F. Tomasz1,
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
Results of spectral analysis of a blinker observed in the transition region O VI 1037.63 AA line and in the chromospheric Ly beta 1025.72 A line which were acquired using the SUMER spectrometer are presented. Chromospheric and coronal plasma in the vicinity of the blinker are investigated using also TRACE Ly alpha, UV continuum and Fe IX channels. It was found that initial release of energy was localized in the transition region and plasma has been spreading from transition region as a bi-directional jet. Energy reached chromosphere ~60 seconds after primary emission in the O VI line. There were detected enhanced emissions for about 25-38% in the chromospheric Ly alpha and UV continuum. Spatial extent of the blinker response is 6'' along the slit in the Ly alpha filtergram what is ~3'' less than extent of the blinker in the O VI line. Maximum extent of the blinker response is 7.5'' in Ly alpha filtergram. Although, both Ly alpha and UV continuum reflect physical conditions in chromosphere, their patterns are completely different: the blinker response is compact in the Ly alpha and UV continuum shows incompact structure below the transition region blinker. Coronal plasma was not influenced by the blinker although plasma moving toward observer was detected in the final phase of evolution of the blinker.
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