A large number of binary systems with non-radially pulsating members were observed by CoRoT. Some of them, which were eclipsing binaries with members of γ Doradus type, were discovered during CoRoT runs.
 The eclipse phenomenon plays a key role since global parameters can immediately follow, bringing invaluable constraints, in addition to the seismic ones, to stellar modeling.

AU Monocerotis: This semi-detached binary system contains a Be star interacting with its G star companion.
Its observation by CoRoT provided an extremely high quality ligthcurve.
Global parameters could then be improved and new ephemeris for the orbital motion as well as for another long term variation were derived.
This long period variation seems to originate from a periodic light attenuation by circumstellar dust.

HD 174884: Tidally induced pulsations have been detected in the high eccentricity (e=0.29) and short period binary system HD 174884 consisting of two B stars.
The upper panel of the figure shows the full light curve of the system.
In the second panel tiny secondary eclipses are seen with a depth of about 1% of the depth of the primary eclipse.
Actually the system is formed of stars of similar mass, size and temperature.
Were the orbit circular, the eclipses would be similar in depth.
However the orbit is highly eccentric and its orientation in space with respect to us is such that the secondary eclipse occurs when the stars are at a larger distance than at primary eclipse.
The third panel of the figure shows the projection on the plane of the sky (i.e. the system as we see it) at different orbital phases.

CoRoT 102918586 (alias CoRoT Sol 1): The relatively bright eclipsing system CoRoT 102918586 is a double-lined spectroscopic binary, observed by CoRoT, which revealed clear evidence of γ Doradus type pulsations.
In addition to CoRoT photometry, a spectroscopic follow-up was performed which yielded the radial velocity curves, the component effective temperatures, the metallicity, and the line-of-sight projected rotational velocities.
The eclipsing binary light curve analysis, combined with the spectroscopic results, provided system physical parameters with 1–2% accuracy while the comparison with evolutionary models led to constraints on the age of the system.
After subtracting the best–fitting eclipsing binary model, the residuals were analyzed to determine the pulsation properties.
The primary star pulsates with typical γ Dor frequencies and shows a period spacing consistent with high order g-modes of degree l=1.

HR 6902: The binary system ζ Aurigae HR 6902 containing a red giant and a B star was observed by CoRoT during two runs, which allowed us to fully cover the primary as well as the secondary eclipses.
This system is presently being analyzed with the ultimate goal of bringing new constraints on the internal structure of the red giant in particular.

A low mass binary: One of the binary system observed by CoRoT is of particular interest since the less massive component is a late M star of 0.23 M⊙ with an estimated effective temperature of about 3000 K. The primary component is a 1.5 M⊙ star MS star.

 A beaming effect in a binary: A binary system observed by CoRoT showed out of eclipses variations which were interpreted as a beaming effect (also called Doppler boosting).
This effect results from the variation in brightness of source approaching or moving away from the observer, with an amplitude proportional to the radial velocity divided by the speed of light.
The periodic variation in the velocity of an orbiting star will thus produce a periodic beaming variation in the light curve.
Such an effect can confirm the binary nature of a system even without any detectable eclipses nor transits.
One of the main advantages of the beaming effect is the possibility to determine the radial velocity directly from the light curve but very different luminosities of the binary components are required and a single radial velocity curve can only be obtained as in an SB1 binary system.
The out of eclipse variations were modeled with the BEER (Beam
A large number of binary systems with non-radially pulsating members were observed by CoRoT. Some of them, which were eclipsing binaries with members of γ Doradus type, were discovered during CoRoT runs.  The eclipse phenomenon plays a key role since global parameters can immediately follow, bringing invaluable constraints, in addition to the seismic ones, to stellar modeling.
AU Monocerotis: This semi-detached binary system contains a Be star interacting with its G star companion. Its observation by CoRoT provided an extremely high quality ligthcurve. Global parameters could then be improved and new ephemeris for the orbital motion as well as for another long term variation were derived. This long period variation seems to originate from a periodic light attenuation by circumstellar dust. 
HD 174884: Tidally induced pulsations have been detected in the high eccentricity (e=0.29) and short period binary system HD 174884 consisting of two B stars. The upper panel of the figure shows the full light curve of the system. In the second panel tiny secondary eclipses are seen with a depth of about 1% of the depth of the primary eclipse. Actually the system is formed of stars of similar mass, size and temperature. Were the orbit circular, the eclipses would be similar in depth. However the orbit is highly eccentric and its orientation in space with respect to us is such that the secondary eclipse occurs when the stars are at a larger distance than at primary eclipse. The third panel of the figure shows the projection on the plane of the sky (i.e. the system as we see it) at different orbital phases.
CoRoT 102918586 (alias CoRoT Sol 1): The relatively bright eclipsing system CoRoT 102918586 is a double-lined spectroscopic binary, observed by CoRoT, which revealed clear evidence of γ Doradus type pulsations. In addition to CoRoT photometry, a spectroscopic follow-up was performed which yielded the radial velocity curves, the component effective temperatures, the metallicity, and the line-of-sight projected rotational velocities. The eclipsing binary light curve analysis, combined with the spectroscopic results, provided system physical parameters with 1–2% accuracy while the comparison with evolutionary models led to constraints on the age of the system. After subtracting the best–fitting eclipsing binary model, the residuals were analyzed to determine the pulsation properties. The primary star pulsates with typical γ Dor frequencies and shows a period spacing consistent with high order g-modes of degree l=1.
HR 6902: The binary system ζ Aurigae HR 6902 containing a red giant and a B star was observed by CoRoT during two runs, which allowed us to fully cover the primary as well as the secondary eclipses. This system is presently being analyzed with the ultimate goal of bringing new constraints on the internal structure of the red giant in particular.
A low mass binary: One of the binary system observed by CoRoT is of particular interest since the less massive component is a late M star of 0.23 M⊙ with an estimated effective temperature of about 3000 K. The primary component is a 1.5 M⊙ star MS star.
 A beaming effect in a binary: A binary system observed by CoRoT showed out of eclipses variations which were interpreted as a beaming effect (also called Doppler boosting). This effect results from the variation in brightness of source approaching or moving away from the observer, with an amplitude proportional to the radial velocity divided by the speed of light. The periodic variation in the velocity of an orbiting star will thus produce a periodic beaming variation in the light curve. Such an effect can confirm the binary nature of a system even without any detectable eclipses nor transits. One of the main advantages of the beaming effect is the possibility to determine the radial velocity directly from the light curve but very different luminosities of the binary components are required and a single radial velocity curve can only be obtained as in an SB1 binary system. The out of eclipse variations were modeled with the BEER (Beam
CoRoT