We examine the effects of acoustic-gravity waves with long and short periods on the solar profile of the K1 7699 line using a dynamic model of line formation.
First we studied the kinetic equilibrium of the K I atoms in a static atmosphere confirming, with up-to-date atomic data and atmospheric model, that a good fit of the resonance line 7699 is possible only when non-LTE effects are accounted for.
Then the static non-LTE line source function and lower-level population are used as input data for calculating the line formation in the presence of waves.
The time behaviour of the synthetic profiles corresponding to 300 s and 30 s waves is extensively discussed. The characteristic redshift induced by the 30 s wave is explained within the framework of the S-S line formation model. Long-period waves yield an anticorrelation between the asymmetry at different residual intensities and the line core shift, as observed. The short-period waves with velocity amplitude of about 100 m s-~ (at the base of the photosphere) produce a mean bisector whose lower part has a slope in agreement with the observed one. The efficiency of waves to produce macro and microturbulence is also discussed.