Kısa Dönemli Değen Çift Yıldızın İlk Fotometrik Analizi: KIC3848042

Year 2022, , 1704 - 1719, 12.12.2022

Muhittin Şahan

https://doi.org/10.47495/okufbed.1062794

Abstract

Bu çalışma, Kepler görüş alanındaki 0.4114527 güns yörünge periyoduna sahip KIC3848042 W UMa tipi değen çift yıldız sisteminin ilk fotometrik analizlerini vermektedir. Fotometrik veriler Wilson-Devinney tabanlı PHOEBE kodu kullanılarak modellenmiştir. Fotometrik ışık eğrisi modeli sonuçlarından, sistemin en iyi çözümü için kütle oranları 0.473, yörüngesel eğikliğin 34.0, ikinci bileşenin sıcaklığı 6330K ve yüzey potansiyelleri (1=2) 2.8 olduğu bulunmuştur. Sonuçlar, KIC3848042'nin, %8.3’lik bir değme derecesi ile yakın düzeyde değen bir çift yıldız sistemi olduğunu göstermiştir. KIC3848042'nin mutlak parametreleri yörünge ekseni a = 3.120Rʘ; kütleler M1 = 1.633Mʘ ve M2 = 0.770Mʘ; yarıçapları R1 = 1.406Rʘ ve R2 = 0.998Rʘ; ışıma güçleri L1 = 2.967Lʘ ve L2 = 1.432Lʘ olarak hesaplanmıştır. Ayrıca, mutlak ve bolometrik parlaklıkları ise sırasıyla birinci bileşen için MV,1=3m.973 ve Mbol,1=3m.589 ve ikinci bileşen için MV,2 =4m.763 ve Mbol,2=4m.380 olarak hesaplanmıştır. Bileşenlerin kütle oranı ve birincil bileşenin kütleleri göz önüne alındığında, KIC3848042 ana kolda W-alt türü W-Uma örten yıldız sistemidir. Bileşenlerin tayf türleri yaklaşık olarak F7V olduğu görülmektedir.

Keywords

W UMa türü çift yıldız, Işık eğrisi analizi, Değen çift sistemler, KIC3848042

The First Photometric Analysis of Short-Period Contact Binary Star: KIC3848042

Abstract

This study gives the first photometric analysis of W Uma type eclipsing contact binary KIC3848042 with an orbital period of 0.4114527 days in the Kepler field of view. The photometric data were modeled using the PHOEBE code based on Wilson-Devinney program. From the results of light-curve modeling, it was found that the best solution for system was to be a mass ratio of 0.473, orbital inclination of 34.0, temperature of the secondary star of 6330K and surface potentials (1=2) of 2.8. The results showed that KIC3848042 is a near-contact binary with a fill-out factor of 8.3%. The absolute parameters of KIC3848042 were calculated as orbital axis a = 3.120Rʘ; masses M1 = 1.633Mʘ and M2 = 0.770Mʘ; radii R1 = 1.406Rʘ and R2 = 0.998Rʘ; luminosities L1 = 2.967Lʘ and L2 = 1.432Lʘ. Moreover, their absolute and bolometric magnitudes were calculated to be MV,1=3m.973 and Mbol,1=3m.589 for the primary component and Mbol,2=4m.380 and MV,2=4 m.763, respectively. Considering the mass ratio and masses of the primary component, KIC3848042 is an W-subtype W-UMa eclipsing binary system in main sequence. The spectral types of the components seem to be approximately F7V.

Keywords

UMa type binary stars, Light curve analysis, Contact binary systems, KIC3848042

References

• Abdul-Masih M., Prsa A., Conroy K., ve ark., Kepler eclipsıng binary stars. VIII. identification of false positive eclipsing binaries and re-extraction of new light curves, The Astronomical Journal, 2016; 151 (4): 1-10.
• Bradstreet DH., Steelman DP., Binary Maker 3, Light Curve Synthesis Program User Manual, Contact Software, 725 Stanbridge St., Norristown, PA, 2004; 19401-5505.
• Binnendijk, L., The orbital elements of W Ursae Majoris systems. Vistas in Astronomy, 1970; 12: 217-256.
• Caldwell DA., Kolodziejczak JJ., Van Cleve JE., ve ark., Instrument Performance in Kepler’s First Months, The Astrophysical Journal Letters, 2010; 713 (2): L92–L96
• Csizmadia SZ., Klagyivik P., On the properties of contact binary stars, Astronomy and Astrophysics, 2004; 426 (3): 1001-1005. Cox AN., Allen's astrophysical quantities, fourth edition, Theoretical Division, Los Alamos National Laboratory MS B288, P.O. Box 1663, Los Alamos, NM 87545, USA, 2002.
• Dimitrov DP., Kjurkchieva DP., Ultrashort-period main-sequence eclipsing systems: new observations and light-curve solutions of six NSVS binaries, Monthly Notices of the Royal Astronomical Society, 2015; 448 (3): 2890-2899.
• Gao X., Li K., Gao X., Liu Y., The first photometric analysis of the totally eclipsing contact binary V811 Cep, Research in Astronomy and Astrophysics, 2021; 21(8):193-203.
• Gazeas KD., Niarchos PG., Masses and angular momenta of contact binary stars, Monthly Notices of the Royal Astronomical Society: Letters, 2006; 370 (1): L29-L32.
• Gazeas K., Stepien K., Angular momentum and mass evolution of contact binaries, Monthly Notices of the Royal Astronomical Society, 2008; 390: 1577–1586.
• Gürol B., Bradstreet DH., Okan A., Absolute and geometric parameters of the W UMa type contact binary V546 And, New Astronomy, 2015; 36:100–109.
• Hilditch RW., King D. J., McFarlane T. M., The evolutionary state of contact and near-contact binary stars, Monthly Notices of the Royal Astronomical Society, 1988; 231 (2): 341–352.
• Hilditch RW., The evolution of binary stars into contact states, Space Science Reviews1989; 50: 289-297.
• Joshi YC., Jagirdar R., Joshi S., Photometric studies of two W UMa type variables in the field of distant open cluster NGC 6866, Research in Astronomy and Astrophysics, 2016; 16 (4): 63 (10 sayfa).
• Koch DG., Borucki WJ., Basri G., ve ark., Fırst Kepler results on Rr Lyrae stars, The Astrophysical Journal Letters, 2010; 713: L198–L203.
• Kolenberg K., Szabo R., Kurtz DW., ve ark., Fırst Kepler results on Rr Lyrae stars, The Astrophysical Journal Letters, 2010; 713: L198–L203. Li XZ., Liua L, KIC 4762887: A near-contact binary or an ellipsoidal variable star? New Astronomy, 2021; 84: (101539), 1-4.
• Lucy LB., the structure of contact binaries, Astrophysical Journal, 1968; 151: 1123-1135.
• Maceroni C., Milano L., Russo G., General properties of W Ursae Majoris systems, Monthly Notices of the Royal Astronomical, 1985, Society, 217: 843-866.
• Matijevic G., Prsa A., Orosz JA., Welsh WF., Bloemen S., Barclay T., Kepler eclipsing binary stars. III. classification of kepler eclipsing binary light curves with locally linear embedding, Astronomical Journal, 2012; 143(5):123, 1-6.
• O’Connell DJK., The so-called periastron effect in close eclipsing binaries, Riverview College Observatory publications, 1951; 2: 85-100.
• Pietrzynski G., Graczyk D., Gallenne A., ve ark., A distance to the Large Magellanic Cloud that is precise to one per cent, Nature, 2019; 567: 200-203.
• Prsa A., Batalha N., Slawson RW., ve ark., Kepler eclipsing binary stars. I. catalog and principal characterization of 1879 eclipsing binaries in the first data release. The Astronomical Journal, 2011; 141 (3): 1-16.
• Prsa A., Zwitter T., A computational guide to physics of eclipsing binaries. I. demonstrations and perspectives. The Astrophysical Journal, 2005; 628 (1): 426-438.
• Prsa A., PHOEBE Scientific Reference PHOEBE version 0.30, Villanova Unıversity College of Arts and Scıences, Dept. of Astronomy And Astrophysıcs, 2011.
• Prsa A., Batalha N., Slawson RW., Doyle LR., ve ark., Kepler eclipsing binary stars. I. catalog and principal characterization of 1879 eclipsing binaries in the first data release. The Astronomical Journal, 2011; 141 (3): 1-16.
• Rucinski SM., Contact binaries, ınstrumentation and research programmes for small telescopes, Proceedings of the 118th. Symposium of the International Astronomical Union (IAUS), held in rch, New Zealand, December 2-6, 1985. Editors, J.B. Hearnshaw, P.L. Cottrell; Publishers, D. Reidel Publishing Company, Dordrecht, Holland. Sold and distributed in the U.S.A. and Canada by Kluwer Academic Publishers, Norwell, Massachusetts, QB88 .I583, 1986. 159-172.
• Skelton PL., Smith DP., Modelling of W UMa-type variable stars, South African Journal of Science, 2009; 105:120-126.
• Slawson RW., Prša A., Welsh WF., Orosz JA., ve ark., Kepler eclipsing binary stars. II. 2165 eclipsing binaries in the second data release, The Astronomical Journal, 2011; 142:160 (14 sayfa).
• Terrell D., Gross J., Cooney Jr WR., A Bv Rc Ic survey of W Ursae Majoris binaries, The Astronomical Journal, 2012; 143:99 (7 sayfa) .
• Thompson SE., Fraquelli D., van Cleve JE., Caldwell DA., Kepler: A Search for Terrestrial Planets, Kepler Archive Manual, KDMC-10008-006, Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, 2016.
• Torres G., Vaz LPR., Lacy CHS., Claret A., Absolute properties of the eclipsing binary system aq serpentis: A stringent test of convective core overshooting in stellar evolution models, The Astronomical Journal, 2014; 147 (36): 1-11.
• Van Cleve JE., Caldwell DA., Haas MR., Howell SB., Kepler: A search for terrestrial planets, Kepler Instrument Handbook, KSCI-19033-002, NASA Ames Research Center, Moffett Field, CA 94035-1000, 2016.
• Van Hamme W., New limb-darkening coefficients for modeling binary star light curves, Astronomical Journal, 1993; 106 (5): 2096-2117.
• Wadhwa SS., Photometric analysis of southern contact binary stars, part 1: GZ Pup, AV Pup and II Aps. Astrophys. Space Sci., 2005; 300: 289-296.
• Wang JM, The Thermal relaxation oscillation states of contact binaries, Astrophysical Journal, 1994; 434: 277-282.
• Wesselink AJ., Surface Brightnesses in the U, B, V system with applications of Mυ and dimensions of stars, Monthly Notices of the Royal Astronomical Society, 1969; 144 (3):2 97–311.
• Wilson RE., Devinney EJ., Realization of accurate close-binary light curves: application to MR Cygni. Astrophysical Journal, 1971; 166: 605-619.
• Wilson RE., Accuracy and efficiency in the binary star reflection effect, Astrophysical Journal, 1990; 356, 613-662.
• Wilson RE., Eclipsing binary solutions in physical units and direct distance estimation, The Astrophysical Journal, 2008; 672 (1): 575-589.
• Yıldız M., Doğan T., On the origin ofW UMa type contact binaries – a new method for computation of initial masses, Monthly Notices of the Royal Astronomical, 2013; 430:2029-2038.