Solar cycle phase dependence of energetic particle intensity and anisotropy in and around the magnetosphere

Details Solar cycle phase dependence of energetic particle intensity and anisotropy in and around the magnetosphere Solar cycle phase dependence of energetic particle intensity and anisotropy in and around the magnetosphere

Mar 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002esasp.477..413k&link_type=abstract

In: Proceedings of the Second Solar Cycle and Space Weather Euroconference, 24 - 29 September 2001, Vico Equense, Italy. Editor:

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Heliospheric Energetic Particles, Solar Cycle, Intensity Variations, Anisotropy, Magnetospheric Effects, Magnetopause, Bow Shock

Scientific paper

Intensities and anisotropy patterns of protons in local interplanetary space are usually considered to be governed by solar-heliospheric effects for energies above ~250 keV, while magnetospheric influences are taken to be restricted to lower energies, except for particularly active periods. Long-term IMP-8 JHU/APL CPME data for 290 to 500 keV protons are used to show that magnetospheric influences on typical directional distributions are, in fact, more important than expected even far upstream, and their pattern also sensitively depends on the phase of the solar cycle. Yearly median omnidirectional particle fluxes along the IMP-8 orbit, on the other hand, do not depend sensitively on position, while they do show a marked solar cycle dependence. Simplified models of the magnetospheric geometry are invoked in order to classify the intensity and anisotropy data according to their measurement site relative to the magnetosphere. It appears that the effect of the magnetosphere on energetic protons is mostly that of a scattering region changing with solar cycle phase, while particle acceleration is of secondary importance.

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