Dynamics of the upper solar photosphere

The dynamics of the upper solar photosphere was studied by using 1-D photos pheric line spectrograms obtained using the VTT of the Observatorio del Tei de. Three spectral lines with line con formation heights between 250 and 50 0 km were analyzed. It is clearly seen that at these levels the velocity an d intensity fields are highly correlated but different from the lower lying tone where convective motions predominate. This is shown by classical meth ods (using correlations and bisectors) as well as by applying the Hurst exp onent method to the data.