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Post Info TOPIC: SS433 Binary System
Blobrana


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Posts: 131433
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V1343 Aquilae
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The high mass X-ray binary V1343 Aquilae (SS 433) is reported undergoing a phase of radio flaring which started around 3rd  August, 2011.

Position (2000):     RA 19 11 49.57  |  Dec +04° 58' 57.9''



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Blobrana


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Posts: 131433
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RE: SS433 Binary System
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Title: SS 433: The wiggle of the wind
Authors: M. G. Bowler

The Balmer H alpha emission line in the stationary spectrum of SS 433 has a component originating in the wind above the accretion disk. The Doppler motion of this line is a blurred representation of the motion of the compact object accreting. I show how this may be understood in terms of emission lasting over a few days, like radiation from the jet bolides.

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Blobrana


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Posts: 131433
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SS 433
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Title: On Purple Mountain Halpha observations of SS 433
Authors: M G Bowler

In this brief note I draw attention to the structure of the stationary Halpha line as a function of orbital phase, using a data set compiled over some years. These data are compared with a set of nightly observations over some 2 orbits. The structures are very similar and this is highly relevant to the question of persistence and stability of spectral features which have been attributed to a circumbinary disk.

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Blobrana


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RE: SS433 Binary System
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SS 433 is one of the most exotic star systems observed. It is an eclipsing X-ray binary system, with the primary most likely a black hole, or possibly a neutron star.
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It is a bizarre 14th magnitude object  about 11,000 light years away, lying in the constellation of Aquila.  Ever since its peculiar nature was discovered  in 1979 by Paul Murdin and David Clark, it has been scrutinised at many wavelengths.
It  was labelled by the popular press as "the star that's both coming and going",  since it displays both redshifted and blueshifted spectral features.
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Blobrana


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Posts: 131433
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Title: The mass of SS 433: a conflict resolved?
Authors: M. G. Bowler

The Galactic microquasar SS 433 is very luminous and launches oppositely-directed jets of cool hydrogen at a quarter of the speed of light. Data from observations of the circumbinary disk imply a system mass exceeding 40 solar masses. The most recent attempts to establish a mass via observation of absorption lines in the spectrum of the companion imply a system mass of no more than 20 solar masses. To examine these conflicting data and present a possible resolution of this conflict. Interpretation of data through the application of simple trigonometry to the configuration of the SS 433 system. The absorption spectra which, attributed to the atmosphere of the companion, yield an orbital speed of ~ 60 km s^{-1} could equally well be attributed to absorption of light from the companion in material of the circumbinary disk. In that case the absorption spectra yield an orbital speed for the circumbinary disk material of ~ 240 km s^{-1}, in agreement with the emission line data. If continuum light from the companion is absorbed in passage through the circumbinary disk material rather than in the atmosphere of the companion itself, the absorption spectra are entirely consistent with observations of the circumbinary disk and a system mass exceeding ~ 40 solar masses. The striking consistency implies that the compact object is a rather massive stellar black hole.

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Blobrana


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Posts: 131433
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Eastern Filament of W50
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Title: The Eastern Filament of W50
Authors: P. Abolmasov, O. Maryeva, N. A. Burenkov

We present new spectral (FPI and long-slit) data on the Eastern optical filament of the well known radionebula W50 associated with SS433. We find that on sub-parsec scales different emission lines are emitted by different regions with evidently different physical conditions. Kinematical properties of the ionised gas show evidence for moderately high (V ~ 100 km/s) supersonic motions. [OIII]5007 emission is found to be multi-component and differs from lower-excitation [SII]6717 line both in spatial and kinematical properties. Indirect evidence for very low characteristic densities of the gas (n ~ 0.1cm^{-3}) is found. We propose radiative (possibly incomplete) shock waves in low-density, moderately high metallicity gas as the most probable candidate for the power source of the optical filament. Apparent nitrogen over-abundance is better understood if the location of W50 in the Galaxy is taken into account.

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Blobrana


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Posts: 131433
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RE: SS433 Binary System
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Title: Revision of distance to SS433
Authors: A. A. Panferov

Critical analysis shows that all estimates of the velocity of the radio jets of SS433 and the distance to the object based on the relativistic effect of light travel time are not accurate enough to be conclusive. From our elaboration of kinematics of knots in the radio jets in a sequence of images, a kinematic model of the radio jets with a velocity of 0.20c is a little better than one with the canonical velocity 0.26c observed actually in the optical and X-ray jets of SS433. Consequently the distance to SS433 should be lowered to 4.3 kpc.
Besides this difference in velocity, the shift of the radio jets in the precession phase reveals itself in non-transient fashion, whereas it is not observed in the optical jets. In light of these differences, the jets must have two-component structure: with on-axis channel - optical jets, and low velocity shell - radio jets.

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Blobrana


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Posts: 131433
Date:
SS 433
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Title: Optical Multicolour Observations of the SS 433=V 1343 Aql Microquasar
Authors: A.N. Sazonov

We report BVR photometry of the V1343 Aql= SS 433 microquasar at different phases of the 13-day orbital cycle for the 1986-1990 observing seasons. The data include five complete cycles of the 163^{d} precession period of the system. We obtain mean light curves and colour-colour diagrams with the orbital period for all intervals of precession phases. The optical component of the close binary system (CBS) fills its critical Roche lobe and loses mass on the thermal relaxation time scale. Gaseous flow show up actively in the system and activity manifestations differ substantially at different precession phases.

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Blobrana


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Posts: 131433
Date:
SS433
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Title: Analysis of hard X-ray eclipse in SS433 from INTEGRAL observations
Authors: A.M. Cherepashchuk (1), R.A. Sunyaev (2), K.A. Postnov (1), E.A. Antokhina (1), S.V. Molkov (2,3) (1- Sternberg Astronomical Institute, Moscow, 2 - Space Research Institute, Moscow, 3 - CESR, Toulouse)

The analysis of hard X-ray INTEGRAL observations (2003-2008) of superaccreting galactic microquasar SS433 at precessional phases of the source with the maximum disk opening angle is carried out. It is found that the shape and width of the primary X-ray eclipse is strongly variable suggesting additional absorption in dense stellar wind and gas outflows from the optical A7I-component and the wind-wind collision region. The independence of the observed hard X-ray spectrum on the accretion disk precessional phase suggests that hard X-ray emission (20-100 keV) is formed in an extended, hot, quasi-isothermal corona, probably heated by interaction of relativistic jet with inhomogeneous wind outflow from the precessing supercritical accretion disk. A joint modelling of X-ray eclipsing and precessional hard X-ray variability of SS433 revealed by INTEGRAL by a geometrical model suggests the binary mass ratio q=m_x/m_v\simeq 0.25\div 0.5. The absolute minimum of joint orbital and precessional \chi˛  residuals is reached at q\simeq 0.3. The found binary mass ratio range allows us to explain the substantial precessional variability of the minimum brightness at the middle of the primary optical eclipse. For the mass function of the optical star f_v=0.268 solar masses as derived from Hillwig & Gies data, the obtained value of q\simeq 0.3 yields the masses of the components m_x\simeq 5.3 solar masses, m_v\simeq 17.7 solar masses, confirming the black hole nature of the compact object in SS433.

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Blobrana


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Posts: 131433
Date:
SS 433
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The RATAN-600 radio telescope,  located near Zelenchukskaya in the Caucasus, is monitoring the high-mass X-ray binary SS433 in the constellation Aquila.
The binary star system consists of an early type star and a compact object (neutron star or black hole).

Image (PNG Image, 792x612 pixels)

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