In this contribution we present an observational study of the interaction of the photosphere with chromospheric layers by studying the correlations between emissions at varying temperature from the temperature minimum region (UV continuum at 1600 A from TRACE) through the low chromosphere (CaII K line from BBSO) to the middle chromosphere (continuum at 3.5 mm from BIMA) and photospheric magnetic field from MDI/SOHO.

We report a high degree of correlation between considered emissions formed at different heights in the chromosphere. A power law was found to be a good representation for the relationship between photospheric magnetic field and chromospheric emissions at all wavelengths. Power laws also describe the chromospheric flux-flux relationships. Our analysis shows that the dependence of chromospheric intensities on magnetic field is different for the network and internetwork regions. In the network the power-law exponent in the relation between the chromospheric brightness and magnetic flux is
close to 0.5-0.6 while almost no dependence on magnetic flux is found for the cell interiors.
The obtained results support the idea of different heating mechanisms acting in the network (magnetic) and cell interiors (acoustic).