A test of the micro-macroturbulence model on the solar flux spectrum

Details A test of the micro-macroturbulence model on the solar flux spectrum A test of the micro-macroturbulence model on the solar flux spectrum

Dec 1977

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1977apj...218..530g&link_type=abstract

Astrophysical Journal, Part 1, vol. 218, Dec. 1, 1977, p. 530-538. Research supported by the National Research Council of Canad

Astronomy and Astrophysics

Astrophysics

48

Magnetohydrodynamic Turbulence, Solar Flux, Solar Spectra, Stellar Models, Microstructure, Solar Rotation, Stellar Spectrophotometry

Scientific paper

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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