Volume 403, Number 2, May IV 2003
|Page(s)||675 - 681|
|Section||Stellar structure and evolution|
|Published online||06 May 2003|
Refinement of third body parameters and new photometric results for the early-type multiple system IU Aurigae*
Çanakkale Onsekiz Mart University, Department of Physics, 17100 Çanakkale, Turkey
2 Çanakkale Astrophysics Research Center, Terzioğlu Campus, 17100 Çanakkale, Turkey
3 Astronomical Institute, Charles University, Švédská 8, 15000 Praha 5, Czech Republic
4 Dr. Remeis-Sternwarte, Astronomisches Institut der Universtät Erlangen-Nürnberg, Sternwartstrasse 7, 96049 Bamberg, Germany
5 Ankara University, Department of Astronomy and Space Sciences, 06100 Ankara, Turkey
Corresponding author: S. Özdemir, email@example.com
Accepted: 7 March 2003
The massive eclipsing binary system IU Aurigae is re-analyzed in the context of new photometric observations and an improved treatment of its long-term period changes (O–C diagram) derived from new times of minima. The best-fit of the O–C curve reveals that the third component is orbiting around the system with a period of 293.3 days in a highly eccentric orbit (). A solution of the most recent UBV light curves obtained during 1997/1998 showed a third light contribution of ≈23% and continuation of the orbital plane precession of IU Aurigae. Since the revised mass of the third component deduced from the analysis of the O–C curve of would imply a larger fraction of third light than suggested by the value of 23% derived from the light curve analysis, the third body is possibly composed of two components. A q-search test applied to the UBV light curves yields a minimum value at , which confirms previous photometric and spectroscopic solutions.
Key words: binaries: eclipsing / stars: early-type / stars: individual: IU Aurigae
© ESO, 2003
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