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Visualization of the microturbulence distribution on the surface of the Sun

A technique is described that can be used to obtain approximate values of microturbulent velocity v mi by comparing theequivalent widths of two spectral lines Fe I λ 6302 and 6301 Å. A map of the distribution of microturbulence over a solarsurface are given according to the observational data of Hinode SOT/SP. It is shown that v mi correlates with the line ofsight (LOS) velocity gradient and that it does not correlate with the solar surface brightness and LOS velocity itself.