  Stellar spectra with a high resolution of 115000 obtained with the HARPS
spectrograph provide an opportunity to examine turbulence velocities and their
depth distributions in the photosphere of stars. Fourier analysis was performed
for 17 iron lines in the spectra of 13 stars with an effective temperature of
4900--6200 K and a logarithm of surface gravity of 3.9--5.0 as well as in the
spectrum of the Sun as a star. Models of stellar atmospheres were taken from
the MARCS database. The standard concept of isotropic Gaussian microturbulence
was assumed in this study. A satisfactory fit between the synthesized profiles
of spectral lines and observational data verified the reliability of the
Fourier method. The most likely estimates of turbulence velocities, the
rotation velocity, and the iron abundance and their photospheric depth
distribution profiles were obtained as a result. Microturbulence does not vary
to any significant degree with depth, while macroturbulence has a marked depth
dependence. The macroturbulence velocity increases with depth in the stellar
atmosphere. The higher the effective temperature of a star and the stronger the
surface gravity, the steeper the expected macroturbulence gradient. The mean
macroturbulence velocity increases for stars with higher temperatures, weaker
gravity, and faster rotation. The mean macro- and microturbulence velocities
are correlated with each other and with the rotation velocity in the examined
stars. The ratio between the macroturbulence velocity and the rotation velocity
in solar-type stars varies from 1 (the hottest stars) to 1.7 (the coolest
stars). The age dependence of the rotation velocity is more pronounced than
that of the velocity of macroturbulent motions.
