Physics
Scientific paper
May 2008
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008agusmsh44a..02c&link_type=abstract
American Geophysical Union, Spring Meeting 2008, abstract #SH44A-02
Physics
2134 Interplanetary Magnetic Fields, 2164 Solar Wind Plasma, 7537 Solar And Stellar Variability (1650)
Scientific paper
Long-term reconstructions of solar wind parameters have implications for topics ranging from the operation of the solar dynamo to solar variability and climate change. Such reconstructions of the solar wind interplanetary magnetic field (IMF) strength, beginning with the seminal work of Lockwood et al. (1999), have been varied and contentious but appear to be converging along the following lines: an IMF floor of ~4.5 nT in the ecliptic plane on which solar cycle variations (closed flux from coronal mass ejections) ride. A recent reconstruction based on cosmic ray data by McCracken is at variance with this picture, however, and the differences remain to be resolved. The average IMF strength near Earth during 2007 was 4.5 nT (rotation averages from January 2007- present ranged from 4.1-5.2 nT). Annual averages approaching this value were last inferred (via the IDV index) for 1901 and 1902 (both ~4.7 nT). During the last century, it appears that there has been an increase, of unknown cause, in the solar wind speed of ~15%.
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