We carry out two-dimensional (2-D) and three-dimensional(3-D) radiation-hydrodynamics (RHD) simulations of surface convection in stellar atmospheres warmer than the Sun (namely, with effective temperatures spanning 6600−9000 K) using the ANTARES numerical code. The resulting datasets will be used: 1) as benchmark to improve multi-dimensional atmospheric models for this type of stellar objects; 2) as the basis for computing synthetic spectra and other observable signatures (e. g. for asteroseismology applications) of the physical properties of relevant target stars; and 3) to investigate the stability of stellar irradiance on the time scales spanned by our simulations. We will continue extending the simulations to cover a time duration of up to several stellar days to study p-mode excitation and damping processes. Here, we present the planned grid of simulations and first results.