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 Aeronomie, D-37189 Katlenburg-Lindau, Germany
3Kiepenheuer-Institut für Sonnenphysik, D-79104 Freiburg, Germany
SOHO/CDS measurements of emission in the network of the quiet solar atmosphere near disk center were used to derive mutual relations of emission and dynamics in different temperature regimes in/above supergranular network. Cross-correlation functions of the line intensities and the Doppler shifts of the chromospheric line He I 584.3 A, the transition region line O V 629.7 A and the coronal line Mg IX 396.1 A,were calculated in order to study relative variability of different atmospheric layers. Relatively high correlations were found between the intensities and the Doppler shifts of the He I and O V lines with two peaks of the intensity correlation function. The maximum value of the correlation of intensities (CC_max=0.86) was reached for the zero time lag and the second maximum (CC=0.78) was obtained for the time lag -190s (O V precedes He I). Only one sharp peak (CC_max=0.55) was detected in the Doppler shift correlation function of these lines for the zero time lag. For the correlation of O V and Mg IX intensities one peak (CC_max=0.57) of the correlation function was also discovered for the time lag +150s (Mg IX falls behind O V). In contrast, no correlation was obtained for the Doppler shifts of the O V and Mg IX lines. Summarizing we can assume clear relation in energy transfer and/or mass motion between chromosphere and transition region but no relation was found between corona and the lower parts of the solar atmosphere above the particular network under study.
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