Abstract
Tests made with a standard, purely radiative hydrodynamical code show that sustained double-mode pulsations of RR Lyrae models with the observed periods are possible. The basic difference with our previous simulations is that the new ones have less dissipation due to reduced artificial viscosity. As a result, some models have larger amplitudes than those given by the observations. The double-mode behavior is demonstrated for several models in a sequence that is representative of Oosterhoff II variables. Similar results are also found for Oosterhoff I stars
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