Yazar "Bulut, I" seçeneğine göre listele

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    A new photometric study of CW Cephei and its apsidal motion
    (Wiley-V C H Verlag Gmbh, 2004) Erdem, A; Soydugan, E; Soydugan, F; Özdemir, S; Çiçek, C; Bulut, I; Demircan, O
    New photoelectric observations of the eccentric orbit binary CW Cephei have been carried out in B, V and R colours during the 2000 observing season at TUBITAK (The Scientific and Technical Research Council of Turkey) National Observatory. The light curves of the system were analyzed with a nonsynchronous rotation approach using the method of Wilson-Devinney in B, V and R bands, simultaneously. Especially, we used the R band to check for a third light in the solution as distinct from previous studies. But, the third light contribution in the light curves comes out to be almost negligible. In this study, the values of the longitude of periastron (omega) of the system's orbit found in the solutions of the light curves and radial velocity curves were collected and the variation of w with time was investigated. A new value of the apsidal motion velocity has been obtained as omega=0.0582 +/- 0.0011 (deg/cycle), corresponding to an apsidal period U=46 +/- 1 yr.
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    A photometric study of the recently discovered eclipsing binary V899 Herculis
    (E D P Sciences, 2002) Özdemir, S; Demircan, O; Erdem, A; Çiçek, C; Bulut, I; Soydugan, E; Soydugan, F
    The radial velocity and UBV light curves of V899 Her as found in the literature were studied for the first time to obtain the orbital parameters and geometry of the system. The solutions obtained by using the Wilson-Devinney code reveal an over-contact system with a fill-out factor of 23.7%. This solution is only possible with a large amount of third light (L-3 approximate to 0.68) which confirms the spectroscopic result obtained by Lu et al. (2001) who reported that the system of which V899 Her is a fainter component is triple, or even quadruple. The distance of the system found by using absolute parameters is comparable with the Hipparcos result.
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    Apsidal motion and photometric elements of the eccentric eclipsing binary V401 lacertae
    (Oxford Univ Press, 2006) Bulut, I; Demircan, O
    New UBV photometric observations of the recently discovered eccentric orbit binary V401 Lacertae were analyzed by using the Wilson-Devinney program. Seven new minimum times were estimated by using new observations. The analysis of the light Curves and all available minimum time,, has revealed that the system is detached, with the orbital eccentricity e = 0.1734 +/- 0.0003, the longitude of the periastron omega = 63 degrees 93 +/- 0 degrees 15, the rate of change of the longitude of periastron omega 0.degrees 0200 +/- 0.degrees 0024 cycle(-1), corresponding to ail apsidal motion period of U=96.2 +/- 11.4yr. The apsidal motion of the system has been confirmed by the significant difference oil the longitude of periastron (omega) obtained from two light Curves (Hipparcos and ourselves) in two different epochs.
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    Catalogue of Algol type binary stars
    (Edp Sciences S A, 2004) Budding, E; Erdem, A; Çiçek, C; Bulut, I; Soydugan, F; Soydugan, E; Bakis, V
    A catalogue of (411) Algol-type (semi-detached) binary stars is presented in the form of five separate tables of information. The catalogue has developed from an earlier version by including more recent information and an improved layout. A sixth table lists (1872) candidate Algols, about which fewer details are known at present. Some issues relating to the classification and interpretation of Algol-like binaries are also discussed.
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    Photometric study of the binary system V397 cephei
    (Oxford Univ Press, 2005) Bulut, I; Demircan, O; Budding, E; Erdem, A; Çiçek, C; Esenoglu, H; Soydugan, F
    The first ground-based UBV observations (2001, Inf. Bull. Variable Stars, 5129) of V397 Cep were analyzed by using the Wilson-Devinney method, and the results were compared with others in the literature. A consistent geometry with a photometric mass-ratio close to unity and an eccentric orbit of e similar or equal to 0.13 was found. The longitude of the periastron (omega) was found significantly different for two different light curves, which is strongly suggestive of an apsidal motion with a period of about 300 yr. This makes V397 Cep an important candidate for studies of apsidal motion.
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    The Light Curve Analysis of The Highly Eccentric Eclipsing Binary KIC 10296163
    (Amer Inst Physics, 2019) Cicek, C.; Bulut, A.; Bulut, I
    In this study, the analysis of the Kepler light curve of the eclipsing binary KIC 10296163 (Gaia DR2 2085670964017513856, R.A.(2000) = 19(h)564(m)40(s).07, DEC2000 = +47(0) 21'21 ''.97, m(R) = 13.43 mag) is presented. The light curve of the system shows a secondary minimum from a shifted phase 0.5 which indicates the ellipticity of the orbit. By using the PHOEBE program we analysed the light curve to achieve the orbital parameters of the system. The results of our analysis indicates a detached system where the orbit is highly eccentric (e = 0.357 +/- 0.003). Therefore, KIC 11858541 is a suitable candidate for apsidal motion studies.