UY Ursae Majoris: A W-subtype W UMa system with a small mass ratio

YL, Yang; QY, Liu; Leung, K. C.

doi:10.1051/0004-6361:20010261

Cited by 14 publications

(2 citation statements)

References 8 publications

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“…No O'Connell effect was found in our light curves with a long-duration totality (approximately 43 m ) at secondary eclipse. The physical parameters derived from the light curve synthesis are totally different from ones suggested by Yang et al (2001): UY UMa is an A-subtype over-contact binary with a low mass ratio of q = 0.21, a high inclination of 81˚.4, a small temperature difference of ∆T = 18˚, a large fill-out factor of f = 0.61, and a third light of approximately 10% of the total systemic light. The absolute dimensions of the system were determined as follows: M 1 = 1.15 M ⊙ , M 2 = 0.24 M ⊙ , R 1 = 1.34 R ⊙ , R 2 = 0.70 R ⊙ , L 1 = 1.95 L ⊙ , and L 2 = 0.52 L ⊙ .…”

Section: Discussionmentioning

confidence: 84%

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UY Ursae Majoris: An A-Subtype W UMa System with a Very Large Fill-Out Factor and an Extreme Mass Ratio

Kim¹,

Song²,

Park³

et al. 2019

Journal of Astronomy and Space Sciences

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We present new BVRI light curves of UY UMa with no O’Connell effect and a flat bottom secondary eclipse. Light curve synthesis with the Wilson-Devinney code gives a new solution, which is quite different from the previous study: UY UMa is an A-subtype over-contact binary with a small mass ratio of q = 0.21, a high inclination of 81°.4, a small temperature difference of ΔT = 18°, a large fill-out factor of f = 0.61, and a third light of approximately 10% of the total systemic light. The absolute dimensions were newly determined. Seventeen new times of minimum light have been calculated from our observations. The period study indicates that the orbital period has intricately varied in a secular period increase in which two cyclical terms with periods of 12y.0 and 46y.3 are superposed. The secular period increase was interpreted to be due to a conservative mass transfer of 2.68 × 10–8 M⊙/yr from the less massive to the more massive star. The cyclical components are discussed in terms of double-light time contributions from two additional bound stars. The statistical relations of Yang & Qian (2015) among the physical parameters of 45 deep, low mass ratio contact binaries were revisited by using the physical parameters of UY UMa and 25 Kepler contact binaries provided by Şenavci et al. (2016).

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Section: Discussionmentioning

confidence: 84%

“…'C' and 'K' denote the comparison (UCAC4 727-048577) and check (UCAC4 726-049111) stars, respectively. 'CY' denotes the comparison star (UCAC4 726-049104) used by Yang et al (2001).…”

Section: Observationsmentioning

confidence: 99%

UY Ursae Majoris: An A-Subtype W UMa System with a Very Large Fill-Out Factor and an Extreme Mass Ratio

Kim¹,

Song²,

Park³

et al. 2019

Journal of Astronomy and Space Sciences

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First light curve and period study of LO Andromedae

Gürol¹,

Müyesseroğlu

2005

Astron. Nachr.

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Abstract. New BV light curves and times of minimum light for the short period W UMa system LO And were analyzed to derive the preliminary physical parameters of the system. The light curves were obtained at Ankara University Observatory during 5 nights in 2003. A new ephemeris is determined for the times of primary minimum. The analysis of the light curves is made using the Wilson-Devinney 2003 code. The present solution reveals that LO And has a photometric mass ratio q = 0.371 and is an A-type contact binary. The period of the system is still increasing, which can be attributed to light-time effect and mass transfer between the components. With the assumption of coplanar orbit of the third body the revealed mass is M3 = 0.21M . If the period change dP/dt = 0.0212 sec/yr is caused only by the mass transfer between components (from the lighter component to the heavier) the calculated mass transfer rate is dm/dt = 1.682 × 10 −7 M /yr. The absolute radii and masses estimated for the components, based on our photometric solution and the absolute parameters of the systems which have nearly same period are R1 = 1.30R , R2 = 0.85R , M1 = 1.31M , M2 = 0.49M respectively for the primary and secondary components.

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The First Photometric Analyses Of Four New Discovered Ew-Type Eclipsing Binaries: GSC 1848-1264, GSC 0804-0118, GSC 0619-0232 And GSC 2936-0478

Gonzalez-Rojas³

et al. 2005

Astrophys Space Sci

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Photometric solutions of four new discovered W UMa-type binaries were carried out for the first time by using the 2003 version of the W-D program. It is discovered that all of the four systems are over-contact binaries. Two binaries, GSC 0804-0118 and GSC 2936-0478, are of A-subtype, while two other binaries, GSC 1848-1264 and GSC 0619-0232, are of W-subtype. From our solutions, the fundamental orbital and physical parameters were determined. For GSC 0619-0232 and GSC 2936-0478, the asymmetries of the light curves (i.e., the O'Connell effect) were explained by the presence of dark spots on the more massive components. Our photometric results reveal that GSC 0619-0232 is an important and interesting system. It is a W-type over-contact binary with a low mass ratio of q = 0.100 and a high over-contact degree of f = 93.4%, which suggests that GSC 0619-0232 may be evolved into a single rapid-rotating star.

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UY Ursae Majoris: A W-subtype W UMa system with a small mass ratio

Cited by 14 publications

References 8 publications

UY Ursae Majoris: An A-Subtype W UMa System with a Very Large Fill-Out Factor and an Extreme Mass Ratio

UY Ursae Majoris: An A-Subtype W UMa System with a Very Large Fill-Out Factor and an Extreme Mass Ratio

First light curve and period study of LO Andromedae

The First Photometric Analyses Of Four New Discovered Ew-Type Eclipsing Binaries: GSC 1848-1264, GSC 0804-0118, GSC 0619-0232 And GSC 2936-0478

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