Gradients of galactic cosmic rays and anomalous components

Details Gradients of galactic cosmic rays and anomalous components Gradients of galactic cosmic rays and anomalous components

Apr 1988

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988ippe.conf..135m&link_type=abstract

In Jet Propulsion Lab., California Inst. of Tech., Interplanetary Particle Environment. Proceedings of a Conference p 135-148 (S

Computer Science

Galactic Cosmic Rays, Gradients, Radiation Measurement, Solar Activity, Helium, Relativistic Particles, Solar Cycles

Scientific paper

Measurements of radial and latitudinal gradients of galactic cosmic rays and anomalous components now cover radii from 0.3 to 40 AU from the sun and latitudes up to 30 deg above the ecliptic plane for particle energies from approx. 10 MeV/n up to relativistic energies. The most accurate measurements cover the period 1972 through 1987, which includes more than one full 11 year cycle of solar activity. Radial gradients for glactic cosmic rays of all energies and species are small (similar to less than 10 percent AU), and variable in time, reaching a minimum of near 0 percent AU out to 30 AU for some species at solar maximum. Gradients for anomalous components are larger, of order 15 percent AU, may show similar time variability, and are relatively independent of particle species and energy. For the period 1985 through 1986 the intensity decreased away from the ecliptic for all species and energies. For galactic cosmic rays, the measured gradients are approx. 0.5 percent/degree near 20 AU, while for anomalous components the gradients are larger, ranging from 3 to 6 percent/degree. Comparison with a similar measurement for anomalous helium in 1975 through 1976 suggests that the latitude gradients for anomalous components have changed sign between 1975 and 1985. For galactic cosmic rays, the available evidence suggests no change in sign of the latitudinal gradient for relativistic particles.

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