Structure of the extended solar magnetic field and the sunspot cycle variation in cosmic ray intensity

Details Structure of the extended solar magnetic field and the sunspot cycle variation in cosmic ray intensity Structure of the extended solar magnetic field and the sunspot cycle variation in cosmic ray intensity

Aug 1976

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1976natur.262..766s&link_type=abstract

Nature, vol. 262, Aug. 26, 1976, p. 766-768. Research supported by the Max C. Fleischman Foundation, U.S. Navy, NASA, and NSF.

Computer Science

25

Magnetic Field Configurations, Primary Cosmic Rays, Solar Magnetic Field, Sunspot Cycle, Galactic Radiation, Interplanetary Magnetic Fields, Particle Flux Density, Photosphere, Polar Regions, Solar Wind

Scientific paper

It is proposed that a relation exists between the extent of interplanetary-magnetic-field sectors and observed variations in cosmic-ray intensity at earth. Changes that take place in the sector magnetic fields and solar polar fields during a sunspot cycle are described. It is argued that a geometrical effect arising from changes in sector-field and polar-field extent during sunspot cycles may be the principal cause of the 11-yr modulation of cosmic-ray intensity observed at earth. The fraction of the heliosphere occupied by sector fields is estimated as a function of time through an average sunspot cycle, the solid angle of the heliosphere occupied by the extended solar polar fields is plotted through the same cycle, and monthly averages of observed absolute intensities of primary cosmic rays with a rigidity greater than 0.5 GV are compared with the plot of polar-field extent. It is found that the average sunspot-cycle variation of the solid angle of the extended polar fields is rather similar to the observed variation in the flux of the cosmic rays considered.

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