  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 encomprise the
introduction of a spherical grid, movable 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+HeI and the HeII
convection zones and the interaction with pulsation seen in the pdV work or
atmospheric structures.
