P. Gömöry1,
J. Rybák1,
A. Kucera1,
W. Curdt2,
H. Wöhl3
1Astronomical Institute of the Slovak Academy of Sciences,
SK-05960 Tatranská Lomnica, Slovakia
2Max-Planck-Institut für Sonnensystemforschung, D-37189 Katlenburg-Lindau, Germany
3Kiepenheuer-Institut für Sonnenphysik, D-79104 Freiburg, Germany
The temporal evolution of the spectral parameters of the chromospheric He I 584.33 A and the transition region O V 629.73A emission lines measured by the Coronal Diagnostic Spectrometer (CDS) in/above the supergranular network near disk center was constructed in order to examine the correlation of the spectral line intensities and the Doppler shifts. The arithmetic process of the correct calculation of the cross-correlation function is shown here in details. The necessity of edge data removal and the subtraction of any background trends before applying the cross-correlation function was revealed. The method was verified using the test example of two ideal sinusoidal functions. Resulting cross-correlation functions were analyzed with a view to describe energy transfer and mass motion between chromosphere and transition region in the particular network. The maximum value (CCmax=0.46) of the cross-correlation function of the He I and the O V line intensities was achieved for a time lag of +27.3s, i.e. some changes in the O V line intensities precede changes in the He I line intensities. In contrast, the cross-correlation function of the Doppler shifts of these lines reached the maximum value (CCmax=0.53) for a time lag of 0 seconds. In summary, we can assume that the non-radiative energy was transported from the transition region down to the chromosphere without any significant mass motion in the studied network element.
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