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Convection plays an essential role in the emerging intensity for many starsthat will be observed by Gaia. Convective-related surface structures affect theshape, shift, and asymmetry of absorption lines, the phocentric and photometricvariability causing bias in Gaia measurements. Regarding the importance of Gaiamission and its goals, it is mandatory to have the best models of the observedstars. 3D time-dependent hydrodynamical simulations of surface convection arecrucial to model the photosphere of late type stars in a very realistic way.These simulations are an important tool to correct the radial velocities andbetter estimates the parallaxes and photometric variability.

3D hydrodynamical model atmospheres: a tool to correct radial velocities and parallaxes for Gaia