On the Solar Wind Ion Composition Properties With Source Regions from Low-Latitude and Polar Coronal Holes of Opposite Polarity

Details On the Solar Wind Ion Composition Properties With Source Regions from Low-Latitude and Polar Coronal Holes of Opposite Polarity On the Solar Wind Ion Composition Properties With Source Regions from Low-Latitude and Polar Coronal Holes of Opposite Polarity

Dec 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011agufmsh43f..04k&link_type=abstract

American Geophysical Union, Fall Meeting 2011, abstract #SH43F-04

Astronomy and Astrophysics

Astrophysics

[2164] Interplanetary Physics / Solar Wind Plasma, [2169] Interplanetary Physics / Solar Wind Sources, [7511] Solar Physics, Astrophysics, And Astronomy / Coronal Holes, [7524] Solar Physics, Astrophysics, And Astronomy / Magnetic Fields

Scientific paper

During Years 2004-2007 there were frequent appearances of low-latitude coronal holes (CHs) and low-latitude extension of polar CHs. These CHs were the source regions of the solar wind measured in-situ at L1. We find that the ion composition has distinct properties between solar wind originating from CHs of opposite polarity. Specifically, the charge states measured by ACE/SWICS were systematically lower-ionized for solar wind ions from CHs of positive polarity (the 'south CH') than those of negative polarity (the 'north CH'), regardless of the solar wind speed. Such differentiation is apparent only in the low-latitude extension of polar CHs and those non-polar CHs with predicted footpoints at latitude higher than 15 degrees. Interestingly, earlier work based on Ulysses fast wind data during the declining/minimum phase of Cycle 22 found that it was the north polar CH that was associated with lower solar wind charge states, opposite to what we found in the following solar cycle. We present these results and search for solar properties that may be factors that govern this north-south difference.

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