Light curve analysis of the short period eclipsing binary RT and

We have analysed the 1978 UBV photoelectric observations of the short-period (RS CVn type) binary system RT And, using the rectifiable methods of Russell and Merrill (1952) and Kitamura (1965). The primary minimum is a transit. The solutions allow us to classify the system as a detached one, but a certain disagreement results with respect to solutions of previous epochs. A graphical test of the reliability of the solution is given.     

Light curve analysis of the new eclipsing binary LD355

The V light curve of eclipsing binary LD355 was analyzed by using the latest version of Wilson Program in order to derive photometric elements of this system. Since no spectroscopic mass ratio is available, the q‐search method was applied to yield the preliminary range of mass ratio in order to search for the final solution. The solution was performed by assuming detached (mode 2) and semi‐detached (mode 5) configurations, since no classification of the system based on the shape of light curve is possible. The solution in mode 5 leads to an acceptable model. The present solution reveals that LD355 has a photometric mass ratio q = 0.178 and is a semi‐detached binary with the secondary component filling the Roche lobe.     

The UV spectrum of the binary system SZ Psc

In this paper we study the far-UV as well as the UV spectrum of the spectroscopic binary system SZ Psc in the wavelength ranges 1235–1950 Å and 2710–3090 Å, respectively, from spectra obtained with the International Ultraviolet Explorer (IUE). The UV spectrum of SZ Psc is mainly an emission spectrum. The short wavelength region includes emission lines formed from the low chromosphere to the transition region (e.g., Siiv,Civ, andNv) and also a deep and broad absorption line of Feii.The Mgii[1] resonance doublet at about 2800 Å presents a P Cygni profile and a multiple structure with two emission and two absorption satellite components. We also present the emission measure diagram in the temperature region 4.4T _e <53.     

Light curve variations of the eclipsing binary V367 Cygni

The long-period eclipsing binary star V367 Cygni has been observed photoelectrically in two colours,B andV, in 1984, 1985, and 1986. These new light curves of the system have been discussed and compared for the light-variability with the earlier ones presented by Heiser (1962). Using some of the previously published photoelectric light curves and the present ones, several primary minima times have been derived to calculate the light elements. Any attempt to obtain a photometric solution of the binary is so complicated by the peculiar nature of the light curve caused by the presence of the circumstellar matter in the system. Despite this difficulty, however, some approaches are being carried out to solve the light curves which will be discussed shortly.     

Three colour photoelectric observations of the symbiotic eclipsing binary CI Cyg

We present three colour photoelectric observations of CI Cyg during the 1980 eclipse. Some interesting photometric peculiarities are shown that must be taken into account for a theoretical model of this eclipsing symbiotic star.     

Light curve analysis of Hipparcos data for the massive O-type eclipsing binary UW CMa

Hipparcos photometric data for the massive O-type binary UW CMa were analysed within the framework of the Roche model. Photometric solutions were obtained for five mass ratios in the q = M₂/M₁ = 0.5–1.5 range. The system is found to be in a contact configuration. Independently of q, the best-fitting model solutions correspond to the orbital inclination i ～ 71° and the temperature of the secondary component T₂ ～ 33500 K, at the fixed temperature of the primary T₁ = 33750 K. Considering that the spectrum of the secondary is very weak, photometric solutions corresponding to the contact configuration favor the mass ratio q smaller than unity (in which case the luminosity of the secondary is smaller than that of the primary). The absolute parameters of the system are estimated for different values of the mass ratio.     

Light curve variations of the RS CVn-type eclipsing binary ER Vulpeculae

Photoelectric observations of the double-lined spectroscopic and eclipsing binary ER Vul were obtained inB andV colours of Johnson'sUBV system, between 1981 and 1986. The light curves show that the system is sometimes very active and sometimes very quiet and have changes in short time intervals. The were-like distortion, which is superimposed on the light curves, has been obtained. Moreover, small-amplitude light fluctuations in the light curves are noticeable.Paper presented at the 11th European Regional Astronomical Meetings of the IAU on New Windows to the Universe, held 3–8 July, 1989, Tenerife, Canary Islands, Spain.     

Two colour photometry and analysis of the eclipsing binary AT Pegasi

Two-colour photoelectric observations of the eclipsing binary AT Pegasi have been carried out at the Ege University Observatory. The light curves were analyzed with the methods of Wood and Wilson-Devinney. It is found that the period of the system is decreasing. The system was found to be an Algol type semi-detached binary. The absolute elements of the system are also deduced.     

Photometric investigation of the short period eclipsing binary star V719 Her

The Behlen observatory 0.76 m telescope CCD photometer is used to obtain 347 observations of the short period (P0^d.4) eclipsing binary star V719 Her. The observations done withV andR bandpass filters were made on 6 nights in 1993. Previously published light elements and the present five timings of minimum provide a new epoch and a more accurate orbital period of 0.4009828 days. Our analyses show that the period of the system appears to decrease. We recommend future monitoring of the eclipse minima for this system. No published spectral classification for V719 Her exists. From the color,V-R=0.391, we estimate it to be about F5.The 1993 version of the Wilson Devinney model gave the photometric solutions. The adopted solution indicates that V719 Her is a W UMa type contact binary. The mass ratio,q=(m ₂/m ₁, where star 1 eclipse at the primary minimum)=0.296 suggests that V719 Her is a WUMa system with type-A (transit during primary eclipse) configuration. The secondary minimum shows a total eclipse. V719 Her with period less than 0.5 and spectral class F5, is probably a zero-age contact system. Since our photometric solution shows that the luminosity difference between the components is very large, we suspect that V719 Her is most likely a single line spectroscopic binary. We recommend spectroscopic study of this system.     

Study of photoelectric observations of the eclipsing binary system FZ-Delphinus

Photoelectric observations in B and V for the FZ Del system are presented and its light curves are analyzed. Absolute parameters are obtained. The system shows a near contact subgaint secondary component with a likely K1 spectral type. The O-C curve is presented and probably a secular orbital period variations is detected on a timescale of about 6.9×10⁶ yrs, suggesting thermal timescale mass transfer. A new light elements for the system have been obtained. The system can be considered as an early stage of conservative case of mass transfer. This revised version was published online in August 2006 with corrections to the Cover Date.     

The spectroscopic orbit of the short period eclipsing binary V 836 Cygni

Spectroscopic elements of the single-lined spectroscopic binary V 836 Cyg are presented.     

UBV photoelectric observations of the eclipsing binary system XZ Cep

Three color photoelectric observations of the close binary system XZ Cep at the Abastumani Astrophysical Observatory are reported. These data cover the entire light curve and represent, up to now, the best and most extensive observations of this star. The positions of the components of XZ Cep on a mass-log g diagram show that it is in a phase following a rapid transfer of mass. The theoretical light curves are not fully consistent with the observed curves at phases of 0.35-0.40 and 0.6-0.9. This is evidently because of the influence of gaseous flows in the system. The existence of circumstellar matter and gas flows at phases of 0.7-0.9 are also confirmed by spectral data and by changes in the intrinsic polarization of XZ Cep. In addition, a polarimetric study of the star indicates that two or more interstellar clouds with different properties lie between XZ Cep and us. A detailed study of the photoelectric data presented here is also extremely interesting for the confirmation of the latter idea.     

Photometric observations and interpretation of the eclipsing binary system XY UMa

Photometric observations of eclipsing binary star XY UMa have been presented. The light curve analysis have been carried out on two colours,B andV, by inferring as much information as possible about the sarr from other published data and then synthesizing light curves and comparing them with our own observations.The light fluctuations of outside eclipses caused by intrinsic light variation of primary component have been obtained by deconvolution of the theoretical light curve from observed one. It has been shown that the intrinsic light variation of primary component can be interpreted in terms of cool star-spot covering 8% of the stellar photosphere.Finally, the significance of star-spot has been discussed.     

The first CCD photometric analysis and modeling for short period eclipsing binary system 1SWASPJ210423.7+073140.4.

We present the first light curve analysis of the new eclipsing binary of WUMa type 1SWASP J2104. A detailed photometric analysis was carried out in VRI bands using the most recent version of Wilson–Devinney (WD) code. The absolute physical parameters of the system were obtained and the previously determined period was confirmed. The evolution state shows that the primary component is slightly evolved above the ZAMS track while the secondary is on TAMS track. Our results show that the spectral types of the primary and secondary stars of the studied system are K4 and K5, respectively. The distance to 1SWASP J2104 was calculated to be 307 ± 21pc.     

Orbital period variation of the eclipsing binary system TT Herculis

New photoelectric UBV observations were obtained for the eclipsing binary TT Her at the Ankara University Observatory (AUO) and three new times of minima were calculated from these observations. The (O – C) diagram constructed for all available times of minima of TT Her exhibits a cyclic character superimposed on a quadratic variation. The quadratic character yields an orbital period decrease with a rate of dP /dt = –8.83 × 10^–8 day yr^–1 which can be attributed to the mass exchange/loss mechanism in the system. By assuming the presence of a gravitationally bound third body in the system, the analysis of the cyclic nature in the (O – C) diagram revealed a third body with a mass of 0.21M_⊙ orbiting around the eclipsing pair. The possibility of magnetic activity cycle effect as a cause for the observed cyclic variation in the (O – C) diagram was also discussed. (© 2007 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)     

The first light curve solutions and period changes of EW Psc and HN Psc

The first light curve solutions of the stars EW and HN in the Pisces constellation are presented. Photometry, and its’ periodic changes are calculated and discussed. The analysis of the O-C diagram is done by the MCMC approach in the OCFit code and a new ephemeris is provided for the two binary systems. The results show that EW Psc is a near contact eclipsing binary system with a photometric mass ratio q = 0.587, and the fillout factor is -0.034 and -0.018 for the primary and secondary components, respectively. The solution results also show that the system HN Psc is a weak-contact W UMa eclipsing binary with a photometric mass ratio q = 0.853, and with a fillout factor of 5.6%. The light curves solutions required a cold spot to account for the O'Connell effect.     

Photospheric and chromospheric activity of the short period X-ray and Algol eclipsing binary UX CrB

We present six \(\mbox{V}R_{c}I_{c}\) light curves of UX CrB from observations carried out from 2011–2015. We also obtained three optical spectra using the 2.16-m optical telescope and LAMOST survey at the national astronomical observatories. We classified its spectral type as \(\mbox{G2}\pm\mbox{2V}\). We noticed that there are strong absorptions in the H_α, H_β, Ca ii H&K and infrared triplet lines in the observed spectra. By subtracting away the photospheric contribution, we also noticed that there are small excess emissions in these chromospheric active lines, which indicate there are weak chromospheric activities. We tried and obtained four photometric solutions with different spot positions from our full and high time-resolution light curves in 2012, using the updated Wilson-Devinney code. The model with two spots on the primary produced the best result for explaining the observed light curves from 2012. Moreover, we explained all other light curves based on our photometric solution using our 2012 light curves. There are two active longitudes at about 68^° and 255^°. We noticed that the starspots have both long-time (years) and short-time (about two months) variation by analyzing the light curves and its starspot parameters. There is also an obvious oscillation of light curve maximum between 0.25 and 0.75 phases by analyzing the values of \(\mbox{Max.~I} - \mbox{Max.~II}\). We conclude UX CrB are the evolved main-sequence stars with strong photometric and chromospheric activities.