Characteristics Of Blinkers Observed With CDS

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Blinkers are transient brightenings seen in the extreme ultraviolet. They probably can not heat the corona, but are candidates for microflare activity. Here we determine their properties on the basis of a larger sample than previously studied. We used the Normal Incidence Spectrometer of the Coronal Diagnostic Spectrometer (CDS) onboard the SOHO satellite in its movie mode, i.e. 90"x240" slit, to find evidence for blinkers in the quiet Sun. The He I 584.3 A (20'000 K), the O V 629.7 (250'000 K) and the Mg IX 368.1 (1'000'000 K) lines are recorded simultaneously at a cadence of 31 seconds for a duration of 4 hours each on December 3 1996. Harrison (1997) defined the blinker as a phenomenon showing an enhancement of a factor 2-3 in the flux of transition region lines at network junctions. The criterion we used was similar to his. We applied the threshold to the O V line, and identified 74 distinct blinkers. The average properties of these blinkers and the scatter around these mean values were then determined. These properties include the duration of the blinker, the energy content of the event, ratio of maximum to minimum brightness and the sizes of these brightenings. We find that the overall brightening is often composed of a number of shorter events. Finally, we checked if these blinkers were also present in the images obtained in the two other lines, of He I and Mg IX. In the He I line we found 65 events and in the Mg IX line 16 events. On average the brightening was smaller in these lines than in O V. The work is still in progress. We plan to investigate how the locations of these events are related to the distribution of the magnetic field and if they are also related to other phenomena. References: Harrison, R.A.: 1997, Solar Physics 162, 467.

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