Application of Spectrophotometry to a Binary Star Problem

Wilson, R. E.

doi:10.1086/128899

Cited by 6 publications

(6 citation statements)

References 2 publications

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“…The partially eclipsing nature of V757 Cen complicated the solution. From spectroscopic data we determined the problem in a similar way as Wilson (1970) did from spectroscopic information. The geometry of V757 Cen shows that the system is probably in contact since r g + r s = 0.76 (Kopal 1959).…”

Section: Discussionmentioning

confidence: 99%

“…Nevertheless, solutions may be obtained when some parameter of the model can be fixed from other observational evidence. R. E. Wilson (1970) considered also the problem of the indeterminacy of binaries showing partial eclipses by complementing the photometric observations with spectropotometric data. In our case we considered spectroscopic information.…”

Section: Light-curve Analysismentioning

confidence: 99%

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The close binary V757 Centauri

Cerruti¹,

Sisteró²

1982

PASP

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The W UMa system V757 Cen has been observed photoelectrically in the UBV system at Bosque Alegre and at El Leoncito Observatories. Full light curves were constructed from 1135 V, 1104 B, and 1104 U individual observations. An improved ephemeris based on about 12,000 cycles is given. A first classical solution for partial eclipses, determined with complementary spectroscopic data, suggests the system to be a contact W UMa star consisting of a larger component of spectral type G1-G2 and an F9-G0 companion.

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Section: Discussionmentioning

confidence: 99%

Section: Light-curve Analysismentioning

confidence: 99%

The close binary V757 Centauri

Cerruti¹,

Sisteró²

1982

PASP

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show abstract

“…12 depicts the projected shadow of a marching mesh compared to the theoretical horizon (see Appendix D) and demonstrates that the determined horizon of each star agrees well with the theoretical expectation. In contrast, the Fourier-based eclipse detection implemented in PHOEBE 1 (and WD) determines the horizon of each star by fitting a Fourier series to the coordinates of surface elements closest to the horizon (Wilson 1993). In consequence, this approach will always underestimate the size of the shadow with respect to the analytic horizon.…”

Section: Eclipse and Horizon Computationmentioning

confidence: 99%

Physics of Eclipsing Binaries. Ii. Toward the Increased Model Fidelity

Prša

Conroy

Horvat

et al. 2016

ApJS

292

214

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The precision of photometric and spectroscopic observations has been systematically improved in the last decade, mostly thanks to space-borne photometric missions and ground-based spectrographs dedicated to finding exoplanets. The field of eclipsing binary stars strongly benefited from this development. Eclipsing binaries serve as critical tools for determining fundamental stellar properties (masses, radii, temperatures and luminosities), yet the models are not capable of reproducing observed data well either because of the missing physics or because of insufficient precision. This led to a predicament where radiative and dynamical effects, insofar buried in noise, started showing up routinely in the data, but were not accounted for in the models. PHOEBE (PHysics Of Eclipsing BinariEs;http://phoebe-project.org) is an open source modeling code for computing theoretical light and radial velocity curves that addresses both problems by incorporating missing physics and by increasing the computational fidelity. In particular, we discuss triangulation as a superior surface discretization algorithm, meshing of rotating single stars, light time travel effect, advanced phase computation, volume conservation in eccentric orbits, and improved computation of local intensity across the stellar surfaces that includes photon-weighted mode, enhanced limb darkening treatment, better reflection treatment and Doppler boosting. Here we present the concepts on which PHOEBE is built on and proofs of concept that demonstrate the increased model fidelity.

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“…We carried out modeling of our data using the PHOEBE package (Prša & Zwitter 2005;Prsa et al 2011;Prša et al 2016) which is based on the Wilson-Devinney (WD) code (Wilson & Devinney 1971;Wilson 1979Wilson , 1993. It allows simultaneous modeling of photometric data in a number of filters and provides a graphical user interface.…”

Section: Light Curve Solutionsmentioning

confidence: 99%

The W UMa binaries USNO-A2.0 1350-17365531, V471 Cas, V479 Lac and V560 Lac: light curve solutions and global parameters based on Gaia distances

Kjurkchieva

Popov

Eneva

et al. 2019

Res. Astron. Astrophys.

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We present photometric observations in Sloan filters g ′ , i ′ of the eclipsing W UMa stars USNO-A2.0 1350-17365531, V471 Cas, V479 Lac and V560 Lac. The sinusoidal-like O-C diagram of V471 Cas shows presence of third body with mass of 0.12 M ⊙ (red dwarf) at distance 897 R ⊙ . The O-C diagram of V479 Lac reveals period decreasing of dP/dt = -1.69 × 10 −6 d yr −1 . The results of the light curve solutions are: (i) The targets are overcontact binaries with small fill-out factors; (ii) Their components are F-K stars, comparable in size, whose temperature differences are below 80 K; (iii) All targets undergo partial eclipses and to limit the possible mass ratios we carried out two-step q-search analysis. The target global parameters (luminosities, radii, masses) were obtained on the base of their GAIA distances and the results of our light curve solutions. The obtained total mass of V560 Lac turns out smaller than the lower mass limit for the presently existing W UMa binaries of 1.0 -1.2 M ⊙ , i.e. this target is an peculiar overcontact system.

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Application of Spectrophotometry to a Binary Star Problem

Cited by 6 publications

References 2 publications

The close binary V757 Centauri

The close binary V757 Centauri

Physics of Eclipsing Binaries. Ii. Toward the Increased Model Fidelity

The W UMa binaries USNO-A2.0 1350-17365531, V471 Cas, V479 Lac and V560 Lac: light curve solutions and global parameters based on Gaia distances

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