'Crossing' method for studying the turbulence in solar and stellar atmospheres. I - Application to the sun

Details 'Crossing' method for studying the turbulence in solar and stellar atmospheres. I - Application to the sun 'Crossing' method for studying the turbulence in solar and stellar atmospheres. I - Application to the sun

Aug 1986

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986soph..106..237g&link_type=abstract

Solar Physics (ISSN 0038-0938), vol. 106, Aug. 1986, p. 237-247.

Statistics

Computation

8

Atmospheric Turbulence, Computational Astrophysics, Solar Atmosphere, Stellar Atmospheres, Stellar Spectra, Abundance, Iron, Oscillator Strengths, Photosphere, Velocity Distribution

Scientific paper

A new 'crossing' method for the study of turbulent velocities in solar and stellar photospheres is considered. The method does not need knowledge of the abundance and oscillator strengths for determining the microturbulent velocity, if the macroturbulent velocity is adopted; or it allows investigation of the microvelocities and macrovelocities simultaneously, if the abundance and oscillator strengths are known. Using the crossing method for 200 lines of neutral iron, microturbulent velocities are obtained for a large range of depths in the solar photosphere. The distribution of macroturbulent velocities with depth is also investigated. The total velocity field calculated from the obtained microvelocities and macrovelocities agrees with previous results from independent methods. This demonstrates the reliability of using the crossing method for separate determination of the microturbulent and macroturbulent velocities in solar and stellar atmospheres.

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