Photometric Analysis of Three W UMa Type Contact Binaries (KIC3732732, KIC3936357 and KIC10802917) from The Kepler Catalogue

Abstract

This study presents the results of photometric studies of three previously unstudied short-period (0d.27 < P < 0d.39) W UMa type eclipsing binary systems from the Kepler Catalogue: KIC3732732, KIC3936357 and KIC10802917. The photometric light curves were analyzed using the PHOEBE modeling package program based on the Wilson-Devinney (WD) (with Mode 3). From photometric light curve analyses, the mass ratios (q), inclination angles (i), temperature of the secondary (T2), potentials (1 = 2), fill-out factors (f) and spots on the secondary components were determined. The best solution for systems were found to be q = 0.5, i = 57.0, T2 = 5966 K,  = 2.8 and f = 25.4%, for KIC3732732, q = 0.41, i = 76.5, T2 = 5940 K,  = 2.6 and f = 39.4%, for KIC3936357, q = 0.48, i = 82.0, T2 = 5080 K,  = 2.79 and f = 16.4% for KIC10802917. The absolute parameters of the systems’ primary and secondary components have also been derived to be M1 = 1.575 M☉, M2 = 0.785 M☉, R1 = 1.383 Rʘ, R2 = 1.019 R☉, a = 3.024 R☉, L1 = 2.143 L☉ and L2 = 1.180 L☉ for KIC3732732 system, M1 = 1.602 M☉, M2 = 0.654 M☉, R1 = 1.373 Rʘ, R2 = 0.938 Rʘ, a = 2.842 R☉, L1 = 2.093 L☉ and L2 = 0.982 L☉ for KIC3936357 system and M1 = 1.078 M☉, M2 = 0.516 M☉, R1 = 0.940 R☉, R2 = 0.675 R☉, a = 2.067 R☉, L1 = 0.470 L☉ and L2 = 0.272 L☉ for KIC10802917 system, respectively. The mass ratios and Roche Lobe fill out factors along with temperature of (T2 > T1) suggest that three binary systems are W-subtype over-contact W UMa binary systems. Considering the temperatures of the components, spectral types of KIC3732732, KIC3936357 and KIC10802917 were estimated as G0V, G0V and K2V, respectively.

Keywords

• UMa type binary stars
• Light curve analysis
• Contact binary systems
• KIC3732732
• KIC3936357
• KIC10802917

Kepler Kataloğundan Seçilen Üç W UMa Tipi Değen Çift Yıldızın (KIC3732732, KIC3936357 ve KIC10802917) Işık Eğrisi Analizleri

Abstract

Bu çalışma, Kepler kataloğundan seçilen daha önce çalışılmamış kısa dönemli (0g.27 < P < 0g.39) KIC3732732, KIC3936357 ve KIC10802917 W UMa tipi örten çift yıldız sistemlerinin fotometrik araştırma sonuçlarını vermektedir. Wilson-Devinney (WD) tabanlı (Mod 3) PHOEBE modelleme paket programı kullanılarak sistemlerin fotometrik ışık eğrileri analiz edilmiştir. Fotometrik ışık eğrisi analizlerinden kütle oranları (q), eğim açıları (i), ikinci bileşenin sıcaklığı (T2), potansiyelleri (1 = 2), Roche lobu doldurma faktörleri (f) ve ikincil bileşenlerinin üzerindeki lekeler belirlenmiştir. Sistemler için en iyi çözümlerin KIC3732732 için q = 0.5, i = 57.0, T2 = 5966 K,  = 2.8 ve f = %25.4, KIC3936357 için q = 0.41, i = 76.5, T2 = 5940 K,  = 2.6 ve f = %39.4 ve KIC10802917 için q = 0.48, i = 82.0, T2 = 5080 K,  = 2.79 ve f = %16.4 olduğu bulunmuştur. Sistemlerin birinci ve ikinci bileşenlerin mutlak parametreleri ise sırasıyla, KIC3732732 sistemi için M1 = 1.575 Mʘ, M2 = 0.785 Mʘ, R1 = 1.383 Rʘ, R2 = 1.019 Rʘ, a = 3.024 Rʘ, L1 = 2.143 Lʘ ve L2 = 1.180 Lʘ, KIC3936357 sistemi için M1 = 1.602 Mʘ, M2 = 0.654 Mʘ, R1 = 1.373 Rʘ, R2 = 0.938 Rʘ, a = 2.842 Rʘ, L1 = 2.093 Lʘ ve L2 = 0.982 Lʘ ve KIC10802917 sistemi için M1 = 1.078 Mʘ, M2 = 0.516 Mʘ, R1 = 0.940 Rʘ, R2 = 0.675 Rʘ, a = 2.067 Rʘ, L1 = 0.470 Lʘ ve L2 = 0.272 Lʘ olarak belirlenmiştir. Kütle oranlarına, Roche Lobu doldurma faktörlerine ve sıcaklıklarına (T2 > T1) göre her üç çift yıldız sisteminin aşırı değen W UMa ikili sistemlerinin W-alt türü oldukları görülmektedir. Bileşenlerin sıcaklıklarına göre KIC3732732, KIC3936357 ve KIC10802917 sistemlerinin sırasıyla G0V, G0V ve K2V tayf türünden oldukları tahmin edilmiştir.

Keywords

• W UMa türü çift yıldız
• Işık eğrisi analizi
• Değen çift sistemler
• KIC3732732
• KIC3936357
• KIC10802917

Thanks

Bu çalışma, Kepler uzay teleskobuyla gözlenen ve Villanova Üniversitesi tarafından hazırlanmış olan Kepler Örten Çift Yıldız Kataloğundan (Kepler Eclipsing Binary Catalogue: KEBC, http://keplerebs.villanova.edu/) elde edilen veriler kullanılmıştır.

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