  Velocity oscillations "measured" simultaneously at the photosphere and the
chromosphere -from time series of spectropolarimetric data in the 10830 A
region- of different solar magnetic features allow us to study the properties
of wave propagation as a function of the magnetic flux of the structure (i.e.
two different-sized sunspots, a tiny pore and a facular region). While
photospheric oscillations have similar characteristics everywhere, oscillations
measured at chromospheric heights show different amplitudes, frequencies and
stages of shock development depending on the observed magnetic feature. The
analysis of the power and the phase spectra, together with simple theoretical
modeling, lead to a series of results concerning wave propagation within the
range of heights of this study. We find that, while the atmospheric cut-off
frequency and the propagation properties of the different oscillating modes
depend on the magnetic feature, in all the cases the power that reaches the
high chromosphere above the atmospheric cut-off comes directly from the
photosphere by means of linear vertical wave propagation rather than from
non-linear interaction of modes.
