Analysis of Intensities, Line Widths and Line Shifts during Blinkers

Details Analysis of Intensities, Line Widths and Line Shifts during Blinkers Analysis of Intensities, Line Widths and Line Shifts during Blinkers

Jan 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004esasp.547..251b&link_type=abstract

Proceedings of 'SOHO 13 - Waves, Oscillations and Small-Scale Transient Events in the Solar Atmosphere: A Joint View from SOHO a

Computer Science

Sun: Chromosphere, Sun: Corona, Sun: Transition Region, Sun: Uv Radiation

Scientific paper

Explosive events and blinkers are two major observational classes of transients seen on the quiet Sun. We analysed five time-series spectra of transition region lines O V 629 Å, O VI 1032 Å and O VI 1038 Å and detected 209 blinkers and 55 explosive events. In 44 cases both events were present at the same pixel simultaneously. This means that about 21% of blinkers coincided with explosive events and that 80% of explosive events had intensity enhancements typical for blinkers on the time scale longer than an hour. In more than a half of the eleven remaining explosive events we found that intensity enhancements relative to the pre-event level were on average on the 100% level on the time scale somewhat longer than duration of explosive event, i.e., shorter than ten minutes. The blinkers without an explosive event signature could be separated into two observational classes: 1) Simple blinkers with smooth increase in intensity having only one significant peak and 2) Complex or oscillating blinkers characterised by multiple (2-4) significant peaks. By percentage the class 1) was represented with about 45% and the class 2) with about 34%.

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