Volume 405, Number 3, July III 2003
|Page(s)||1063 - 1074|
|Section||Stellar structure and evolution|
|Published online||30 June 2003|
The massive binary CPD - 41° 7742 I. High-resolution optical spectroscopy *
Institut d'Astrophysique et de Géophysique, Université de Liège, Allée du 6 Août 17, Bât. B5c, 4000 Liège, Belgium e-mail: firstname.lastname@example.org
2 Royal Observatory of Belgium, Ringlaan 3, 1180 Brussels, Belgium e-mail: Herman.Hensberge@oma.be
Corresponding author: H. Sana, email@example.com
Accepted: 23 April 2003
We present the results of a spectroscopic campaign on the early-type binary CPD - 41° 7742. For the first time, we unambiguously detect the secondary's spectral signature and derive an accurate orbital solution for both components of the system. We confirm that the orbit displays a slight but definite eccentricity () despite the short period ( days). Previous radial velocity measurements available in the literature constitute together with our new observations a data set that spans more than 30 years. The combined primary orbital solution inferred is in excellent agreement with our solution and gives a period days. Based on spectroscopic criteria, we derive a spectral and luminosity classification of O9 III + B1 III. However, the luminosities and radii inferred from the membership of NGC 6231 rather indicate lower luminosity classes. We show that the equivalent widths of well isolated primary lines display variations that suggest that CPD - 41° 7742 is an eclipsing binary. This makes CPD - 41° 7742 the second known SB2 eclipsing early-type binary of the NGC 6231 cluster. We approximately constrain the inclination of the system . This may indicate that the system does not offer enough room for two stars with radii typical of giant stars and lends further support to a less evolved luminosity classification for at least one of the objects.
Key words: stars: individual: CPD - 41° 7742 / stars: binaries: close / stars: binaries: spectroscopic / stars: early-type / stars: fundamental parameters
© ESO, 2003
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