Abstract
We performed the first light curve analysis of GW Leo and a new ephemeris is obtained for QT Boo. The light curve investigation also yields that the system GW Leo is a contact W UMa eclipsing binary with a photometric mass ratio of q = 0.44 ± 0.03, a fillout factor of f = 59.6%, and an inclination of 50.77° ± 0.09°. Due to the O’Connell effect which is known as asymmetries in the light curves’ maxima, a cold spot is employed along with the solution. The photometric and physical parameters of GW Leo were determined (e.g., Mh = 1.373 ± 0.024, Mc = 0.604 ± 0.027, Rh = 1.261 ± 0.041, Rc = 0.909 ± 0.039, and a(\({{R}_{ \odot }}\)) = 2.553 ± 0.004). According to the light curve solution results, we suggest that GW Leo is an A-type W UMa binary system. We also calculate the distance of GW Leo from the distance modulus formula as 483.5 ± 41 pc, which is in a good agreement to the quantity measured by the Gaia EDR3 using the binary systems' parallax. Moreover, the positions of their components on the H–R diagram are represented.
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REFERENCES
E. F. Guinan and D. H. Bradstreet, in Formation and Evolution of Low Mass Stars, Ed. by A. K. Dupree and M. T. V. T. Lago (Kluwer Academic, Dordrecht, 1988).
B. Paczyński, D. M. Szczygieł, B. Pilecki, and G. Pojmański, Mon. Not. R. Astron. Soc. 368, 1311 (2006).
C. Rinner, D. Starkey, C. Demeautis, S. Charbonnel, L. Bernasconi, and R. Behrend, Inform. Bull. Var. Stars 5428, 1 (2003).
A. V. Khruslov, Perem. Zvezdy Pril. 8 (52), 52 (2008).
F. Davoudi, A. Poro, F. Alicavus, A. Halavati, et al., Open Astron. 29, 72 (2020).
K. A. Collins, J. F. Kielkopf, K. G. Stassun, and F. V. Hessman, Astron. J. 153, 77 (2017).
A. Poro, F. Davoudi, F. Alicavus, E. M. Esmer, et al., arXiv: 2006.00528 (2020).
J. Salvatier, T.V. Wiecki, and C. Fonnesbeck, Peer J. Comput. Sci. 2, e55 (2016).
K. Hoňková, J. Juryšek, M. Lehký, L. Šmelcer, J. Trnka, M. Mašek, and M. Urbaník, Open Eur. J. Var. Stars 160, 1 (2013);
Open Eur. J. Var. Stars 165, 1(E) (2014).
K. Hoňková, J. Juryšek, M. Lehký, L. Šmelcer, et al., Open Eur. J. Var. Stars 168, 1 (2015).
J. Hübscher and P. B. Lehmann, Inform. Bull. Var. Stars 6149, 1 (2015).
J. Jurysek, K. Hoňková, L. Smelcer, M. Masek, et al., Open Eur. J. Var. Stars 179, 1 (2017).
J. Hübscher, Inform. Bull. Var. Stars 6157, 1 (2016).
R. H. Nelson, Inform. Bull. Var. Stars 6164, 1 (2016).
R. H. Nelson, Inform. Bull. Var. Stars 6195, 1 (2017).
R. H. Nelson, Inform. Bull. Var. Stars 6234, 1 (2018).
L. Pagel, Inform. Bull. Var. Stars 6244, 1 (2018).
D. Foreman-Mackey, D. W. Hogg, D. Lang, and J. Goodman, Publ. Astron. Soc. Pacif. 125, 306 (2013).
A. Prša and T. Zwitter, Astrophys. J. 628, 426 (2005).
L. B. Lucy, Zeitschr. Astrophys. 65, 89 (1967).
S. M. Rucinski, Acta Astron. 19, 245 (1969).
W. van Hamme, Astron. J. 106, 2096 (1993).
J. M. Wang, Astrophys. J. 434, 277 (1994).
E. F. Schlafly and D. P. Finkbeiner, Astrophys. J. 737, 103 (2011).
A. N. Cox, Allen’s Astrophysical Quantities (Springer, New York, 2000).
D. J. K. O’Connell, Mon. Not. R. Astron. Soc. 111, 642 (1951).
S. Qian, Mon. Not. R. Astron. Soc. 342, 1260 (2003).
Z. Kopal, Close Binary Systems (Springer, Berlin, 1959).
P. J. Flower, Astrophys. J. 469, 355 (1996).
S. B. Qian and Y. G. Yang, Astron. J. 128, 2430 (2004).
S. Zola, K. Gazeas, J. M. Kreiner, W. Ogloza, M. Siwak, D. Koziel-Wierzbowska, and M. Winiarski, Mon. Not. R. Astron. Soc. 408, 464 (2010).
ACKNOWLEDGMENTS
This manuscript was prepared by the International Occultation Timing Association Middle East section (IOTA/ME) as a scientific sponsor in the form of the APTO project, carried out between several observatories in Iran during 2019 and 2020. Thank Dr. Mohammad Fadaeian for his cooperation and for providing the Payame Noor Observatory of Ardabil University for this project. Also, thanks to PegahSadat MirshafieKhozani for making some corrections in the text. Furthermore, the authors would like to give great thanks to Dr. Fahri Alicavus for his consultations.
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Poro, A., Halavati, A., Lashgari, E. et al. The First Light Curve Solution of GW Leo and Refined Ephemeris of Two Contact Binary Systems. Astron. Rep. 65, 543–551 (2021). https://doi.org/10.1134/S1063772921070040
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DOI: https://doi.org/10.1134/S1063772921070040