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

Year 2022, Volume: 12 Issue: 2, 735 - 751, 01.06.2022

Muhittin Şahan

https://doi.org/10.21597/jist.1054191

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.

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

References

• Binnendijk, L., 1970. The orbital elements of W Ursae Majoris systems, Vistas in Astronomy, 12: 217-226.
• Bradstreet DH, 2005. BINARY MAKER 3.0, Contact Software, 725 Stanbridge Street, Norristown, PA 19401–5505, USA. http://www.binarymaker.com/
• Conroy KE, Prsa A, Stassun, Orosz JA, Fabrycky DC, Welsh WF, 2014. Kepler eclipsing binary stars. IV. precise eclipse times for close binaries and identification of candidate three-body systems. The Astronomical Journal 147: 45 (15 sayfa).
• Csizmadia SZ, Klagyivik P, 2004. On the properties of contact binary stars, Astronomy and Astrophysics, 426 (3): 1001-1005.
• Deb S., Singh, H. P. 2011. Physical parameters of 62 eclipsing binary stars using the all sky automated survey-3 data – I. Monthly Notices of the Royal Astronomical Society, 412 (3): 1787-1803.
• Dimitrov DP, Kjurkchieva DP, 2015. Ultrashort-period main-sequence eclipsing systems: new observations and light-curve solutions of six NSVS binaries, Monthly Notices of the Royal Astronomical Society, 448 (3): 2890-2899.
• Eggen, O. J., 1967, Contact binaries, II., Memoirs of the Royal Astronomical Society, 70: 111-164.
• Gazeas K, Stepien K, 2008. Angular momentum and mass evolution of contact binaries, Monthly Notices of the Royal Astronomical Society, 390: 1577–1586.
• Gazeas KD, Niarchos PG, 2006. Masses and angular momenta of contact binary stars, Monthly Notices of the Royal Astronomical Society, 370: L29–L32.
• Joshi YC, Jagirdar R, Joshi S, 2016. Photometric studies of two W UMa type variables in the field of distant open cluster NGC 6866, Research in Astronomy and Astrophysics 16 (4), 63 (10pp).
• Kirk B, Conroy K, Prsa A, Abdul-Masih M, Kochoska A, Matijevič G, Hambleton K, Barclay T, Bloemen S, Boyajian T, Doyle LR, Fulton BJ, Hoekstra AJ, ve ark., 2016. Kepler eclipsing binary stars. VII. the catalog of eclipsing binaries found in the entire kepler data set. The Astronomical Journal, 151: 68 (21 sayfa).
• Kolenberg K, Szabo R, Kurtz DW, Gilliland RL, Christensen-Dalsgaard J, Kjeldsen H, Brown TM, Benko JM, Chadid M, Derekas A, Di Criscienzo M, Guggenberger E, Kinemuchi K, Kunder A, Kollath Z, Kopacki G, Moskalik P, Nemec JM, Nusp J, Silvotti R, Suran MD, Borucki WJ, Koch D, Jenkins JM, 2010. Fırst Kepler results on Rr Lyrae stars, The Astrophysical Journal Letters, 713: L198–L203.
• Li XZ, Liua L, 2021. KIC 4762887: A near-contact binary or an ellipsoidal variable star? New Astronomy 84: (101539), 1-4.
• Lucy LB, 1967. Gravity-darkening for stars with convective envelopes. Zeitschrift für Astrophysik, 65: 89-92.
• Lucy LB, 1968. The Structure of Contact Binaries. Astrophysical Journal, 151: 1123-1135.
• Lucy LB, Wilson RE, 1979. Observational tests of theories of contact binaries Astrophysical Journal, Part 1, 231:502-513.
• Maceroni C, Milano L, Russo, G, 1983. Determination of parameters of W UMa systems. IV - BV Dra, BW Dra, EM Lac, SW Lac, Astronomy and Astrophysics Supplement Series, 51: 435-442.
• Mochnacki SW, 1981. Contact binary stars, Journal: Astrophysical Journal, 245: 650-670.
• O’Connell DJK, 1951. The so-called periastron effect in close eclipsing binaries, Riverview College Observatory publications, 2: 85-100.
• Pecaut MJ; Mamajek EE, 2013. Intrinsic colors, temperatures, and bolometric corrections of pre-main-sequence stars, The Astrophysical Journal Supplement, 208 (1): 9, (22 sayfa).
• Prsa A, 2011. PHOEBE Scientific Reference PHOEBE version 0.30, Villanova Unıversity College of Arts and Sciences, Dept. of Astronomy And Astrophysics.
• Prsa A, Batalha N, Slawson RW, Doyle LR, Welsh WF, Orosz JA, Seager S, Rucker M, Mjaseth K, Engle SG, Conroy K, Jenkins J, Caldwell D, Koch D, Borucki W, 2011. Kepler eclipsing binary stars. I. catalog and principal characterization of 1879 eclipsing binaries in the first data release. The Astronomical Journal, 141 (3): 1-16.
• Prsa A, Zwitter T, 2005. A Computational guide to physics of eclipsing binaries. I. demonstrations and perspectives. The Astrophysical Journal, 628 (1): 426-438.
• Rucinski SM, 1969. The proximity effects in close binary systems. II. The bolometric reflection effect for stars with deep convective envelopes, Acta Astronomica, 19: 245-255.
• Rucinski SM, 1994. Mv=Mv(logP , logTe) Calibrations for W Ursae Majoris Systems, Publications of the Astronomical Society of the Pacific, 106: 462-471.
• Rucinski SM, Duerbeck HW, 1997. Absolute magnitude calibration for the W UMa-type systems based on Hipparcos data, Publications of the Astronomical Society of the Pacific (PASP), 109 (109): 1340-1350.
• Skelton PL, Smith DP, 2009. Modelling of W UMa-type variable stars, South African Journal of Science, 105:120-126.
• Slawson RW, Prša A, Welsh WF, Orosz JA, Rucker M, Batalha N, Doyle LR, Engle SG, Conroy K, Coughlin J, Gregg TA, Fetherolf T, Short DR, Windmiller G, Fabrycky DC, Howell SB, Jenkins JM, Uddin K, Mullally F, Seader SE, Thompson SE, Sanderfer DT, Borucki W, Koch D, 2011. Kepler eclipsing binary stars. II. 2165 eclipsing binaries in the second data release, The Astronomical Journal, 142:160 (14 sayfa).
• Terrell D, 2001. Eclipsing Binary Stars: Past, Present, and Future, Journal of American Association of Variable Star Observer (JAVSO), 30: (15 sayfa).
• Terrell D, Gross J., Cooney Jr WR, 2012. A Bv Rc Ic Survey Of W Ursae Majoris Binaries, The Astronomical Journal, 143:99 (7 sayfa) .
• Van Hamme W, 1993. New limb-darkening coefficients for modeling binary star light curves. Astronomical Journal, 106 (5): 2096-2117.
• Wadhwa SS, 2005. Photometric analysis of southern contact binary stars, part 1: GZ Pup, AV Pup and II Aps. Astrophys. Space Sci. 300: 289–296.
• Wang JM, 1994. The Thermal relaxation oscillation states of contact binaries, Astrophysical Journal, 434: 277-282.
• Wesselink A J, 1969. Surface Brightnesses in the U, B, V system with applications of Mυ and dimensions of stars, Monthly Notices of the Royal Astronomical Society, 144 (3):297–311.
• Wilson RE, 1990. Accuracy and efficiency in the binary star reflection effect, Astrophysical Journal, 356, 613.
• Wilson RE, 1994. Binary-star light-curve models, Publications of the Astronomical Society of the Pacific, 106 (703): 921-94.
• Wilson RE, Devinney EJ, 1971. Realization of accurate close-binary light curves: application to MR Cygni. Astrophysical Journal, 166: 605-619.