Computer Science
Scientific paper
Apr 2003
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003eaeja....11509j&link_type=abstract
EGS - AGU - EUG Joint Assembly, Abstracts from the meeting held in Nice, France, 6 - 11 April 2003, abstract #11509
Computer Science
Scientific paper
The transport of cosmic rays in the heliosphere is determined mainly by the interplanetary magnetic and its convection with the solar wind. The major transport effects of diffusion and drift both scale inversely with the magnetic-field intensity. So, if the magnetic field intensity varies over time scales of a year or greater, we expect that the galactic cosmic-ray intensity observed in the inner heliosphere will vary, as the particles gain easier or more-difficult access. If the magnetic field is weaker for a significant period of time, the easier access of galactic cosmic rays will raise the observed intensity, and vice versa. The drift of cosmic rays depends, in addition, on the structure of the magnetic field. So, if the magnetic field structure is very complex, the drift motions will be less direct, and the access of the cosmic rays to the inner heliosphere will be more difficult, and the intensity in the inner heliosphere correspondingly lower. We will discuss various scenarios for long-term solar variations and their expected effects on cosmic rays.
Jokipii Randy J.
Kota József
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