High-latitude activity and its relationship to the mid-latitude solar activity

Details High-latitude activity and its relationship to the mid-latitude solar activity High-latitude activity and its relationship to the mid-latitude solar activity

Dec 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008agufmsh51a1590b&link_type=abstract

American Geophysical Union, Fall Meeting 2008, abstract #SH51A-1590

Physics

2162 Solar Cycle Variations (7536), 7509 Corona, 7524 Magnetic Fields, 7536 Solar Activity Cycle (2162), 7549 Ultraviolet Emissions

Scientific paper

The high-latitude activity at photosphere and corona, and their relation to the mid-latitude activity in cycle 23 have been explored using the MDI magnetic synoptic maps available on the SOHO web page with a new calibration and EIT synoptic maps. The EIT synoptic maps of EUV images in three lines Fe and in one line He II (171A, 195A, 284A and 304A) are obtained for period June 1996 - May 2006 (CR1911-CR2042) from the full disk EIT images. They are represented by values of the line intensity centered on the central meridian and can be directly compared with magnetic synoptic maps (MDI maps). It is found that the solar cycle dependence of the EUV polar corona occurs because of the large-scale topology of the solar corona and its relationship with the mid-latitude magnetic flux. It is seen more pronounced on the rising phase of the solar cycle due to the connectivity of the coronal structures extended from the mid-latitude to the high-latitude. But, after the solar cycle maximum the EUV polar corona shows a less dependence of the mid-latitude corona. In the polar regions the absent of the correlation of the unsigned magnetic flux and EUV corona occurs not only due to the effect of projection. But it tells us about the numerous emerging bi-polar and unipolar regions inside the polar region which does not contribute to the brightness of the EUV corona. Really, during the solar minimum when the polar magnetic field reaches its maximum and number of unipolar magnetic regions of strong magnetic field increases, we observe dimming and coronal holes instead of the bright EUV corona.

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