Volume 572, December 2014
|Number of page(s)||8|
|Section||Catalogs and data|
|Published online||28 November 2014|
Astronomical Institute, Charles University in Prague, Faculty of
Mathematics and Physics, 180
00 Praha 8, V Holešovičkách 2, Czech Republic
2 Department of Theoretical Physics and Astrophysics, Masaryk University, Kotlářská 2, 611 37 Brno, Czech Republic
Received: 26 May 2014
Accepted: 1 September 2014
Aims. The Danish 1.54-meter telescope at the La Silla observatory was used for photometric monitoring of selected eccentric eclipsing binaries located in the Small Magellanic Cloud. The new times of minima were derived for these systems, which are needed for accurate determination of the apsidal motion. Moreover, many new times of minima were derived from the photometric databases OGLE and MACHO. Eighteen early-type eccentric-orbit eclipsing binaries were studied.
Methods. Their O–C diagrams of minima timings were analysed and the parameters of the apsidal motion were obtained. The light curves of these eighteen binaries were analysed using the program PHOEBE, giving the light curve parameters. For several systems, the additional third light also was detected.
Results. We derived for the first time and significantly improved the relatively short periods of apsidal motion from 19 to 142 years for these systems. The relativistic effects are weak, up to 10% of the total apsidal motion rate. For one system (OGLE-SMC-ECL-0888), the third-body hypothesis was also presented, which agrees with high value of the third light for this system detected during the light curve solution.
Key words: binaries: eclipsing / stars: early-type / stars: general / stars: fundamental parameters / Magellanic Clouds
Table A.1 is only available at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (188.8.131.52) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/572/A71
© ESO, 2014
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