Aims. Eclipsing binary systems with pulsating components allow
determination of several physical parameters of the stars, such as mass and radius, that
can be used to constrain the modeling of stellar interiors and evolution when combined
with the pulsation properties. We present the results of the study of CoRoT 105906206, an
eclipsing binary system with a pulsating component located in the CoRoT LRc02 field.
Methods. The analysis of the CoRoT light curve was complemented by
high-resolution spectra from the Sandiford at McDonald Observatory and FEROS at ESO
spectrographs, which revealed a double-lined spectroscopic binary. We used an iterative
procedure to separate the pulsation-induced photometric variations from the eclipse
signals. First, a Fourier analysis was used to identify the significant frequencies and
amplitudes due to pulsations. Second, after removing the contribution of the pulsations
from the light curve we applied the PIKAIA genetic-algorithm approach to derive the best
parameters for describing the system orbital properties.
Results. The light curve cleaned for pulsations contains the partial
eclipse of the primary and the total eclipse of the secondary. The system has an orbital
period of about 3.694 days and is formed by a primary star with mass M1 = 2.25 ± 0.04
M⊙, radius R1 =
4.24±0.02
R⊙, and effective temperature
Teff,1 = 6750
± 150 K, and a secondary
with M2 = 1.29 ±
0.03
M⊙, R2 =
1.34±0.01
R⊙, and Teff,2 = 6152 ± 162 K. The best solution for the
parameters was obtained by taking into account the asymmetric modulation observed in the
light curve, known as the O’Connell effect, presumably caused by Doppler beaming. The
analysis of the Fourier spectrum revealed that the primary component has p-mode pulsations
in the range 5–13 d-1, which are typical of δ Scuti type stars
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