The simulated features of heliospheric cosmic-ray modulation with a time-dependent drift model. III - General energy dependence

Details The simulated features of heliospheric cosmic-ray modulation with a time-dependent drift model. III - General energy dependence The simulated features of heliospheric cosmic-ray modulation with a time-dependent drift model. III - General energy dependence

Jun 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992apj...392..300p&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 392, no. 1, June 10, 1992, p. 300-309. Research supported by University of

Astronomy and Astrophysics

Astrophysics

21

Astronomical Models, Galactic Cosmic Rays, Interplanetary Medium, Particle Acceleration, Solar Activity, Heliosphere, Interplanetary Magnetic Fields, Solar Protons, Transport Theory

Scientific paper

The time-dependent cosmic-ray transport equation is solved numerically in an axially symmetric heliosphere. Gradient and curvature drifts are incorporated, together with an emulated wavy neutral sheet. This model is used to simulate heliospheric cosmic-ray modulation for the period 1985-1989 during which drifts are considered to be important. The general energy dependence of the modulation of Galactic protons is studied as predicted by the model for the energy range 1 MeV to 10 GeV. The corresponding instantaneous radial and latitudinal gradients are calculated, and it is found that, whereas the latitudinal gradients follow the trends in the waviness of the neutral sheet to a large extent for all energies, the radial gradients below about 200 MeV deviate from this general pattern. In particular, these gradients increase when the waviness decreases for the simulated period 1985-1987.3, after which they again follow the neutral sheet by increasing rapidly.

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