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The amplitude of solar p-mode oscillations is governed by stochasticexcitation and mode damping, both of which take place in the surface convectionzone. However, the time-dependent, turbulent nature of convection makes itdifficult to self-consistently study excitation and damping processes throughthe use of traditional one-dimensional hydrostatic models. To this end, wecarried out \textit{ab initio} three-dimensional, hydrodynamical numericalsimulations of the solar atmosphere to investigate how p-modes are driven anddissipated in the Sun. The description of surface convection in the simulationsis free from the tuneable parameters typically adopted in traditionalone-dimensional models. Mode excitation and damping rates are computed based onanalytical expressions whose ingredients are evaluated directly from thethree-dimensional model. With excitation and damping rates both available, weestimate the theoretical oscillation amplitude and frequency of maximum power,$\nu_{\max}$, for the Sun. We compare our numerical results with helioseismicobservations, finding encouraging agreement between the two. The numericalmethod presented here provides a novel way to investigate the physicalprocesses responsible for mode driving and damping, and should be valid for allsolar-type oscillating stars.

The amplitude of solar p-mode oscillations from three-dimensional convection simulations