A Catalog of 1022 Bright Contact Binary Stars

Gettel, Sara; Geske, M.; McKay, Timothy A.

doi:10.1086/498016

Cited by 93 publications

(49 citation statements)

References 17 publications

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“…Calibrated photometry for large parts of the sky reaching down to V < 15 has been undertaken by a few wide-sky surveys. In addition to the Hipparcos and the Tycho-2 catalogs, data for V max have been taken from three other sources that we judged to be large enough to provide sufficient uniformity : Gettel et al (2006), Pojmanski et al (2005) 5 , and Terrell et al (2012). We re-evaluated the errors for V max and assumed that they are not smaller than 0.01 mag due to residual calibration errors.…”

Section: Photometric Datamentioning

confidence: 99%

“…The motivation for this study is the availability of newly measured, high precision parallaxes from the Gaia mission as well as standardized UBV photometry for W UMa binaries; the details of the photometric database are described in the next sub-section. Cross-matching of the catalogs led to the selection of EW binaries from Rucinski & Duerbeck (1997), Pojmanski et al (2005), Gettel et al (2006), andTerrell et al (2012), provided that they have corresponding Gaia parallaxes. After removing the poorer data points, the final sample consists of 318 EW binaries with absolute-magnitude errors σ(M V ) < 0.5 mag 3 .…”

Section: Introductionmentioning

confidence: 99%

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Absolute-magnitude Calibration for W UMa-type Systems Based on Gaia Data*

Mateo

Ruciński

2017

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Tycho-Gaia Astrometric Solution (TGAS) parallax data are used to determine absolute magnitudes M V for 318 W UMa-type (EW) contact binary stars. A very steep (slope ≃ −9), single-parameter (log P ), linear calibration can be used to predict M V to about 0.1 -0.3 mag over the whole range of accessible orbital period, 0.22 < P < 0.88 days. A similar calibration for the most common systems with 0.275 < P < 0.575 days predicts M V values to about 0.06 -0.16 mag. For orbital period values both shorter and longer than the central range, the period dependence is respectively steeper and shallower, i.e. the binaries are fainter in M V than predicted by the whole-range, linear law. The steepness of the relation for short-period systems implies important consequences for the detectability of the faintest binaries defining the short-period cut-off of the period distribution. Although the scatter around the linear log P -fit is fairly large (0.2 -0.4 mag), the current data do not support the inclusion of a B −V color term in the calibration.

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Section: Photometric Datamentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Absolute-magnitude Calibration for W UMa-type Systems Based on Gaia Data*

Mateo

Ruciński

2017

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“…Further expansion would carry the envelope to the equipotential surface that contains the outer Lagrangian point (L 2 ), through which material would then be lost from the system. Contact binaries are known to be quite common among variable stars; their spatial density is approximately 10 À4 pc À3 (see Gettel et al 2006 and references therein). The problem of existence of contact binaries was considered by Kuiper (1941), assuming the synchronous rotation of two stars in a circular orbit.…”

Section: Introductionmentioning

confidence: 99%

A Model for Contact Binary EP Andromedae

Manzoori¹

2012

Publ. – Astron. Soc. Aust

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This paper presents the first comprehensive study of the EP And system, a contact binary. In this work the solution of the standard V light curve was obtained using the PHOEBE program (version 0.3c). Absolute parameters of the stellar components were then determined, enabling us to discuss the structure and evolutionary status of the close binary EP And. The times of minima data ('OÀC curve') were analyzed. It was found that a third body with a period of 41.20 yr and mass 0.15 M } is orbiting around the system. Also a modulating period of an 11.72-yr cycle along with a relative period increase of DP P ¼ 1:79 Â 10 À7 were obtained, which were attributed to the magnetic activity cycle and mass transfer with rate Dm m ¼ 9:98 Â 10 À8 yr À1 between the components, respectively.

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“…The color indices of the binary star given by Gettel et al (2006) and Cutri et al (2003) are B − V = 0.525, J − H = 0.222, H − K = 0.049, and V − K = 1.399, which correspond to different values of temperature for the primary component (Cox 2000). Therefore, we choose a mean value, i.e., the temperature for star 1 (star eclipsed at primary light minimum) was fixed at T 1 = 6144 K. During the analysis, all of the original individual data points were used.…”

Section: Complete Ccd Light Curves and Photometric Solutions For Xy Lmentioning

confidence: 99%

High Fill-Out, Extreme Mass Ratio Overcontact Binary Systems. X. The Newly Discovered Binary Xy Leonis Minoris

Qian

Liu

Zhu

et al. 2011

The Astronomical Journal

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The newly discovered short-period close binary star, XY LMi, has been monitored photometrically since 2006. Its light curves are typical EW-type light curves and show complete eclipses with durations of about 80 minutes. Photometric solutions were determined through an analysis of the complete B, V , R, and I light curves using the 2003 version of the Wilson-Devinney code. XY LMi is a high fill-out, extreme mass ratio overcontact binary system with a mass ratio of q = 0.148 and a fill-out factor of f = 74.1%, suggesting that it is in the late evolutionary stage of late-type tidal-locked binary stars. As observed in other overcontact binary stars, evidence for the presence of two dark spots on both components is given. Based on our 19 epochs of eclipse times, we found that the orbital period of the overcontact binary is decreasing continuously at a rate of dP/dt = −1.67 × 10 −7 days yr −1 , which may be caused by mass transfer from the primary to the secondary and/or angular momentum loss via magnetic stellar wind. The decrease of the orbital period may result in the increase of the fill-out, and finally, it will evolve into a single rapid-rotation star when the fluid surface reaches the outer critical Roche lobe.

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A Catalog of 1022 Bright Contact Binary Stars

Cited by 93 publications

References 17 publications

Absolute-magnitude Calibration for W UMa-type Systems Based on Gaia Data*

Absolute-magnitude Calibration for W UMa-type Systems Based on Gaia Data*

A Model for Contact Binary EP Andromedae

High Fill-Out, Extreme Mass Ratio Overcontact Binary Systems. X. The Newly Discovered Binary Xy Leonis Minoris

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