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The micro-macroturbulence model of velocity fields is applied to 20 lines taken from a solar flux spectrum obtained with high photometric precision and high spectral resolution. The analysis is performed first by adopting a value of 1.9 km/s for the sun's rotational velocity and then by treating the rotational velocity as an unknown. The results obtained are compared with those of previous intensity profile analyses. It is concluded that if the sun were seen as a distant (unresolved) star, it would be interpreted as having a classical microturbulence dispersion of 0.5 + or - 0.1 km/s along with a radial-tangential macroturbulence characterized by a dispersion of 3.1 + or - 0.1 km/s.
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David F. Gray (1977) studied this question.
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