The massive binary CPD - 41 degr 7742 I. High-resolution optical spectroscopy

Details The massive binary CPD - 41 degr 7742 I. High-resolution optical spectroscopy The massive binary CPD - 41 degr 7742 I. High-resolution optical spectroscopy

Jul 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003a%26a...405.1063s&link_type=abstract

Astronomy and Astrophysics, v.405, p.1063-1074 (2003)

Astronomy and Astrophysics

Astrophysics

22

Stars: Individual: Cpd, 41 Degr 7742, Stars: Binaries: Close, Stars: Binaries: Spectroscopic, Stars: Early-Type, Stars: Fundamental Parameters

Scientific paper

We present the results of a spectroscopic campaign on the early-type binary CPD - 41 degr 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 (e=0.027+/-0.006) despite the short period (P=2.44070+/-0.00043 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 P=2.44062+/-0.00005 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 degr 7742 is an eclipsing binary. This makes CPD - 41 degr 7742 the second known SB2 eclipsing early-type binary of the NGC 6231 cluster. We approximately constrain the inclination of the system i_min~60degr . 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.
Based on observations collected at the European Southern Observatory (La Silla, Chile).

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