Manifestations of solar differential rotation in the solar wind: An update

Details Manifestations of solar differential rotation in the solar wind: An update Manifestations of solar differential rotation in the solar wind: An update

May 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008agusmsh31a..02l&link_type=abstract

American Geophysical Union, Spring Meeting 2008, abstract #SH31A-02

Physics

2102 Corotating Streams, 2134 Interplanetary Magnetic Fields, 2162 Solar Cycle Variations (7536), 2169 Solar Wind Sources

Scientific paper

It has been appreciated for decades that the periodicity of recurring fast solar wind streams is seen most prominently and clearly around solar minimum. An updated, synoptic overview of the corotating structure as seen in the ACE and the recent STEREO data illustrates how long-lived some of its source regions appear to be, spanning many months in some cases and even occasionally reappearing months later. We show how these features appear throughout Solar Cycle 23. We also show how the solar latitude of the source(s) determines their periodicities, and note that solar differential rotation may be a consideration in the formation of some stream interaction regions. We use the WSA/ENLIL model developed by CISM (Center for Integrated Space Weather Modeling), now available at the Community Coordinated Modeling Center (CCMC), to identify the coronal hole sources of the fast solar wind stream structures. The WSA/ENLIL model describes the steady solar wind structure and its origins in the corona, based on photospheric magnetic field synoptic maps.

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