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Macro-microturbulence in the solar photosphere

The velocity distribution of the large and small-scale motion in solar photosphere has been obtained by crossing method based on fitting the observed and calculated equivalent widths as well as the central depths of the spectral lines at the center of the and the limb of the solar disk. We used about 200 Fe I lines. According to our results the motions in photosphere are anisotropic. The radial component of microturbulent velocity decreases from 1.0 to 0.3 km/s and the tangential one from 1.7 to 1.3 km/c at the photosphere heights from 200 to 500 km (log tau_5 = -1.4 and -3.5). At the same heights the radial component of the macroturbulent velocity decreases from 1.8 to 1.2 km/s and the tangential one from 2.3 to 0.8 km/s.