Eclipsing Binaries Research Papers - Academia.edu (original) (raw)

We present the first release of the Czech Variable star catalogue that currently contains 1228 stars whose variability was discovered by 60 Czech observers. The catalogue contains confirmed variable stars of various types, but also... more

We present the first release of the Czech Variable star catalogue that currently contains 1228 stars whose variability was discovered by 60 Czech observers. The catalogue contains confirmed variable stars of various types, but also candidates. We give precise coordinates, cross identification with other catalogues, information about constellation, variability type, brightness, light elements, name of the discoverer and year of discovery. In eighty-eight percent of stars the variability type is estimated, for more than 60 % of the stars the light ephemerides are given.

Jupiter Trojans represent a population of asteroids dynamically decoupled from the Main Belt. They show rather uniform spectral characteristics and geometric albedos. The distribution of their rotational properties (spin rates, light... more

Jupiter Trojans represent a population of asteroids dynamically decoupled from the Main Belt. They show rather uniform spectral characteristics and geometric albedos. The distribution of their rotational properties (spin rates, light curve amplitudes and spin axis orientation) carries information about their origin and about the processes that controlled their evolution. For this reason, comparing the rotational properties of the Trojans with those of Main Belt asteroids (MBAs) can help provide a better understanding of both populations. We recently published the observational results from a uniform and unbiased survey of rotational properties of Jupiter Trojans carried out during the past two decades. This body of observations provide a statistically significant sample which is the basis for our analysis.

113F263 Nolu TUBITAK destegi ile yurutulen bu calisma ile TUBITAK Ulusal Gozlemevi (TUG)'da bulunan 1.5 m capindaki (Rus-Turk Teleskobu) RTT150 icin isigi cift kirma ozelligi ile bilinen WeDoWo (Wedge Double Wollaston) tipi prizma... more

113F263 Nolu TUBITAK destegi ile yurutulen bu calisma ile TUBITAK Ulusal Gozlemevi (TUG)'da bulunan 1.5 m capindaki (Rus-Turk Teleskobu) RTT150 icin isigi cift kirma ozelligi ile bilinen WeDoWo (Wedge Double Wollaston) tipi prizma RTT150-TFOSC sistemine uygun olarak tasarlanmis ve sisteme entegre edilmistir. Boylece, fotometri ve spektroskopi ozelliklerine sahip olan RTT150 teleskopunun gozlem olanagi artirilmistir. TFOSC-WP polarimetresi olarak adlandirilan polarimetre ile es zamanli olarak 0$^{\\circ}$, 45$^{\\circ}$, 90$^{\\circ}$, 135$^{\\circ}$'de goruntuler alinabilmektedir. Tasarimin polarimetrik ozellikleri, guclu polarize ve polarize olmayan standart yildizlardan toplanan gozlemsel veriler ile incelenmistir. Cihazsal polarizasyondan kaynaklanan polarizasyon derecesinin sistematik hatasi ekvatoral koordinat sisteminde 1 x 5 yaydakika icin 0.2% ve konum acisinin hatasi 1.9$^{\\circ}$ olarak hesaplanmistir. Sistemin parlaklik limiti ise 17 Kadir'dir. Bu sinirlamalar ve ...

Eclipsing binary systems are significant objects for astrophysics in that direct observations can determine the fundamental parameters of stars. In this study, we precisely determined the fundamental parameters of the binary component... more

Eclipsing binary systems are significant objects for astrophysics in that direct observations can determine the fundamental parameters of stars. In this study, we precisely determined the fundamental parameters of the binary component stars obtained by simultaneous analysis of radial velocities and the TESS light curve using the Wilson and Devinney code. Following the analysis, the masses and radii of the primary and secondary components were determined as M 1 = 1.58 ± 0.01M ⊙ , M 2 = 0.48 ± 0.02M ⊙ , and R 1 = 1.93 ± 0.01R ⊙ , R 2 = 1.14 ± 0.01R ⊙ , respectively. Furthermore, the distance of IS CMa is calculated as 92.7 ± 6.5 pc. On the basis of the analysis of the mid-eclipse times, it was found that the variation in the orbital period is represented by an upward parabola. It has an increasing rate of dP∕dt = 1.09 × 10 −7 day year −1. Using PARSEC stellar evolutionary tracks and isochrones with solar metallicity estimated the age of IS CMa as 1.3 ± 0.1 Gyr. Kinematic and Galactic orbital parameters of IS CMa were obtained from the astrometric and spectroscopic data of the system. The Galactic orbit analysis reveals that IS CMa formed inside the solar circle and it is a member of the young thin-disc population.

The GO Cygni system is a short period -0.7177 days- eclipsing binary with a % beta Lyrae-type light curve. In this study our new BV photoelectric observations of the system, made at the Bucharest Observatory during 1993-94 are presented.... more

The GO Cygni system is a short period -0.7177 days- eclipsing binary with a % beta Lyrae-type light curve. In this study our new BV photoelectric observations of the system, made at the Bucharest Observatory during 1993-94 are presented. These, and our old ones -made at the Kryonerion Astronomical Station of the National Observatory of Athens, Greece, in 1985- are analysed using Wood's program. The geometrical elements of the system -derived from the present analysis- correspond to a contact configuration suggesting that it belongs to the so-called near contact binaries. Moreover, its physical parameters lead to an unevolved system with both of its components located very close to the ZAMS. Finally, its orbital period is examined and found to show continuous increased.

We present results of two-color photometric study of the newly discovered EW– type eclipsing binary star GSC 04370-00206 in the field of the intermediate polar MU Cam. CCD V,R observations were obtained in the Astronomical Observatories... more

We present results of two-color photometric study of the newly discovered EW– type eclipsing binary star GSC 04370-00206 in the field of the intermediate polar MU Cam. CCD V,R observations were obtained in the Astronomical Observatories in Hlohovec, Baja and Kolonica in 2007-2009. Improved photometric elements for the primary minimum were determined: Min.BJD=2454805.75635+0.44264511(27)E. The range of the brightness variations is 13.79-14.13 (V) and 13.07-13.44 (R). The accuracy of the period determination is by a factor of ∼ 7, 000 times better than the one published by the discoverers based on only one night of observations. We report on the night-to-night variability of the shape of the light curve which is interpreted by a presence of spots in the atmosphere of one or both components (O'Connel effect).