Diagnostics of SS433 with the RXTE

Filippova, E.V.; Revnivtsev, M.; Fabrika, S.; Постнов, К. А.; Seifina, Elena

doi:10.1051/0004-6361:20054784

Cited by 30 publications

(48 citation statements)

References 27 publications

(43 reference statements)

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“…The best-fit radial velocity curve for the combined sets of data shown in Figure 2 gives from the optical (Antokhina & Cherepashchuk 1987) and Xray (Antokhina et al 1992;Filippova et al 2006) light curves. We caution that our adopted value of K X is not conclusive and that the systemic velocity, g, is significantly different from the surrounding nebulosity and absorption features.…”

Section: Discussionmentioning

confidence: 99%

Spectroscopic Observations of the Mass Donor Star in SS 433

Hillwig¹,

Gies²

2008

ApJ

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The microquasar SS 433 is an interacting massive binary consisting of an evolved mass donor and a compact companion that ejects relativistic jets. The mass donor was previously identified through spectroscopic observations of absorption lines in the blue part of the spectrum that showed Doppler shifts associated with orbital motion and strength variations related to the orbital modulation of the star-to-disk flux ratio and to disk obscuration. However, subsequent observations revealed other absorption features that lacked these properties and that were probably formed in the disk gas outflow. We present follow-up observations of SS 433 at orbital and precession phases identical to those from several previous studies, with the goals of confirming the detection of the mass donor spectrum and providing more reliable masses for the two system components. We show that the absorption features present as well as those previously observed almost certainly belong to the mass donor star, and find revised masses of and for the mass donor and compact object, respectively. 12.3 ‫ע‬ 3.3 4.3 ‫ע‬ 0.8 M ,

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Section: Discussionmentioning

confidence: 99%

Spectroscopic Observations of the Mass Donor Star in SS 433

Hillwig¹,

Gies²

2008

ApJ

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“…6d,7d). Cherepashchuk et al (2005), based on the RXTE/ASM and Ginga data, and also Filippova et al (2006), based on the RXTE/PCA data, found that during the 'edge-on' precession phase the flux in the standard X-ray range is only 2 times smaller than at the phase of maximal opening of the funnel. We confirm this result: despite the fact that the jet and the inner parts of the funnel are obscured during the 'edge-on' phase, the observer sees a considerable X-ray flux.…”

Section: Power Spectrum At the 'Edge-on' Precession Phasementioning

confidence: 95%

X-ray variability of SS 433: effects of the supercritical accretion disc

Атапин

Fabrika

Medvedev

et al. 2014

Monthly Notices of the Royal Astronomical Society

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We study a stochastic variability of SS 433 in the 10 −4 − 5 × 10 −2 Hz frequency range based on RXTE data, and on simultaneous observations with RXTE and optical telescopes. We find that the cross-correlation functions and power spectra depends drastically on the precession phase of the supercritical accretion disc. When the wind funnel of the disc is maximally open to the observer, a flat part emerges in the power spectrum; a break is observed at the frequency 1.7 × 10 −3 Hz, with a power-law index β ≈ 1.67 at higher frequencies. The soft emission forming mostly in the jets, lags behind the hard and optical emission. When the observer does not see the funnel and jets (the 'edge-on' disc), the power spectrum is described by a single power-law with β ≈ 1.34 and no correlations between X-ray ranges are detected. We investigated two mechanisms to explain the observed variability at the open disc phase, 1) reflection of radiation at the funnel wall (X-rays and optical) and 2) the gas cooling in the jets (X-rays only). The X-ray variability is determined by the contribution of both mechanisms, however the contribution of the jets is much higher. We found that the funnel size is (2 − 2.5) × 10 12 cm, and the opening angle is ϑ f ∼ 50 • . X-ray jets may consist of three fractions with different densities: 8 × 10 13 , 3 × 10 13 and 5 × 10 11 cm −3 , with most of the jet's mass falling within the latter fraction. We suppose that revealed flat part in the power spectrum may be related to an abrupt change in the disc structure and viscous time-scale at the spherization radius, because the accretion disc becomes thick at this radius, h/r ∼ 1. The extent of the flat spectrum depends on the variation of viscosity at the spherization radius.

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“…The companion star is supposed to be centered at the (400, 0, 400) point (Filippova et al 2006), outside the computational domain, while a collapsed stellar remnant is situated at the jet base, i.e. at (60, 0, 60).…”

Section: Hydrodynamical Code Employedmentioning

confidence: 99%

Dynamical and radiative simulations of γ-ray jets in microquasars

Smponias¹,

Kosmas²

2013

Monthly Notices of the Royal Astronomical Society

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The emission of γ-rays in jets emanating from the vicinity of collapsed stellar remnants, in binary systems known as microquasars, is investigated using a three dimensional relativistic hydrocode (PLUTO), in combination with two in-house radiative transfer codes. Even though a great number of stellar systems may be addressed by such models, we restrict ourselves to the concrete example of the SS433 X-ray binary, the only microquasar with a definite hadronic content in its jets, as verified from spectral line observations. A variety of system configurations have been examined, by employing a hadron-based emission mechanism. The dependence of the γ-ray emissions on certain dynamical source properties, such as the hydrodynamic parameters of the mass-flow density, the gas-pressure and the temperature of the ejected matter, is simulated. Radiative properties, especially the assumed high energy proton population inside the jet plasma, and its effect on the calculated emission, are also examined. Two sets of initial conditions of the chosen microquasar are employed, in order to cover different scenarios pertaining to the system under consideration.

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Diagnostics of SS433 with the RXTE

Cited by 30 publications

References 27 publications

Spectroscopic Observations of the Mass Donor Star in SS 433

Spectroscopic Observations of the Mass Donor Star in SS 433

X-ray variability of SS 433: effects of the supercritical accretion disc

Dynamical and radiative simulations of γ-ray jets in microquasars

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