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. Zejda21 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)
Abstract
Several new times of minimum light have been observed photoelectricaly
for the early-type double-lined eccentric eclipsing binaries
V539 Ara (
),
GG Lup (
),
V526 Sgr (
) and
AO Vel (
).
The 
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