The third body in the eclipsing system RR Lyn

Khaliullin, Kh. F.; Khaliullina, A. I.

doi:10.1134/1.1451925

Cited by 21 publications

(38 citation statements)

References 10 publications

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“…All photoelectric times of minimum light published in Khaliullina & Khaliullin (1992), Todoran (1992, his Caton & Burns (1993), Hegedüs et al (1996), Agerer & Hübscher (1996, 1997, Borkovits & Bíró (1998), Bíró & Borkovits (2000), as well as Agerer et al (2001) were incorporated in our analysis. A total of 85 times of minimum light were used, including 39 secondary eclipses.…”

Section: Hs Hermentioning

confidence: 99%

Apsidal motion and light-time effect in eclipsing binaries HS Herculis and U Ophiuchi

Wolf

Harmanec

Diethelm

et al. 2002

A&A

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Abstract. Several new times of minima, based on photoelectric observations, have been secured for two bright and well-known eclipsing binaries with eccentric orbits and with very similar orbital periods: HS Her (P = 1.d 637, e = 0.02) and U Oph (P = 1.d 677, e = 0.003). For HS Her, an apsidal motion with a period of 78 years is confirmed and a third body in an eccentric orbit with a period of 85 years is found. An analysis of all available eclipse timings of U Oph has confirmed the presence of an apsidal motion with one of the shortest known periods (20.1 yr) and a light-time effect with the improved period of 37.6 yr. The corresponding internal structure constants log k2 were also derived. It is estimated that the tertiaries of both systems are detectable via speckle interferometry.

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Section: Hs Hermentioning

confidence: 99%

Apsidal motion and light-time effect in eclipsing binaries HS Herculis and U Ophiuchi

Wolf

Harmanec

Diethelm

et al. 2002

A&A

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“…In that case its luminosity can be completely neglected (even in NIR) and we included this system in our sample. RR Lyn is a proposed triple system with a companion of 0.1 M ⊙ (Khaliullin & Khaliullina 2002). Even if the companion will be confirmed with future spectroscopic monitoring at the moment no third light is visible in high quality light curves (e.g.…”

Section: Multiplicitymentioning

confidence: 99%

The Surface Brightness-color Relations Based on Eclipsing Binary Stars: Toward Precision Better than 1% in Angular Diameter Predictions

Graczyk

Konorski

Pietrzyński

et al. 2017

ApJ

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In this study we investigate the calibration of surface brightness-color (SBC) relations based solely on eclipsing binary stars. We selected a sample of 35 detached eclipsing binaries with trigonometric parallaxes from Gaia DR1 or Hipparcos, whose absolute dimensions are known with an accuracy better than 3% and that lie within 0.3 kpc from the Sun. For the purpose of this study, we used mostly homogeneous optical and near-infrared photometry based on the Tycho-2 and 2MASS catalogs. We derived geometric angular diameters for all stars in our sample with a precision better than 10%, and for 11 of them with a precision better than 2%. The precision of individual angular diameters of the eclipsing binary components is currently limited by the precision of the geometric distances (∼5% on average). However, by using a subsample of systems with the best agreement between their geometric and photometric distances, we derived the precise SBC relations based only on eclipsing binary stars. These relations have precisions that are comparable to the best available SBC relations based on interferometric angular diameters, and they are fully consistent with them. With very precise Gaia parallaxes becoming available in the near future, angular diameters with a precision better than 1% will be abundant. At that point, the main uncertainty in the total error budget of the SBC relations will come from transformations between different photometric systems, disentangling of component magnitudes, and for hot OB stars, the main uncertainty will come from the interstellar extinction determination. We argue that all these issues can be overcome with modern high-quality data and conclude that a precision better than 1% is entirely feasible.

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“…In order to determine which parts of mass plane are consistent with the observed variation, we constructed model V-band light curves using the GENSYN code (Mochnacki & Doughty 1972;Gies & Bolton 1986a) for the four values of fill-out factor illustrated in Figure 8. There is a unique solution for the best fit of the light curve along each line of constant fill-out factor, since the light curve amplitude (Khaliullin & Khaliullina 1981) at each value of the fill-out factor. monotonically decreases with decreasing inclination (increasing distance).…”

Section: Mass Of the Supergiantmentioning

confidence: 99%

“…This small fraction is consistent with our successful fitting of the UV and optical line features Figure 7. UV light curve from both the HST and IUE spectra (diamonds) compared with the V-band light curve (circles) from Khaliullin & Khaliullina (1981). The UV data were divided into eight orbital phase bins, and the error bars indicate the standard deviation within each bin.…”

Section: Uv-ir Spectral Energy Distributionmentioning

confidence: 99%

THE ULTRAVIOLET SPECTRUM AND PHYSICAL PROPERTIES OF THE MASS DONOR STAR IN HD 226868 = Cygnus X-1

Caballero-Nieves

Gies

Bolton

et al. 2009

ApJ

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We present an examination of high-resolution, ultraviolet (UV) spectroscopy from Hubble Space Telescope of the photospheric spectrum of the O-supergiant in the massive X-ray binary HD 226868 = Cyg X-1. We analyzed this and ground-based optical spectra to determine the effective temperature and gravity of the O9.7 Iab supergiant. Using non-LTE, line-blanketed, plane-parallel models from the TLUSTY grid, we obtain T eff = 28.0 ± 2.5 kK and log g 3.00 ± 0.25, both lower than in previous studies. The optical spectrum is best fit with models that have enriched He and N abundances. We fit the model spectral energy distribution for this temperature and gravity to the UV, optical, and infrared (IR) fluxes to determine the angular size and extinction toward the binary. The angular size then yields relations for the stellar radius and luminosity as a function of distance. By assuming that the supergiant rotates synchronously with the orbit, we can use the radius-distance relation to find mass estimates for both the supergiant and black hole (BH) as a function of the distance and the ratio of stellar to Roche radius. Fits of the orbital light curve yield an additional constraint that limits the solutions in the mass plane. Our results indicate masses of 23 +8 −6 M for the supergiant and 11 +5 −3 M for the BH.

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The third body in the eclipsing system RR Lyn

Cited by 21 publications

References 10 publications

Apsidal motion and light-time effect in eclipsing binaries HS Herculis and U Ophiuchi

Apsidal motion and light-time effect in eclipsing binaries HS Herculis and U Ophiuchi

The Surface Brightness-color Relations Based on Eclipsing Binary Stars: Toward Precision Better than 1% in Angular Diameter Predictions

THE ULTRAVIOLET SPECTRUM AND PHYSICAL PROPERTIES OF THE MASS DONOR STAR IN HD 226868 = Cygnus X-1

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