Non-polar Coronal Holes and Solar Wind

Details Non-polar Coronal Holes and Solar Wind Non-polar Coronal Holes and Solar Wind

Dec 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010agufmsh11b1668k&link_type=abstract

American Geophysical Union, Fall Meeting 2010, abstract #SH11B-1668

Astronomy and Astrophysics

Astrophysics

[7509] Solar Physics, Astrophysics, And Astronomy / Corona, [7511] Solar Physics, Astrophysics, And Astronomy / Coronal Holes, [7549] Solar Physics, Astrophysics, And Astronomy / Ultraviolet Emissions

Scientific paper

We investigate properties of non-polar coronal holes (CHs) and their correlation with fast solar wind at 1 AU. Using EIT/SOHO observations taken from 1998-2008 in 195A and 284A wavelength bands, we identify boundaries of coronal holes, and compute their area, total brightness of corona integrated over the CH, as well as the area and total brightness of pixels inside the CH associated with coronal bright points (CBPs). We investigate the effect of each parameter on solar wind speed, the mutual dependency of the parameters, and their changes with the sunspot activity. Our findings suggest that the reconnection events associated with coronal bright points situated in CHs do not play a major role in acceleration of the fast solar wind.

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