Manifestations of cyclic variations in the solar magnetic field in long-term modulation of cosmic rays

Details Manifestations of cyclic variations in the solar magnetic field in long-term modulation of cosmic rays Manifestations of cyclic variations in the solar magnetic field in long-term modulation of cosmic rays

Oct 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008ge%26ae..48..571g&link_type=abstract

Geomagnetism and Aeronomy, Volume 48, Issue 5, pp.571-577

Computer Science

1

94.20.Wq

Scientific paper

The possibilities of improving the semiempirical model of cosmic ray (CR) modulation, proposed by us previously, are discussed. The following characteristics have been considered as model parameters in order to describe long-period CR variations using a unified model and to more completely reflect solar cycles in CR modulation as a complex interaction between two systems of fields (large-scale and local): the value and sign of the polar solar field, the average strength of the solar magnetic field (the B ss integral index), partial indices (zone-even ( ZE) and zone-odd ( ZO) and sector-even ( SE) and sector-odd ( SO) indices), the tilt of the heliospheric current sheet, and the special index ( F x ) taking into account X ray flares. The role of each index in CR modulation has been revealed. When we described the long-term CR variations using many parameters and taking into account the integral index or one of four partial indices, the best results of modulation modeling during 1976 1999 were obtained for the B ss total energetic index and SO index. A difference between the model calculations and observations increases beginning from the middle of 2000; the problem features of the CR behavior and the specific features of modeling this behavior in cycle 23 of solar activity (SA) are discussed. It is assumed that a decrease in the CR density at the last SA minimums (from cycle to cycle) can be related to a decrease in the ZO index and to a recently detected similar decrease in the vertical component of the solar dipole magnetic moment.

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