Nearly everywhere in the Hertzsprung-Russell diagram, internal gravity waves (IGW) are of primary importance to understand the dynamic of the radiative interiors. Their behaviour, directly related to the structure of their resonant cavity, is strongly influenced by rotation. For the stars where they have been observed, standing IGWs, or gravity modes (g modes), have shown evidences of a solid body rotational state for radiative interiors. If we want to probe in the same way the deep regions of solar-like stars, such g-mode observations are required at this range of effective temperatures. However, for these stars, the task is made difficult by the presence of the convective envelope, where IGWs are evanescent. Convective envelopes are found to be shallower in late F-type stars, which still exhibit solar-like acoustic pulsations. Therefore, we want to predict the surface amplitude of stochastically excited g modes for F-type stars with Teff ~ 6350 K. We use 3D simulations as they constitute a powerful tool to explore stellar interior dynamics. In particular, they are able to capture non-linearities of the considered system, especially concerning IGWs stochastic excitation.

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