Gravitational darkening coefficients of the stars in the semidetached binary V Puppis

Antokhina, É. A.; Seifina, Elena; Черепащук, А. М.

doi:10.1134/1.1862357

Cited by 23 publications

(55 citation statements)

References 8 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…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

View full text Add to dashboard Cite

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 ,

show abstract

Section: Discussionmentioning

confidence: 99%

Spectroscopic Observations of the Mass Donor Star in SS 433

Hillwig¹,

Gies²

2008

ApJ

View full text Add to dashboard Cite

show abstract

“…Clearly, this is an unacceptable model. Now let us decrease K v down to 85 km s −1 , the lower limit that follows from a more accurate treatment of the heating effect in the radial velocity curve analysis (Wade & Horne 1988;Antokhina et al 2005). This would yield a better fit with m x = 17 M , m v = 55 M , and K x = 283 km s −1 , still too high to be acceptable.…”

Section: Implications For Binary Massesmentioning

confidence: 99%

“…The analysis (Wade & Horne 1988;Antokhina et al 2005) indicates that the true value of the semiamplitude of the radial velocity curve as derived from these absorption lines can be reduced to ∼85 km s −1 (see below).…”

Section: Measurements Of the Radial Velocity Of The Optical Starmentioning

confidence: 99%

“…To interpret the X-ray light curve of SS433 we used a geometric model applied earlier to the analysis of the Ginga X-ray eclipse (Antokhina et al 1992). We consider a close binary system consisting of an opaque "normal" star limited by the Roche equipotential surface and a relativistic object surrounded by an optically and geometrically thick "accretion disk".…”

Section: The Geometric Model Of the Systemmentioning

confidence: 99%

See 1 more Smart Citation

INTEGRAL observations of SS433: Results of a coordinated campaign

Черепащук¹,

Sunyaev

Fabrika

et al. 2005

A&A

Self Cite

136

View full text Add to dashboard Cite

Abstract. Results of simultaneous INTEGRAL and optical observations of the galactic microquasar SS433 in May 2003and INTEGRAL /RXTE observations in March 2004 are presented. Persistent precessional variability with a maximum to minimum uneclipsed hard X-ray flux ratio of ∼4 is discovered. The 18-60 keV X-ray eclipse is found to be in phase with optical and near infrared eclipses. The orbital eclipse observed by INTEGRAL in May 2003 is at least two times deeper and apparently wider than in the soft X-ray band. The broadband 2-100 keV X-ray spectrum simultaneously detected by RXTE/INTEGRAL in March 2004 can be explained by bremsstrahlung emission from optically thin thermal plasma with kT ∼ 30 keV. Optical spectroscopy with the 6-m SAO BTA telescope confirmed the optical companion to be an A5-A7 supergiant. For the first time, spectorscopic indications of a strong heating effect in the optical star atmosphere are found. The measurements of absorption lines which are presumably formed on the non-illuminated side of the supergiant yield its radial velocity semi-amplitude K v = 132 ± 9 km s −1 . The analysis of the observed hard X-ray light curve and the eclipse duration, combined with the spectroscopically determined optical star radial velocity corrected for the strong heating effect, allows us to model SS433 as a massive X-ray binary. Assuming that the hard X-ray source in SS433 is eclipsed by the donor star that exactly fills its Roche lobe, the masses of the optical and compact components in SS433 are suggested to be M v ≈ 30 M and M x ≈ 9 M , respectively. This provides further evidence that SS433 is a massive binary system with supercritical accretion onto a black hole.

show abstract

“…The synthesis of the theoretical absorption-line profiles and radial-velocity curves for the optical star in an X-ray binary system was carried out using the algorithm described in detail by Antokhina et al [5,6]. We will briefly summarize the basis of this method here.…”

Section: Synthesis Of the Radial-velocity Curves For The Optical Starmentioning

confidence: 99%

Dependence of the absorption-line profiles and radial-velocity curve of the optical star in an X-ray binary on the orbital inclination and component-mass ratio

Абубекеров¹,

Antokhina²,

Черепащук³

2005

Astron. Rep.

Self Cite

View full text Add to dashboard Cite

Abstract-Theoretical absorption-line profiles and radial-velocity curves for tidally deformed optical stars in X-ray binary systems are calculated assuming LTE. The variations in the profile shapes and radialvelocity curve of the optical star are analyzed as a function of the orbital inclination of the X-ray binary system. The dependence of the shape of the radial-velocity curve on the orbital inclination i increases with decreasing component-mass ratio q = m x /m v . The integrated line profiles and radial-velocity curves of the optical star are calculated for the Cyg X-1 binary, which are then used to estimate the orbital inclination and mass of the relativistic object: i < 43• and m x = 8.2−12.8 M . These estimates are in good agreement with earlier results of fitting the radial-velocity curve of Cyg X-1 using a simpler model (i < 45• , m x = 9.0−13.2 M ). c 2005 Pleiades Publishing, Inc. INTRODUCTIONThe optical component in an X-ray binary system is tidally deformed and has a complex temperature distribution on its surface due to the effects of gravitational darkening and X-ray heating. These effects of the interaction between the components give rise to orbital variability of the absorption-line profiles of an optical star. The orbital variability of the absorption profiles leads to a dependence of both the half-amplitude and the shape of the radial-velocity curve on the orbital inclination i and the component-The dependence of the shape of the radial-velocity curve of a tidally deformed optical star on the parameters of a close binary system was first pointed out by Sofia and Wilson [1]. Antokhina and Cherepashchuk [2] and Shabaz [3] proposed a new method for determining the component-mass ratio q = m x /m v and orbital inclination i of an X-ray binary based on the orbital variability of the absorptionline profiles in the spectrum of the optical star. Abubekerov et al. [4] estimated the orbital inclination of the X-ray binary Cyg X-1 using a high-accuracy observational radial-velocity curve.Here, we present the results of theoretical modeling of the radial-velocity curve of the optical star in a Roche model assuming LTE for various orbital inclinations, for X-ray systems with low-, moderate-, and high-mass optical stars. We analyze variations in the radial-velocity curve with variations of i for various values of q, together with the corresponding variations in the Hγ absorption-line profile.

show abstract

Gravitational darkening coefficients of the stars in the semidetached binary V Puppis

Cited by 23 publications

References 8 publications

Spectroscopic Observations of the Mass Donor Star in SS 433

Spectroscopic Observations of the Mass Donor Star in SS 433

INTEGRAL observations of SS433: Results of a coordinated campaign

Dependence of the absorption-line profiles and radial-velocity curve of the optical star in an X-ray binary on the orbital inclination and component-mass ratio

Contact Info

Product

Resources

About