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Eclipsing binary systems with pulsating components allow the determination ofseveral physical parameters of the stars, such as mass and radius, that, whencombined with the pulsation properties, can be used to constrain the modelingof stellar interiors and evolution. Hereby, we present the results of the studyof CoRoT 105906206, an eclipsing binary system with a pulsating componentlocated in the CoRoT LRc02 field. The analysis of the CoRoT light curve wascomplemented by high-resolution spectra from the Sandiford at McDonaldObservatory and FEROS at ESO spectrographs, which revealed a double-linedspectroscopic binary. We used an iterative procedure to separate thepulsation-induced photometric variations from the eclipse signals. First, aFourier analysis was used to identify the significant frequencies andamplitudes due to pulsations. Second, after removing the contribution of thepulsations from the light curve we applied the PIKAIA genetic-algorithmapproach to derive the best parameters that describe the orbital properties ofthe system. The light curve cleaned for pulsations contains the partial eclipseof the primary and the total eclipse of the secondary. The system has anorbital period of about 3.694 days and is formed by a primary star with mass M1= 2.25 +/- 0.04 solar masses, radius R1 = 4.24 +/- 0.02 solar radii, andeffective temperature Teff1 = 6750 +/- 150 K, and a secondary with M2 = 1.29+/- 0.03 solar masses, R2 = 1.34 +/- 0.01 solar radii, and Teff2 = 6152 +/- 162K. The best solution for the parameters was obtained by taking into account theasymmetric modulation observed in the light curve, known as the O'Connelleffect, presumably caused by Doppler beaming. The analysis of the Fourierspectrum revealed that the primary component has p-mode pulsations in the range5-13 c/d, which are typical of Delta Scuti type stars.

CoRoT 105906206: a short-period and totally eclipsing binary with a Delta Scuti type pulsator