EDP Sciences
Free Access
Volume 437, Number 2, July II 2005
Page(s) 545 - 551
Section Stellar structure and evolution
DOI https://doi.org/10.1051/0004-6361:20041868
Published online 21 June 2005

A&A 437, 545-551 (2005)
DOI: 10.1051/0004-6361:20041868

Apsidal motion in southern eccentric eclipsing binaries: V539 Ara, GG Lup, V526 Sgr and AO Vel

M. Wolf1 and M. Zejda2

1  Astronomical Institute, Charles University Prague, 180 00 Praha 8, V Holesovickách 2, Czech Republic
    e-mail: wolf@cesnet.cz
2  Nicholas Copernicus Observatory and Planetarium, 616 00 Brno, Czech Republic

(Received 20 August 2004 / Accepted 20 February 2005)

Several new times of minimum light have been observed photoelectricaly for the early-type double-lined eccentric eclipsing binaries V539 Ara ( $P = 3\fd2, e = 0.05$), GG Lup ( $1\fd9, 0.15$), V526 Sgr ( $1\fd9, 0.22$) and AO Vel ( $1\fd6, 0.07$). The $\rm O{-}C$ diagrams are analysed using all reliable timings found in the literature and improved values for the elements of the apsidal motion are computed. We find more precise, relatively short periods of apsidal motion of about 162, 102, 155 and 54 years for V539 Ara, GG Lup, V526 Sgr and AO Vel, respectively. The corresponding internal structure constants, log k2, are then found to be -2.33, -2.16, -2.36 and -2.24 under the assumption that the component stars rotate pseudosynchronously. The relativistic effects are negligible, being about 6-7% of the total apsidal motion rate in all systems. Using the light-time effect solution, for V539 Ara we have found a third component orbiting with a period of about 42 years, for AO Vel we confirmed the third body with an orbital period of 33 years.

Key words: stars: binaries: eclipsing -- stars: individual: V539 Ara -- stars: individual: GG Lup -- stars: individual: V526 Sgr -- stars: individual: AO Vel -- stars: fundamental parameters

SIMBAD Objects

© ESO 2005

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