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We have developed a three-dimensional radiation hydrodynamics code tosimulate the interaction of convection and radial pulsation in classicalvariable stars. One key goal is the ability to carry these simulations to fullamplitude in order to compare them with observed light curves. Previousmulti-dimensional calculations were prevented from reaching full amplitudebecause of drift in the radial coordinate system, due to the algorithm definingradial movement of the coordinate system during the pulsation cycle. We haveremoved this difficulty by defining our radial coordinate flow algorithm torequire that the mass in a spherical shell remains constant for every time-stepthroughout the pulsation cycle. We have used our new code to perform 2Dsimulations of the interaction of radial pulsation and convection. We have madecomparisons between light curves from our 2D convective simulations withobserved light curves and find that our 2D simulated light curves are betterable to match the observed light curve shape near the red edge of the RR Lyraeinstability strip than light curves from previous 1D time dependent convectivemodels.

Radial Stellar Pulsation and Three-Dimensional Convection. II. Two-Dimensional Convection In Full Amplitude Radial Pulsation