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Context. The interpretation of stellar pulsations in terms of internalstructure depends on the knowledge of the fundamental stellar parameters.Long-base interferometers permit us to determine very accurate stellar radii,which are independent constraints for stellar models that help us to locate thestar in the HR diagram. Aims: Using a direct interferometric determination ofthe angular diameter and advanced three-dimensional (3D) modeling, we derivethe radius of the CoRoT target HD 49933 and reduce the global stellar parameterspace compatible with seismic data. Methods: The VEGA/CHARAspectro-interferometer is used to measure the angular diameter of the star. A3D radiative hydrodynamical simulation of the surface is performed to computethe limb darkening and derive a reliable diameter from visibility curves. Theother fundamental stellar parameters (mass, age, and Teff) are found by fittingthe large and small p-mode frequency separations using a stellar evolutionmodel that includes microscopic diffusion. Results: We obtain a limb-darkenedangular diameter of {\theta}LD = 0.445 \pm 0.012 mas. With the Hipparcosparallax, we obtain a radius of R = 1.42 \pm 0.04 Rsun. The correspondingstellar evolution model that fits both large and small frequency separationshas a mass of 1.20 \pm 0.08 Msun and an age of 2.7 Gy. The atmosphericparameters are Teff = 6640 \pm 100 K, log g = 4.21 \pm 0.14, and [Fe/H] =-0.38.

The diameter of the CoRoT target HD 49933. Combining the 3D limb darkening, asteroseismology, and interferometry