The Ground-Based Photometric Observation and Light Curve Analyses of Eclipsing Binary KIC 12418816

Document Type : Research Paper


Department of Theoretical Physics and Astrophysics, Faculty of Physics, University of Tabriz, Tabriz, Iran


Here, the photometric CCD observations in RIAAM observatory and light curve analyses of KIC 12418816 are presented. For comparison, the Kepler long cadence (LC) photometric data was studied. The analyses of the recorded light curve in R-band filter and Kepler LC photometric data were performed by PHOEBE software by using the last version of Wilson-Devinney code. Initially, the search of mass ratio (q=m2/m1) of the binary system was done with finding the minimum chi-square value (cost function χ^2), which takes all sources of noise in to account. By photometric modeling which was obtained from our observations, the mass ratio was calculated as about 0.76. The results were comparable with modeling extracted from Kepler LC data which was obtained about 0.75. Our observations showed that the effective temperature (Teff) for primary and secondary stars were about 4421 and 4412 Kelvin, respectively. The similar results were obtained from Kepler LC data which were about 4463 and 4419 for primary and secondary stars, respectively. Our modeling demonstrated that we can introduce a spotted model with one spot on the primary component.


[1] Kallrath, J., Milone, E. F., & Wilson, R. 2009, Eclipsing binary stars: modeling and analysis, Springer.
[2] Xue-fu, L., Zhi-an, L., Leung, K., & Hui-song, T. 1990, ChJAA, 14, 167.
[3] Manzoori, D., Jassur, D. M., & Kermani, M. H. 2006, Ap&SS, 302, 145.
[4] Heidarnia, R., Ebadi, H., & Rooydargard, H. 2016, NEW ASTRON, 49, 28.
[5] Kasting, J. F., Whitmire, D. P., & Reynolds, R. T. 1993, ICARUS, 101, 108.
[6] Morton, T. D., Bryson, S. T., Coughlin, J. L., Rowe, J. F., Ravichandran, G., Petigura, E. A., Haas, M. R., & Batalha, N. M. 2016, ApJ, 822, 86.
[7] Monet, D. 1998, Bulletin of the American Astronomical Society.
[8] Watson, C., Henden, A., & Price, A. 2006, Sciences 25th Annual Symposium on Telescope Sciences.
[9] Coughlin, J. L., Lopez-Morales, M., Harrison, T. E., Ule, N., & Hoffman, D. I. 2011, AJ, 141, 78. [10] Armstrong, D. J., Gomez Maqueo Chew, Y., Faedi, F., and Pollacco, D. 2013, MNRAS, 437, 3473.
[11] Dal, H. A. & Ozdarcan, O. 2018, MNRAS, 474, 326.
[12] Prsa, A. & Zwitter, T. 2005, ApJ, 628, 426.
[13] Wilson, R. E. & Devinney, E. J. 1971, ApJ, 166, 605.
[14] Van Hamme, W. 1993, AJ, 106, 2096.
[15] Al-Naimiy, H. M. 1978, Ap&SS, 59, 3.
[16] Lucy, L. B. 1967, Z. Astrophys., 65, 89.
[17] Rucinski, S. 1969, ACTA ASTRONOM., 19, 245.
[18] Prsa, A., Batalha, N., Slawson, R. W., Doyle, L. R., Welsh, W. F., Orosz, J. A., Seager, S., Rucker, M., Mjaseth, K., Engle, S. G., et al. 2011, AJ, 141, 83.
[19] Slawson, R. W., Prsa, A., Welsh, W. F., Orosz, J. A., Rucker, M., Batalha, N., Doyle, L. R., Engle, S. G., Conroy, K., Coughlin, J., et al. 2011, AJ, 142, 160.
[20] Kirk, B., Conroy, K., Prsa, A., Abdul-Masih, M., Kochoska, A., MatijeviC, G., Hambleton, K., Barclay, T., Bloemen, S., Boyajian, T., et al. 2016, AJ, 151, 68.
[21] Devor, J., Charbonneau, D., ODonovan, F. T., Mandushev, G., & Torres, G. 2008, AJ, 135, 850.