Dynamics of the upper solar photosphere

Details Dynamics of the upper solar photosphere Dynamics of the upper solar photosphere

Apr 2000

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000a%26a...356..308h&link_type=abstract

Astronomy and Astrophysics, v.356, p.308-314 (2000)

Astronomy and Astrophysics

Astrophysics

14

Convection, Sun: Atmosphere, Sun: Granulation, Sun: Photosphere

Scientific paper

The dynamics of the upper solar photosphere was studied by using 1-D photospheric line spectrograms obtained using the VTT of the Observatorio del Teide. Three spectral lines with line core formation heights between 250 and 500 km were analyzed. It is clearly seen that at these levels the velocity and intensity fields are highly correlated but different from the lower lying zone where convective motions predominate. This is shown by classical methods (using correlations and bisectors) as well as by applying the Hurst exponent method to the data.

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