Understanding structures at the base of the solar corona - polar plumes

Details Understanding structures at the base of the solar corona - polar plumes Understanding structures at the base of the solar corona - polar plumes

Mar 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009iaus..257..145g&link_type=abstract

Universal Heliophysical Processes, Proceedings of the International Astronomical Union, IAU Symposium, Volume 257, p. 145-149

Astronomy and Astrophysics

Astronomy

Sun: Corona, Solar Wind

Scientific paper

Recent work on coronal polar plumes (Gabriel et al. 2003, 2005) has aimed at determining the outflow velocity in plume and interplume regions, using the Doppler dimming technique on oxygen VI observations by SUMER and UVCS on SOHO. By comparing observations of SOHO/EIT with plume modelling, we show that the major part of plumes is the result of chance alignments along the line-of-sight of small enhancements in intensity. This confirms the so-called curtain model. These plumes can be attributed to reconnection activity along the boundaries of supergranule cells. A second population of plumes has a lower abundance and arises from surface bright points having a particular magnetic configuration. New observations using the Hinode/EIS spectrometer are in progress, with the aim of providing further insight for this model.

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