Relation of transition region blinkers to the low chromosphere

Details Relation of transition region blinkers to the low chromosphere Relation of transition region blinkers to the low chromosphere

Jul 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003a%26a...406..363b&link_type=abstract

Astronomy and Astrophysics, v.406, p.363-371 (2003)

Astronomy and Astrophysics

Astrophysics

5

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

Scientific paper

We investigated the coupling between the low chromosphere, lower and upper transition region through the study of blinkers. Blinkers are extreme ultraviolet (EUV) small-scale transient brightenings best detected in transition region lines showing an intensity enhancement on the 60-100% level on average. We analysed time-series spectra of the \cii 1037 Å (2-4x 104 K, lower transition region) and \oxvi 1038 Å (3x 105 K, upper transition region) lines, as well as the \ci continuum at 1042 Å formed about 1 Mm above the solar surface, obtained with the Solar Ultraviolet Measurement of Emitted Radiation (SUMER) spectrometer on SOHO. Blinkers detected in \cii and \oxvi have similar enhancement levels. We found a modest space-time overlap between blinkers in the two lines and a small correlation between \cii or \oxvi blinkers and the corresponding light curve in the chromospheric continuum. This suggests a relation of EUV blinkers to the chromosphere, which could support the idea that blinkers are the consequence of granular collisions. The average duration of \oxvi blinkers amounts to 10.0 min and of \cii blinkers to 6.7 min.

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