  Response functions to perturbations in the temperature, pressure,
microturbulent velocity, and magnetic intensity were calculated for the Stokes
parameter profiles of the lines Fe I 525.06, 525.02 and Fe II 614.92 nm. The
procedure proposed by Grossmann-Doerth, Larsson, and Solanki (1988) was used.
We show that the depression response functions may be used not only to
determine the depths at which changes in the physical conditions affect most
effectively the absorption and emission in the continuum and in lines, but to
estimate the response of Stokes profiles as well. The response was estimated
using sensitivity indicators calculated as an integral of the response function
over all photospheric layers. An anomalous temperature sensitivity was found
for the Stokes profiles in lines with high excitation and ionization potentials
such as the lines of O I, C I, Fe II. The depression of such lines increases
rather than decreases with growing temperature. The magnetic sensitivity of
Stokes profiles depends primarily on the magnetic field conditions. The
response of V profiles is the greatest under the weak-field and
intermediate-field conditions for photospheric lines with large values of the
Lande factor, wavelength, and equivalent width. The results of calculations of
sensitivity indicators are presented for magnetic lines together with the
indices of magnetic and temperature enhancement.
