SS 433: results of a recent multiwavelength campaign

Chakrabarti, Sandip K.; Anandarao, B. G.; Pal, Sabyasachi; Mondal, Soumen; Nandi, A.; Bhattacharyya, A.; Mandal, Samir; Sagar, Ram; Pandey, J. C.; Pati, A. K.; Saha, S. K.

doi:10.1111/j.1365-2966.2005.09368.x

Cited by 12 publications

(8 citation statements)

References 33 publications

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“…However, assuming flare stages are reported with accurate time-stamping and a dependence of these on orbital phase is discerned, we remark that this would be circumstantial evidence that there is ellipticity in the binary orbit of SS433, supporting our discussion in Section 3.1. Chakrabarti et al (2005) present a study of the variability of SS433's emission at radio, IR and optical wavelengths and report that there is typically a delay of 2 d between IR and radio variability. It seems plausible that this delay arises as type-2 flare peaks move from high radio frequency to low radio frequency as bolides expand and thus transition from being optically thick at a given frequency to optically thin.…”

Section: Clustering Timing and Phasing Of Flaresmentioning

confidence: 99%

SS433’s accretion disc, wind and jets: before, during and after a major flare

Blundell

Schmidtobreick

Трушкин

2011

Monthly Notices of the Royal Astronomical Society

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The Galactic microquasar SS433 launches oppositely directed plasma jets at speeds approximately a quarter of the speed of light along an axis which precesses, tracing out a cone of polar angle ∼20°. Occasionally the system exhibits a major flare when the intensity of its emission, especially at radio wavelengths, increases significantly and rapidly. We present an analysis of high‐resolution, almost‐nightly optical spectra obtained before, during and after a major flare, whose complex emission lines are deconstructed into single Gaussians and we demonstrate the different modes of mass loss in the SS433 system. During our monitoring, an initial period of quiescence was followed by increased activity which culminated in a radio flare. In the transition period, the accretion disc of SS433 became visible in Hα and He i emission lines and remained so until the observations were terminated; the line‐of‐sight velocity of the centre of the disc lines during this time behaved as though the binary orbit has significant eccentricity rather than being circular, consistent with three recent lines of evidence. After the accretion disc appeared, its rotation speed (as measured by the separation of the Hα disc emission lines) increased steadily from 500 to 700 km s−1. The launch speed of the jets first decreased then suddenly increased. At the same time, as the jet launch speed increased, the wind from the accretion disc doubled in speed. Two days afterwards, the radio flux exhibited a flare. These data suggest that a massive ejection of material from the companion star loaded the accretion disc and the system responded with mass loss via different modes that together comprise the flare phenomena. We find that archival data reveal similar behaviour, in that when the measured jet launch speed exceeds 0.29c, this is invariably simultaneous with, or a few days before, a radio flare. Thus the manifestation of a major flare is surmised to comprise the overloading of the accretion disc manifested in the speeding up of the Hα rotation, followed by enhanced mass loss not just via its famous jets at higher‐than‐usual speeds but also directly from its accretion disc’s wind.

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Section: Clustering Timing and Phasing Of Flaresmentioning

confidence: 99%

SS433’s accretion disc, wind and jets: before, during and after a major flare

Blundell

Schmidtobreick

Трушкин

2011

Monthly Notices of the Royal Astronomical Society

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“…However, assuming flare stages are reported with accurate time-stamping and a dependence of these on orbital phase is discerned, we remark that this would be circumstantial evidence that there is ellipticity in the binary orbit of SS433, supporting our discussion in Sec 3.1. Chakrabarti et al (2005) present a study of the variability of SS433's emission at radio, infra-red and optical wavelengths and report that there is typically a delay of two days between infrared and radio variability. It seems plausible that this delay arises as type-2 flare peaks move from high radio frequency to low radio frequency as bolides expand and thus transition from being optically thick at a given frequency to optically thin.…”

Section: Clustering Timing and Phasing Of Flaresmentioning

confidence: 99%

SS433's accretion disc, wind and jets: before, during and after a major flare

Blundell,

Schmidtobreick,

Trushkin

2011

Preprint

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The Galactic microquasar SS433 occasionally exhibits a major flare when the intensity of its emission increases significantly and rapidly. We present an analysis of high-resolution, almost-nightly optical spectra obtained before, during and after a major flare, whose complex emission lines are deconstructed into single gaussians and demonstrate the different modes of mass loss in the SS433 system. During our monitoring, an initial period of quiescence was followed by increased activity which culminated in a radio flare. In the transition period the accretion disc of SS433 became visible in Hα and He I emission lines and remained so until the observations were terminated; the line-of-sight velocity of the centre of the disc lines during this time behaved as though the binary orbit has significant eccentricity rather than being circular, consistent with three recent lines of evidence. After the accretion disc appeared its rotation speed, as measured by the separation of the Hα disc emission lines, increased steadily from 500 km/s to 700 km/s. The launch speed of the jets first decreased then suddenly increased. At the same time as the jet launch speed increased, the wind from the accretion disc doubled in speed. Two days afterwards, the radio flux exhibited a flare. These data suggest that a massive ejection of material from the companion star loaded the accretion disc and the system responded with mass loss via different modes that together comprise the flare phenomena. We find that archival data reveal similar behaviour, in that when the measured jet launch speed exceeds 0.29 c this is invariably simultaneous with, or a few days before, a radio flare. Thus we surmise that a major flare consists of the overloading of the accretion disc, resulting in the speeding up of the H-alpha rotation disc lines, followed by enhanced mass loss not just via its famous jets at higher-than-usual speeds but also directly from its accretion disc's wind.

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“…: [293,90]; evolutionary status: [381]; absorption features from accretion disc wind? : [25]; sharp variations in the X-ray, IR and radio, double X-ray Fe line profiles from the jet: [85]; massive ejection event with a QPO-like feature near 0.1 Hz: [398]; extended radio emission: [48]; X-ray dominated by precessing jets: [551,476]; bullet-like jets: [84]; highly ionized Doppler-shifted iron emission lines: [511]; identifiable deviations from the traditional kinematic model: [49]; rapid chaotic optical variability: [647] Pos. (x 0.6"): [344]; also known as EXO 1912+097: [443]; a HMXB with a NS: [670]; variable absorption column density: [670]; bright iron line: [670] Pos.…”

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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SS 433: results of a recent multiwavelength campaign

Cited by 12 publications

References 33 publications

SS433’s accretion disc, wind and jets: before, during and after a major flare

SS433’s accretion disc, wind and jets: before, during and after a major flare

SS433's accretion disc, wind and jets: before, during and after a major flare

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

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