Solar Wind Structural and Magnetic Field Changes Associated With 11-yr Cosmic Ray Modulation at 1 AU

Details Solar Wind Structural and Magnetic Field Changes Associated With 11-yr Cosmic Ray Modulation at 1 AU Solar Wind Structural and Magnetic Field Changes Associated With 11-yr Cosmic Ray Modulation at 1 AU

May 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002agusmsh32a..07c&link_type=abstract

American Geophysical Union, Spring Meeting 2002, abstract #SH32A-07

Physics

2102 Corotating Streams, 2104 Cosmic Rays, 2111 Ejecta, Driver Gases, And Magnetic Clouds, 2134 Interplanetary Magnetic Fields, 2162 Solar Cycle Variations (7536)

Scientific paper

Using a recent classification of the solar wind at 1 AU into its principal components (slow solar wind, high-speed streams, and coronal mass ejections (CMEs; including shocks and post shock flows)) for 1972-2000, we show that the galactic cosmic ray intensity is anti-correlated with the percentage of time (each month) that the Earth is imbedded in CME flows. We suggest that this correlation results primarily from a CME-related change in the tail of the distribution function of hourly-averaged values of the solar wind magnetic field (B) between solar minimum and solar maximum. The number of high-B values (> 10 nT) increases by a factor of three from minimum to maximum, with 70% of this increase due to CMEs. On an hour-to-hour basis, average changes of cosmic ray intensity become negative for solar wind magnetic field values > 10 nT. These findings indicate a central role for CMEs for 11-yr modulation at 1 AU. Strong (> 10 nT) fields in the interaction regions between high and low speed streams appear to have been responsible for the cosmic ray "mini-cycles" in 1973 and 1974.

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