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Space-borne missions CoRoT and Kepler have provided a rich harvest ofhigh-quality photometric data for solar-like pulsators. It is now possible tomeasure damping rates for hundreds of main-sequence and thousands of red-giant.However, among the seismic parameters, mode damping rates remain poorlyunderstood and thus barely used for inferring the physical properties of stars.Previous approaches to model mode damping rates were based on mixing-lengththeory or a Reynolds-stress approach to model turbulent convection. While ableto grasp the main physics of the problem, those approaches are of little helpto provide quantitative estimates as well as a definitive answer on therelative contribution of each physical mechanism. Our aim is thus to assess theability of 3D hydrodynamical simulations to infer the physical mechanismsresponsible for damping of solar-like oscillations. To this end, a solarhigh-spatial resolution and long-duration hydrodynamical 3D simulation computedwith the ANTARES code allows probing the coupling between turbulent convectionand the normal modes of the simulated box. Indeed, normal modes of thesimulation experience realistic driving and damping in the super-adiabaticlayers of the simulation. Therefore, investigating the properties of the normalmodes in the simulation provides a unique insight into the mode physics. Wedemonstrate that such an approach provides constraints on the solar dampingrates and is able to disentangle the relative contribution related to theperturbation of the turbulent pressure, the gas pressure, the radiative flux,and the convective flux contributions. Finally, we conclude that using thenormal modes of a 3D numerical simulation is possible and is potentially ableto unveil the respective role of the different physical mechanisms responsiblefor mode damping provided the time-duration of the simulation is long enough.

Solar $p$-mode damping rates: insight from a 3D hydrodynamical simulation