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Öğe A comprehensive photometric study of the Algol-type eclipsing binary: BG Pegasi(Elsevier Science Bv, 2011) Soydugan, Esin; Soydugan, Faruk; Senyuz, T.; Puskullu, C.; Demircan, O.This study presents new photometric observations of classical Algol type binary BC Peg with a delta Scuti component The light curve modeling was provided with the physical parameters of the component stars in the BC Peg system for the first time After modeling light curves in B and V filters, the eclipse and proximity effects were removed from the light curve to analyze intrinsic variations caused by the hotter component of the system Frequency analysis of the residuals light represents the multi-mode pulsation of the more massive component of the BC Peg system at periods of 0.039 and 0 047 clays Two frequencies could be associated with non-radial (l = 2) modes The total amplitude of the pulsational variability in the V light curve was found to be about 0 045 mag The long-term orbital period variation of the system was also investigated for the first time The O-C analysis indicates periodic variation superimposed on a downward parabola The secular period variation means that the orbital period of the system is decreasing at a rate of -5 5 seconds per century, probably due to the magnetic activity of the cooler component. The tilted sinusoidal O-C variation may be caused by the gravitational effect of an unseen component around the system (C) 2010 Elsevier B V All rights reservedÖğe New Discovered Pulsational Components in Algol Type Binaries and their Positions on the plane of Porb-Ppuls(Astronomical Soc Pacific, 2010) Soydugan, Esin; Soydugan, Faruk; Senyuz, T.; Tuysuz, M.; Bakis, V.; Bilir, S.; Cicek, C.In this study, eclipsing binaries located in the delta Scuti region of the instability strip were chosen from the list of candidate eclipsing binary systems with delta Scuti components. These candidate systems were photometrically observed and some of them were announced to be new Algol-type binaries with delta Scuti components. Although the pulsational variability could not be determined for some of the candidate Algols, pulsational components in EW Boo and DY Aqr have been discovered for the first time. The light curves of EW Boo and DY Aqr were analyzed to model the variations caused by the eclipsing behavior and then we determined the pulsational periods and amplitudes of the pulsating components in these Algols. The relationship between the pulsation and orbital periods of the eclipsing binaries were tested and discussed for the cases of EW Boo and DY Aqr.Öğe The early-type near-contact binary system V337 Aql revisited(Elsevier Science Bv, 2014) Tuysuz, M.; Soydugan, Faruk; Bilir, S.; Soydugan, Esin; Senyuz, T.; Yontan, T.The close binary V337 Aql consists of two early B-type components with an orbital period of 2.7339 d. New multi-band photometric observations of the system together with published radial velocities enabled us to derive the absolute parameters of the components. The simultaneous light and radial velocity curves solution yields masses and radii of M-1 = 17.44 +/- 0.31 M-circle dot and R-1 = 9.86 +/- 0.06 R-circle dot for the primary and M-2 = 7.83 +/- 0.18 M-circle dot and R-2 = 7.48 +/- 0.04 R-circle dot for the secondary component. Derived fundamental parameters allow us to calculate the photometric distance as 1355 +/- 160 pc. The present analysis indicates that the system is a near-contact semi-detached binary, in which a primary star is inside its Roche lobe with a filling ratio of 92% and the secondary star fills its Roche lobe. From O-C data analysis, an orbital period decrease was determined with a rate of -7.6 x 10(-8) yr(-1). Kinematic analysis reveals that V337 Aql has a circular orbit in the Galaxy and belongs to a young thin-disc population. (C) 2013 Elsevier B.V. All rights reserved.Öğe TOWARD UNDERSTANDING THE NATURE OF THE YOUNG DETACHED BINARY SYSTEM HD 350731(Iop Publishing Ltd, 2015) Soydugan, Faruk; Alicavus, F.; Bilir, S.; Soydugan, Esin; Puskullu, C.; Senyuz, T.The young binary system HD 350731 is a noteworthy laboratory for studying early-type binaries with similar components. We present here an analysis of differential multi-color photometric and spectroscopic observations of the double-lined detached system. Accurate absolute parameters were determined for the first time from a simultaneous solution of the light and radial velocity curves. HD 350731 consists of two B8V-type components with masses and radii, respectively, of M-1= 2.91 +/- 0.13 M-circle dot, M-2= 2.80 +/- 0.14 M-circle dot, R-1= 2.11 +/- 0.05 R-circle dot, and R-2= 2.07 +/- 0.05 R-circle dot. The effective temperatures were determined based on analysis of disentangled spectra of the components and were derived to be 12,000 +/- 250 and 11,830 +/- 300 K for the primary and secondary components, respectively. The measured projected rotational velocities, 69.2 +/- 1.5 km s(-1) for the primary and 70.1 +/- 1.7 km s-1 for the secondary, were found to be closer to the pseudo-synchronous velocities of the components. Comparison with evolutionary models suggests an age of 120 +/- 35 Myr. Kinematic analysis of the unevolved binary system HD 350731 revealed that it belongs to the young thin-disk population of the Galaxy.
