The ANTARES code has been designed for simulation of astrophysical flows in a variety of situations, in particular in the context of stellar physics. Here, we describe extensions as necessary to model the interaction of pulsation and convection in classical pulsating stars. These extensions comprise the introduction of a spherical grid, moveable in the radial direction, specific forms of grid-refinement and considerations regarding radiative transfer. We then present the basic parameters of the Cepheid we study more closely. For that star we provide a short discussion of patterns of the H + He I and the Hell convection zones and the interaction with pulsation seen in the pdV work or atmospheric structures.
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