Statistics – Computation
Scientific paper
Jul 1981
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1981georl...8..837j&link_type=abstract
Geophysical Research Letters, vol. 8, July 1981, p. 837-839.
Statistics
Computation
8
Computerized Simulation, Cosmic Rays, Heliosphere, Interplanetary Magnetic Fields, Particle Flux Density, Solar Terrestrial Interactions, Diffusion Coefficient, Drift, Galactic Radiation, Magnetic Field Configurations, Perturbation Theory, Solar Cycles, Solar Wind Velocity
Scientific paper
Results are presented of numerical simulations of cosmic ray drift due to perturbations in the interplanetary medium affecting solar-terrestrial parameters. Computations were performed for a model spherical heliosphere of radius 25 AU, with an interplanetary magnetic field in the shape of an Archimedean spiral with magnitude of 5 gamma at 1 AU, corresponding to a wind velocity of 400 km/sec, and diffusion coefficients corresponding to the assumption that the parallel mean free path is somewhat larger han the cyclotron radius at earth orbit, and its spatial dependence is proportional to the gyroradius. It is found that perturbations in the heliospheric equatorial regions affect galactic cosmic rays more effectively when the Northern Hemisphere heliospheric magnetic field is directed inward rather than outward, with perturbations in the parallel drift coefficient more effective than perturbations in solar wind velocity or perpendicular drift velocity. Results are consistent with the observed variation of the correlation between the geomagnetic aa index and the neutron monitor counting rate on Mt. Washington with the solar cycle.
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