Coronal structures following sunspot maximum

Coronal structures following sunspot maximum

. Miloslav Druckmuller and Peter Aniol took this image of the solar corona during the total eclipse of 29 March 2006 from Libya. At this time, the Sun was in a declining phase from a maximum in the solar activity cycle, in 2000, so polar coronal holes, with their radial magnetic fields, were well developed, but active regions were still present at a variety of solar latitudes. The bulk of the long fine rays arise from polar and low-latitude plumes that overlie small magnetic bipoles inside coronal holes, helmet streamer rays that overlie large loop arcades and separate coronal holes of opposite polarity, and “pseudostreamer” rays that overlie twin loop arcades and separate coronal holes of the same polarity. [Courtesy of Miloslav Druckmüller, Peter Aniol and Serge Koutchmy, and adapted from Yi-Ming Wang, et al. (2007).]

Copyright 2010, Professor Kenneth R. Lang, Tufts University