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Astron. Astrophys. 356, 308-314 (2000)

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Dynamics of the upper solar photosphere

A. Hanslmeier 1, A. Kuera 2, J. Rybák 2, B. Neunteufel 1 and H. Wöhl 3

1 Institute for Geophysics, Astrophysics and Meteorology, Universitäts-Platz 5, 8010 Graz, Austria (arh@igam06ws@kfunigraz.ac.at)
2 Astronomical Institute of the Slovak Academy of Sciences, 05960, Tatranska Lomnica, Slovakia
3 Kiepenheuer-Institut für Sonnenphysik, Schöneckstrasse 6, 79104 Freiburg, Germany (hw@kis.uni-freiburg.de)

Received 16 June 1999 / Accepted 3 January 2000


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.

Key words: convection – Sun: atmosphere – Sun: granulation – Sun: photosphere

Send offprint requests to: A. Hanslmeier

© European Southern Observatory (ESO) 2000

Online publication: March 28, 2000