Astronomy and Astrophysics – Astrophysics
Scientific paper
Nov 1990
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990a%26a...239..340k&link_type=abstract
Astronomy and Astrophysics (ISSN 0004-6361), vol. 239, no. 1-2, Nov. 1990, p. 340-346. Research supported by DFG.
Astronomy and Astrophysics
Astrophysics
45
Luminous Intensity, Photosphere, Power Spectra, Solar Atmosphere, Vertical Distribution, Fraunhofer Lines, Line Spectra, Solar Radiation
Scientific paper
The results are presented of a power and coherence analysis of intensity variations derived from the wings of the solar Mg b2 line. It is found that the power spectra can be represented by a power law function in the range of wavenumbers between 2.8/Mm. The deep photosphere shows the Kolmogorov (-5/3)-scaling law. The values of the exponent and also of the rms intensity itself decrease with height, attain a minimum, and increase again. While small structures are coherent up to higher photospheric layers, the coherence of the larger structures breaks down in the same layer where the rms intensity shows its minimum. It is concluded that the large intensity structures reflect the effect of convective overshoot, and the breakdown of the coherence reflects the disappearance of convective structures up to a certain height in the photosphere, while the small structures are of turbulent origin.
Komm Rudi
Mattig Wolfgang
Nesis Anastasios
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