Photometric Analysis and Period Investigation of the EW Type Eclipsing Binary V441 Lac

New light curves and photometric solutions of FP Lyn, FV CVn and V354 UMa are presented. It is found that these three systems are W-subtype shallow contact binaries. In addition, it is obvious that the light curves of FP Lyn and V354 UMa are asymmetric. Therefore, a hot spot was added on the primary star of FP Lyn and a dark spot was added on the secondary star of V354 UMa. At the same time, we added a third light to the photometric solution of FP Lyn for the final result. The obtained mass ratios and fill-out factors are q = 1.153 and f = 13.4% for FP Lyn, q = 1.075 and f = 4.6% for FV CVn, q = 3.623 and f = 10.7% for V354 UMa. The investigations of orbital period of these three systems indicate that the periods are variable. FP Lyn and V354 UMa were discovered existing the secular increase component with a rate of dp/dt = 4.19 × 10 −7 d yr −1 and dp/dt = 7.70 × 10 −7 d yr −1 respectively, which are feasibly caused by the conservative mass transfer from the less massive component to the more massive component. In addition, some variable components were discovered for FV CVn, which is a rate of dp/dt = −1.13 × 10 −6 d yr −1 accompanied by a cyclic oscillation with amplitude and period of 0.0069 days and 10.65 yr. The most likely explanation for the long-term decrease is angular momentum loss. And the existence of an additional component is the most plausible explanation for the periodic variation.

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Magnetic Activity and Period Variation Studies of the Short-period Eclipsing Binaries. III. V1175 Her, NSVS 2669503, and 1SWASP J133417.80+394314.4

Lu¹,

Michel

Zhang

et al. 2018

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New multi-band CCD light curves of three binaries W UMa-type V1175 Her, NSVS 2669503, and 1SWASP J133417.80+394314.4 are presented. Spectroscopic data for V1175 Her and NSVS 2669503 show that their spectral types are G7V and K4V, respectively. Photometric solutions of these three objects were obtained with the help of the Wilson–Devinney program. We find that V1175 Her is a semi-detached binary star with a hot spot located on the secondary component, while NSVS 2669503 and 1SWASP J133417.80+394314.4 are contact eclipsing binaries with contact factors of f = 1.070 ± 0.002% and f = 21.250 ± 0.005%, respectively. Moreover, we found that the orbital period of V1175 Her is increasing at a rate of (+3.1 ± 0.1) × 10−7 days yr−1. This increase may be attributed to a mass-transfer rate from the primary to the secondary component. Finally, we discuss the evolutionary stage of the component stars of these three systems.

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Photometric Analysis and Period Investigation of the EW Type Eclipsing Binary V441 Lac

Cited by 3 publications

References 25 publications

Investigative study of five low mass ratio semi-detached binaries

Investigative study of five low mass ratio semi-detached binaries

Photometric investigation and orbital period analyses of the WUMa binaries FP Lyn, FV CVn and V354 UMa

Magnetic Activity and Period Variation Studies of the Short-period Eclipsing Binaries. III. V1175 Her, NSVS 2669503, and 1SWASP J133417.80+394314.4

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