Drama

Brinkmann, Richard

doi:10.1007/978-3-476-03131-0_22

Cited by 2 publications

(2 citation statements)

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“…Margon et al 1979;Kotani et al 1994) from thermal gas. The model developed and generally accepted to describe the emission of the thermal component of the jets is the 'adiabatic cooling model' (Brinkmann et al 1991;Kotani et al 1996; see also Marshall et al 2002). The temperature and the density of the jet gas decrease with increasing distance from the binary core.…”

Section: Introductionmentioning

confidence: 99%

Rapid variability of the arcsec-scale X-ray jets of SS 433

Migliari

Fender

Blundell

et al. 2005

Monthly Notices of the Royal Astronomical Society

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We present the X-ray images of all the available Chandra observations of the galactic jet source SS 433. We have studied the morphology of the X-ray images and inspected the evolution of the arcsec X-ray jets, recently found to be manifestations of in situ reheating of the relativistic gas downstream in the jets. The Chandra images reveal that the arcsec X-ray jets are not steady long term structures; the structure varies, indicating that the reheating processes have no preference for a particular precession phase or distance from the binary core. Three observations made within about five days in May 2001, and a 60 ks observation made in July 2003 show that the variability of the jets can be very rapid, from timescales of days to (possibly) hours. The three May 2001 images show two resolved knots in the east jet getting brighter one after the other, suggesting that a common phenomenon might be at the origin of the sequential reheatings of the knots. We discuss possible scenarios and propose a model to interpret these brightenings in terms of a propagating shock wave, revealing a second, faster outflow in the jet.Comment: accepted for publication in MNRA

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Section: Introductionmentioning

confidence: 99%

Rapid variability of the arcsec-scale X-ray jets of SS 433

Migliari

Fender

Blundell

et al. 2005

Monthly Notices of the Royal Astronomical Society

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“…(o,r): [64]; X-ray obs. : [23,35,68,69,259,372]; Doppler shift X-ray Fe line: [497,822]; extended X-ray lobes: [701,821]; γ-ray obs. : [226,415]; Doppler shifted opt.…”

Section: Conclusion and Remarksmentioning

confidence: 99%

Catalogue of high-mass X-ray binaries in the Galaxy ($4^{th}$ edition)

Liu,

van Paradijs,

Heuvel

2007

Preprint

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Aims. The aim of this catalogue is to provide the reader with some basic information on the X-ray sources and their counterparts in other wavelength ranges (γ-rays, UV, optical, IR, radio). Methods. Some sources, however, are only tentatively identified as high-mass X-ray binaries on the basis of their X-ray properties similar to the known high-mass X-ray binaries. Further identification in other wavelength bands is needed to finally determine the nature of these sources. In cases where there is some doubt about the high-mass nature of the X-ray binary this is mentioned. Literature published before 1 October 2005 has, as far as possible, been taken into account.Results. We present a new edition of the catalogue of high-mass X-ray binaries in the Galaxy. The catalogue contains source name(s), coordinates, finding chart, X-ray luminosity, system parameters, and stellar parameters of the components and other characteristic properties of 114 high-mass X-ray binaries, together with a comprehensive selection of the relevant literature. About 60% of the high-mass X-ray binary candidates are known or suspected Be/X-ray binaries, while 32% are supergiant/X-ray binaries.

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Drama

Cited by 2 publications

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Rapid variability of the arcsec-scale X-ray jets of SS 433

Rapid variability of the arcsec-scale X-ray jets of SS 433

Catalogue of high-mass X-ray binaries in the Galaxy ($4^{th}$ edition)

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