two successive high-resolution SW spectra is used. (Violes et al, 1982).…”

Section: Uv Observationsmentioning

confidence: 99%

Section: Signe IIIunclassified

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A 0535 + 26/HDE 245770: A typical X-ray/Be system

Giovannelli

Graziati

1992

Space Sci Rev

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“…Figure 4 shows the optical flare (red stars) constructed from the Bartolini et al (1978) and Rössiger (1978) data, and the subsequent X-ray outburst (black crosses) (Violes et al 1982). The data are consistent: the optical flare precedes the beginning of the X-ray outburst by several days, in this case by ∼3.…”

Section: Fig 3 Optical Outburst In U B V R Imentioning

confidence: 76%

“…Figure 10 shows the first X-ray emission detected from A0535+26 (black crosses and points) and the periastron passage at cycle 22 before 811205-E (red line). The X-ray detection of (Bartolini et al 1978;Rössiger 1978) (red stars) preceding the X-ray outburst of A 0535+26 (black crosses) (Violes et al 1982). The red line marks the periastron passage at the thirteenth cycle before 811205-E. .…”

Section: Fig 3 Optical Outburst In U B V R Imentioning

confidence: 97%

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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X-ray emission from Be star/X-ray binaries

Apparao

1994

Space Sci Rev

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A0535+26 - A hard X-ray observation of the 1977 December flare-up with the Prognoz 6 Signe II experiment

Cited by 4 publications

References 0 publications

A 0535 + 26/HDE 245770: A typical X-ray/Be system

A 0535 + 26/HDE 245770: A typical X-ray/Be system

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

X-ray emission from Be star/X-ray binaries

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