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In binaries composed of either early-type stars or white dwarfs, the dominanttidal process involves the excitation of internal gravity waves (IGWs), whichpropagate towards the stellar surface, and their dissipation via nonlinear wavebreaking. We perform 2D hydrodynamical simulations of this wave breakingprocess in a stratified, isothermal atmosphere. We find that, after an initialtransient phase, the dissipation of the IGWs naturally generates a sharpcritical layer, separating the lower stationary region (with no mean flow) andthe upper "synchronized" region (with the mean flow velocity equal to thehorizontal wave phase speed). While the critical layer is steepened byabsorption of these waves, it is simultaneously broadened by Kelvin-Helmholtzinstabilities such that, in steady state, the critical layer width isdetermined by the Richardson criterion. We study the absorption and reflectionof incident waves off the critical layer and provide analytical formulaedescribing its long-term evolution. The result of this study is important forcharacterizing the evolution of tidally heated white dwarfs and other binarystars.

Physics of Tidal Dissipation in Early-Type Stars and White Dwarfs: Hydrodynamical Simulations of Internal Gravity Wave Breaking in Stellar Envelopes