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Light-Time Effect and Mass Transfer in the Triple Star SW Lyncis
Published 1999-06-01“…In this paper all the photoelectric times of minimum for the triple star SW Lyn have been analyzed in terms of light-time e ect due to the third-body and secular period decreases induced by mass transfer process. …”
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Light-Time Effects in Two Eclipsing Binaries V343 AQL and CX AQR
Published 2005-06-01“…Possible causes of secular period variations for two systems were discussed. …”
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The BV Photometry of the RR Lyrae Star, BH Ursae Majoris: Light Curves and Period Study
Published 2011-06-01“…We also analyzed all of the available unanalyzed minimum timings and found for the first time that the period of BH UMa has varied dramatically in at least three independent sinusoidal ways superposed on a secularly downward parabola over 66 years. The secular period decreasing rate was obtained as 6.d684 × 10-8 y-1, corresponding to -0.58 s/century. …”
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Period Change of the Contact Binary AH Tauri
Published 2004-12-01“…It is found that the orbital period of AH Tau has varied in a cyclic way superposed on a secular period decrease. The rate of the secular period decrease is calculated to be 1^s.04 per century, implying that a mass of about 3.8 × 10-8 M⊙/yr from the more massive primary flows into the secondary if a conservative mass transfer is assumed. …”
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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
Published 2019-12-01“…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. …”
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V700 Cygni: A Dynamically Active W UMa-type Binary Star II
Published 2012-06-01“…The small secular period increase is interpreted as a combination of both angular momentum loss (due to magnetic braking) and mass-transfer from the less massive component to the more massive component. …”
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WZ Cephei: A Dynamically Active W UMa-Type Binary Star
Published 2011-09-01“…It was found that the orbital period of the system has complexly varied in two cyclical components superposed on a secularly downward parabola over about 80y. The downward parabola, corresponding to a secular period decrease of -9.d97 × 10-8 y-1, is most probably produced by the action of both angular momentum loss (AML) due to magnetic braking and mass-transfer from the massive primary component to the secondary. …”
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CCD Photometric Observations and Light Curve Synthesis of the Near-Contact Binary XZ Canis Minoris
Published 2009-06-01“…An intensive period study with all published timings, including ours, confirms that the period of XZ CMi has varied in a cyclic period variation superposed on a secular period decrease over last 70 years. Assuming the cyclic change of period to occur by a light-time effect due to a third-body, the light-time orbit with a semi-amplitude of 0.0056d, a period of 29y and an eccentricity of 0.71 was calculated. …”
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A Period Study of the Near Contact Binary EG Cep
Published 2006-06-01“…It was found that the orbital period have varied in a cyclical way superposed on an upward parabola. A secular period increase of 3.22 times 10^{-8} d/y was calculated. …”
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Period Change of W UMa Type Contact Binary AB And
Published 1997-12-01“…From the quadratic coefficient of this orbital elements, we calculated the secular variation of 0.73 seconds, and from the sinusoidal term, the period variation turned out to be 62.9 years with amplitude of 0d.024. …”
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On the Period Change of the Contact Binary GW Cephei
Published 2010-06-01“…The upward parabolic O-C diagram corresponding to a secular period increase of about 4.12 × 10^(-8) d/yr was interpreted as mass being transferred from the lesser to more massive component. …”
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