Bilesenlerinden biri Gamma Dor turu zonklayan orten cift yildizlarin sayisi oldukca azdir. Yildizlarin salt parametrelerini ancak cift cizgili orten ciftlerin isik ve dikine hiz egrlerinin analizi ile duyarli olarak olculebilir. Bu kosul altinda bulunan sonuclar birlestirilerek salt parametreler duyarli olarak bulunur. Boylece Gama Dor bilesenli orten ciftin uyeleri HR diyagraminda guvenilir bir sekilde isaretlenebilir. Yapilan uzun donemli ve atmosfer disi yuksek duyarlikli fotometrik veriler de bu yildizlara ait zonklama dogasinin ortaya cikarilmasinda onemli bir rol oynar. Sayica az olan, HR diyagramindaki yerleri henuz tam olarak anlasilamayan Gama Dor yildizlari belirlenebilir ve astrofiziksel acidan onemli bir sorun hakkinda ongorulerimiz olusabilir.

We present the first comprehensive catalog of the gamma Doradus type pulsating stars. This catalog covers observational properties of all gamma Dor variables obtained until January 2017. The photometric and physical properties of 109 well - known gamma Dor pulsators, 18 hybrid stars, 13 anomalous gamma Dor stars, and 22 gamma Dor stars in eclipsing plus 1 non-eclipsing SB2 binary systems are presented as separate tables. In addition, 291 candidate gamma Dor variables discovered by CoRot, 307 candidate gamma Dor, 205 hybrid and 11 candidate gamma Dor in binaries discovered by Kepler were also presented. Distribution of the genuine single gamma Dor pulsators in the P-puls-T-eff, Amplitude-T-eff, Amplitude-P-puls, and L-T-eff diagrams are presented and discussed. We find following correlations for the gamma Dor pulsators in the eclipsing binaries: P-puls proportional to P-orb(0.27), P-puls proportional to Q(0.45), and P-puls proportional to r(-0.44), where (Q) is the pulsation constant and r is the fractional radius of the pulsating component in the binary system. The correlation coefficients are not high enough due to limited sample and scattering in the data.

UV Psc has been observed since 1976 at the Ankara and Ege University Observatories. Mean light curves in B and V colours obtained using the maxima levels of observed light curves of the system. Assuming this light curves as the least active onesj the orbital parameters of the system have been obtained using the Wilson- Devinney code. The radial velocity curves of both components have been used during the solution. Wave-like distortion curves for each year have been obtained subtracting the theoretical light curves from the observed ones. Using these curves, the spot parameters have been roughly determined and finally spotted light curve solutions and the accurate spot parameters have been obtained. Activity and colour behaviour were examined.

We present new spectroscopic observations of the double-lined eclipsing binary V850 Cyg. The long cadence photometric observations obtained by Kepler were analysed and combined with the analysis of radial velocities for deriving the absolute parameters of the components. Masses and radii were determined as M-p=1.601 +/- 0.076 M-circle dot and R-p=4.239 +/- 0.076 R-circle dot, M-s=0.851 +/- 0.053 M-circle dot and R-s=5.054 +/- 0.087 R-circle dot for the components of V850 Cyg. We estimate an interstellar reddening of 0.28 +/- 0.12 mag and a distance of 1040 +/- 160 pc for the system. The measured rotational velocity of the secondary appears to lower than that of synchronize rotation. However its spectral lines are too weak to be measured the rotational velocity with reasonable accuracy. We have extracted the synthetic light curve from the observations and excluded the data within the eclipses for the frequency analysis. We obtained at least nine frequencies in the gamma Dor regime. It seems that the primary component oscillates with a dominant period of about 1.152549 +/- 0.000009 days. We also compare pulsational properties of the primary star of V850 Cyg with the gamma Dor type pulsating components in other binaries. (C) 2016 Elsevier B.V. All rights reserved.

We present new spectroscopic observations of the double-lined eclipsing binary V2653 Ophiuchii. The photometric observations obtained by ASAS were analyzed and combined with the analysis of radial velocities for deriving the absolute parameters of the components. Masses and radii were determined for the first time as M-p = 1.537 +/- 0.021 M-circle dot and R-p = 2.215 +/- 0.055 R-circle dot, M-s = 1.273 +/- 0.019 M-circle dot and R-s = 2.000 +/- 0.056 R-circle dot for the components of V2653 Oph. We estimate an interstellar reddening of 0.15 +/- 0.08 mag and a distance of 300 +/- 50 pc for the system, both supporting the membership of the open cluster Collinder 359. Using the out-of-eclipse photometric data we have made frequency analysis and detected a periodic signal at 1.0029 +/- 0.0019 c/d. This frequency and the location of the more massive star on the HR diagram lead to classification of a gamma Dor type variable. Up to date only eleven gamma Dor type pulsators in the eclipsing binaries have been discovered. For six out of 11 systems, the physical parameters were determined. Although a small sample, we find empirical relations that P-puls infinity P-orb(0.43) and P-puls infinity g(-0.83). While the pulsation periods increase with longer orbital periods, they decrease with increasing surface gravities of pulsating components and gravitational pull exerted by the companions. We present, briefly, the underlying physics behind the correlations we derived. (C) 2015 Elsevier B.V. All rights reserved.

We present new spectroscopic observations of the early type, double-lined eclipsing binary V1441 Aql. The radial velocities and the available photometric data obtained by ASAS is analysed for deriving the parameters of the components. The components of V1441 Aql are shown to be a B3 IV primary with a mass M-p = 8.02 +/- 0.51 M-circle dot and radius R-p = 7.33 +/- 0.19 R-circle dot and a B9 III secondary with a mass = 1.92 +/- 0.14 M-circle dot and radius R-s = 4.22 +/- 0.11 R-circle dot. Our analyses show that V1441 Aql is a doublecontact system with rapidly rotating components. Based on the position of the components plotted on the theoretical Hertzsprung-Russell diagram, we estimate that the ages of V1441 Aql is about 30 Myr, neglecting the effects of mass exchange between the components. Using the UBVJHK magnitudes and interstellar absorption we estimated the mean distance to the system V1441 Aql as 550 +/- 25 pc. (C) 2014 Elsevier B.V. All rights reserved.

We present new spectroscopic observations of the early type, double-lined eclipsing binary V446 Cep. The radial velocities and the photometric data obtained by Hipparcos were analysed for deriving the astrophysical parameters of the components. Masses and radii were determined as M_p=17.94±1.16 M_⊙ and R_p=8.33±0.29 R_⊙, M_s=2.64±0.30 M_⊙ and R_s=2.13±0.10 R_⊙ for the components of V446 Cep. Our analyses show that V446 Cep is a detached Algol-type system. Based on the position of the components plotted on the theoretical Hertzsprung-Russell diagram, we estimate that the age of V446 Cep is about 10 Myr, neglecting the effects of mass-loss and mass exchange between the components. Using the UBVJHK magnitudes and interstellar absorption we estimated the mean distance to the system V446 Cep as 1100±62 pc.

We present spectroscopic observations of the massive early-type system V745 Cas, embedded in a multiple-star system. The brightest star of the system is the eclipsing binary V745 Cas with an orbital period of 1.41 d. The radial velocities of both components and light curves obtained by INTEGRAL and Hipparcos missions were analysed. The components of V745 Cas are shown to be a B0 V primary with a mass M-p = 18.31 +/- 0.51 M-aS (TM) and radius R-p = 6.94 +/- 0.07 R-aS (TM) and a B(1-2) V secondary with a mass M-s = 10.47 +/- 0.28 M-aS (TM) and radius R-s = 5.35 +/- 0.05 R-aS (TM). Our analysis shows that both components fill their corresponding Roche lobes, indicating double contact configuration. Using the UBVJHK magnitudes and interstellar absorption, we estimated the mean distance to the system as 1700 +/- 50 pc. The locations of the component stars in the mass-luminosity, mass-radius, effective temperature-mass and surface gravity-mass are in agreement with those of the main-sequence massive stars. We also obtained UBV photometry of the three visual companions and we estimate that all are B-type stars based upon their de-reddened colours. We suspect that this multiple system is probably a member of the Cas OB4 association in the Perseus arm of the Galaxy.

We present spectroscopic observations of the massive multiple system HD 167971, located in the open cluster NGC 6604. The brighter component of the triple system is the overcontact eclipsing binary MY Ser with an orbital period of 3.32 d. The radial velocities and the previously published UBV data obtained by Mayer et al. and the UBVRI light curves by Davidge & Forbes are analysed for the physical properties of the components. We determine the following absolute parameters: for the primary star M-p = 32.23 +/- 0.54 M-circle dot, R-p = 14.23 +/- 0.75 R-circle dot; and for the secondary star M-s = 30.59 +/- 0.53M(circle dot), R-s = 13.89 +/- 0.75 R-circle dot. Photoelectric times of minimum light are analysed under the consideration of the light-time orbit. The centre-of-mass of the eclipsing binary is orbiting around the common centre-of-gravity of the triple system with a period of 21.2 +/- 0.7 yr and with a projected semi-major axis of 5.5 +/- 0.7 au. The mass function for the third star was calculated as 0.370 +/- 0.036 M-circle dot. The light contributions of the third star to the triple system in the UBV passbands were derived and the intrinsic magnitudes and colours were calculated individually for the three stars. The components of the eclipsing pair were classified as O7.5III and O9.5III. The intrinsic colour indices for the third star yield a spectral type of (O9.5-B0) III-I. This classification leads to constrain the inclination of the third-body orbit, which should be about 30 degrees, and therefore its mass should be about 29 M-circle dot. MY Ser is one of the rare massive O-type triple system at a distance of 1.65 +/- 0.13 kpc, the same as for the NGC 6604 embedded in the Ser OB2 association.

We present the multi-color, five-year light curves and the radial velocities of the near-contact binary system KR Cyg. We derived the masses of the components as 2.88 ± 0.20 Mand 1.26 ± 0.07 Mand the radii as 2.59 ± 0.06 Rand 1.80 ± 0.04 R� . We also searched for the empirical determination of albedo and effective temperature of the cooler, less massive star of KRCyg, and of two similar near contact binaries AKCMi, and DOCas. The residuals between the observed and computed fluxes are attributed to the effect of mutual illumination which heats the surface layers of the illuminated star and does vary not only its bolometric albedo but also its limb-darkening coefficient and gravity-brightening exponent. The effective albedos are generally smaller than that expected from an envelope of convective star. These results are preliminary and speculative.

BVR light curves and radial velocities for the double-lined eclipsing binary V1135 Her were obtained. Our analyses of the multi-color light curves and radial velocities led to the determination of fundamental stellar properties of both components of the interesting system V1135 Her. The system consists of two evolved stars, G1+K3 between giants and supergiants, with masses of M-1 = 1.461 +/- 0.054 M-circle dot and M-2 = 0.504 +/- 0.040 M-circle dot and radii of R-1 = 27.1 +/- 0.4 R-circle dot and R-2 = 10.4 +/- 0.2 R-circle dot. Most of the observed and calculated parameters of the V1135 Her and its location on the color-magnitude and period-luminosity diagrams lead to a classification of an Anomalous Cepheid.

The multicolour light curves and radial velocities for TYC 1031 1262 1 have been obtained and analysed. TYC 1031 1262 1 includes a Cepheid with a period of 4.15270 +/- 0.00061 d. The orbital period of the system is about 51.2857 +/- 0.0174 d. The pulsation period indicates that the secular period is increasing at a rate of of 2.46 +/- 0.54 min yr(-1). The observed B, V and R magnitudes have been cleaned of the intrinsic variations of the primary star. The remaining light curves that have been obtained consist of eclipses and proximity effects, and these have been analysed to obtain the orbital parameters. The system consists of two evolved stars, F8 II + G6 II, with masses of M-1 = 1.640 +/- 0.151 M-circle dot and M-2 = 0.934 +/- 0.109 M-circle dot and radii of R-1 = 26.9 +/- 0.9 R-circle dot and R-2 = 15.0 +/- 0.7 R-circle dot, respectively. The pulsating star almost fills its corresponding Roche lobe, which indicates the possibility that mass loss or transfer has taken place. We find an average distance of d = 5070 +/- 250 pc, using the BVR and JHK magnitudes, and also the V-band extinction. The kinematic properties and the distance to the Galactic plane (i.e. 970 pc) indicate that it belongs to the thick-disc population. Most of the observed and calculated parameters of TYC 1031 1262 1 lead to its classification as an anomalous Cepheid.

New spectroscopic observations of the double-lined eclipsing binary AQCas are presented. All available spectroscopic and photometric observations have been analysed for the fundamental properties of the components. Analyses show that the system consists of a massive primary with a mass of 17.63 +/- 0.91 Me and radius of 13.48 +/- 0.64 R-circle dot and a secondary with 12.56 +/- 0.81 M-circle dot and radius of 23.55 +/- 0.73 R-circle dot, corresponding spectral types of B0.5(+/- 2) II-III + B3(+/- 1) II. The secondary star fills its corresponding Roche lobe and mass transfer to the primary star is going on. This stream considerably does affect the photometric observations both starting from the second quarter up to the first contact of primary eclipse and just at the second maximum. Thus, the light curve is distorted and tightly depended on the wavelength of the observations. The available multi passband light curves have been analysed by taking the stream effects, as either hot or cool spots, into account. The comparison of the models and observations in the log(L/L-circle dot) log - T-eff and logg - log T-eff diagrams clearly shows that the more massive star is consistent with models and is predicted to be close to the phase of hydrogen shell ignition. Average distance to the system is estimated as 4150 +/- 240 pc using the BVJHK magnitudes and V-passband extinction. (C) 2013 Elsevier B.V. All rights reserved.

The eclipsing binary T-Cyg1-12664 has been observed both spectroscopically and photometrically, and the radial velocities of both the components and the ground-based VRI light curves have been obtained. The Kepler R data and radial velocities for the system have been analysed simultaneously. Masses and radii have been obtained as 0.680 +/- 0.021 M-circle dot and 0.613 +/- 0.007 R-circle dot for the primary star and 0.341 +/- 0.012 M-circle dot and 0.897 +/- 0.012 R-circle dot for the secondary star. The distance to the system has been estimated as 127 +/- 14 pc. The observed wave-like distortion at out-of-eclipse is modelled with two separate spots on the more massive star, which is also confirmed by the Ca II K and H emission lines in its spectra. The locations of the components in the mass-radius and mass-effective temperature planes have been compared with the well-determined low-mass components of eclipsing binaries as well as with the theoretical models. While the radius of the primary star is consistent with the main-sequence stars, the radius of the less massive component appears to be 2.8 times larger than that of the main-sequence models. A comparison of the radii of low-mass stars with the models reveals that the observationally determined radii begin to deviate from the models with a mass of 0.27 M-circle dot, and suddenly reach to maximum deviation at a mass of 0.34 M-circle dot. Then, the deviations begin to decrease up to the solar mass. The maximum deviation, seen at a mass of about 0.34 M-circle dot, is very close to the mass of fully convective stars, as suggested by theoretical studies. A third star in the direction of the eclipsing pair has been detected from our VRI images. The observed infrared excess of the binary most probably arises from this star, which can be radiated mostly in the infrared bands.

We observed spectroscopically the eclipsing binary system T-Cyg1-01385 in order to determine physical properties of the components. The double-lined nature of the system is revealed for the first time and the radial velocities are obtained for both stars. We have derived masses, radii and luminosities for both components. Analyzes of the radial velocities and the KeplerCam and the TrES light curves yielded masses of M-1 = 1.059 +/- 0.032 M-circle dot and M-2 = 0.342 +/- 0.017 M-circle dot and radii of R-1 = 1.989 +/- 0.022 R-circle dot and R-2 = 0.457 +/- 0.013 R-circle dot. Locations of the low-mass companion in the mass-radius and mass-effective temperature planes and comparison with the other low-mass stars show that the secondary star appears just at the transition from partially to fully convective interiors for the M dwarfs. When compared to stellar evolution models, the luminosities and effective temperatures of the components are consistent with Z = 0.004 and an age of about 6 Gyr. A distance to the system was calculated as d = 355 +/- 7 pc using the BV and JHK magnitudes. (C) 2013 Elsevier B.V. All rights reserved.

The multi-color photometric and spectroscopic observations of the newly discovered eclipsing binary T-Lyr0-08070 were obtained. The resultant light and radial velocities were analysed and the absolute parameters of the components were determined. The system is composed of an F3 and an M3 main-sequence stars. Masses and radii were estimated to be 1.37±0.23M⊙ and 1.60±0.09R⊙ for the primary and 0.32±0.04M⊙ and 0.86±0.06R⊙ for the secondary star. The less massive secondary component has a radius at least two times larger with respect to its mass. Using the BVJHK magnitudes of the system we estimated an interstellar reddening of 0.22mag and a distance to the system as 479±36pc.

The equivalent widths (EWs) of the C ii lambda 4267 angstrom line were measured for the mass-gaining primary stars of 18 Algol-type binary systems. The EWs of the gainers were compared with the EWs of single standard stars that have the same effective temperature and luminosity class. This comparison clearly indicates that the EWs of the gainers are systematically smaller than those of the standard stars. The primary components of the classical Algols, located in the main-sequence band of the HertzsprungRussell diagram, appear to be carbon-poor stars. We estimate [NC/Ntot] relative to the Sun as -1.91 for GT Cep, -1.88 for AU Mon and -1.41 for TU Mon, indicating poorer carbon abundance. An average differential carbon abundance has been estimated to be -0.82 dex relative to the Sun and -0.54 dex relative to the main-sequence standard stars. This result is taken to be an indication of material transferring from the evolved less-massive secondary components to the gainers, such that the CNO cycle processed material changed the original abundance of the gainers. There appear to be relationships between the EWs of the C ii?4267 angstrom line and the rates of orbital period increase and mass transfer in some Algols. As the mass transfer rate increases, the EW of the C ii line decreases. This indicates that accreted material has not yet been completely mixed in the surface layers of the gainers. This result supports the idea of mixing as an efficient process to remove the abundance anomaly built up by accretion. The chemical evolution of the classical Algol-type systems could lead to constraints on the initial masses of the less massive, evolved, mass-losing stars.

We present the results of the high-resolution spectroscopic observations of the neglected binary system HD\,194495 (B3\,IV-V+B4\,V). A combined analysis of three different photometric data set ($Tycho$ B$_T$ and V$_T$ photometry, H$_p$-band data of $Hipparcos$ and $V-$band data of ASAS3 photometry) and radial velocities indicates that the system has an orbital period of 4.90494 $\pm$ 0.00005 days and an inclination of 69$\pm$1 degrees. This solution yields masses and radii of $M_{\rm 1}$ = 7.57$\pm$0.08 $M_{\odot}$ and $R_{\rm 1}$ = 5.82$\pm$0.03 $R_{\odot}$ for the primary and $M_{\rm 2}$ = 5.46$\pm$0.09 $M_{\odot}$ and $R_{\rm 2}$ = 3.14$\pm$0.08 $R_{\odot}$ for the secondary. Based on the position of the two stars plotted on a theoretical H-R diagram, we find that the age of the system is $\gtrsim$ 28 Myr, according to stellar evolutionary models. The spectroscopic and photometric results are in agreement with those obtained using theoretical predictions.

We present spectroscopic observations of the double-lined early type eclipsing binary V1898\,Cyg. The radial velocities were obtained by means of the cross-correlation technique. Analyses of the BV light curves and RVs led to determination of the fundamental stellar parameters of the V1898\,Cyg's components. We derived new ephemerides for the eclipsing pair using the observed times of mid-eclipses. The residuals between the observed and computed times of mid-eclipses were analysed and a rate of the period change $\dot{P}/P= 6.68 \times 10^{-7}\,yr^{-1}$ was obtained. The orbital period is increased by about 0.38 s in the last 24 years due to the mass transfer from less massive secondary to the more massive primary star with an amount of $1.88\times10^{-7}\,$ \Msun in a year, assuming conservative case. Results of the light and radial velocity curves' analyses were combined and the physical parameters of the components were revealed. The absolute parameters for the stars are derived as: M$_1$=6.054$\pm$0.037 M$_{\odot}$, M$_2$=1.162$\pm$0.011 M$_{\odot}$, R$_1$=3.526$\pm$0.009 R$_{\odot}$, R$_2$=2.640$\pm$0.010 R$_{\odot}$, T$_{eff_1}$=18\,000$\pm$600 K, and T$_{eff_2}$=6\,200$\pm$200 K. We have calculated the distance to the system of V1898\,Cyg as 501$\pm$5 pc using the infrared JHK magnitudes and bolometric corrections for the primary star. While the more massive star locates in the main-sequence band the less massive secondary appears in the giant branch which is common in the classical Algols. Any attempt for comparison with current stellar evolution models was made because the system seems in the phase of fast mass transfer. Moreover, the components of the system's proper motions present some indications about membership of the North America nebula.

Accurate absolute properties are determined for the first time for the 3.15 day period eccentric eclipsing binary star FT Ori based on new absolute photometry, five differential light curves, and a radial velocity curve. The stars appear to be normal for their spectral types, A0 + A2. The orbit is highly eccentric (e = 0.409) and shows apsidal motion with a period of 536 years. The absolute properties and the degree of central mass concentration of the stars are consistent with current theoretical models at an age of 190 Myr.