Coronal response of Bi-directional Jets

Details Coronal response of Bi-directional Jets Coronal response of Bi-directional Jets

May 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004soph..221...51d&link_type=abstract

Solar Physics, v. 221, Issue 1, p. 51-64 (2004).

Physics

7

Scientific paper

EUV bi-directional jets are a prominent class of phenomena characterizing the solar transition region. Using simultaneously obtained SUMER observations in the chromospheric Si ii 1251.16 Å and C i 1251.17 Å, transition region N v 1238.8 Å and coronal Mg x 625 Å lines we show an example of a bi-directional jet observed in the chromospheric and the transition region lines but not showing any detectable signature in the coronal line. The phenomenon, however, was also clearly detected by the TRACE imager with the 171 Å filter. This discrepancy is explained here with a non-Maxwellian electron distribution which makes a significant fraction of the plasma in the TRACE 171 Å pass-band to be derived from temperatures around ≈ 300 000 K, as opposed to ≈ 800 000 K. This could have implications for other phenomena observed in the TRACE pass-bands, including the transition region ‘moss’ and the 3- and 5-min oscillations.

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