Outer Belt Variation Along Solar Cycle Inferred From Akebono (EXOS-D) Observations

Details Outer Belt Variation Along Solar Cycle Inferred From Akebono (EXOS-D) Observations Outer Belt Variation Along Solar Cycle Inferred From Akebono (EXOS-D) Observations

Dec 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002agufmsm51a0509o&link_type=abstract

American Geophysical Union, Fall Meeting 2002, abstract #SM51A-0509

Physics

2720 Energetic Particles, Trapped, 2730 Magnetosphere: Inner, 2788 Storms And Substorms

Scientific paper

The most dramatic intervals of particle energization in the vicinity of the Earth occur episodically within the inner magnetosphere during periods of CMEs and high speed solar wind. Since 1989 we have been measuring radiation particle environment by means of Akebono (EXOS-D) satellite and following long-term variations were revealed. (1) Location of the outer radiation belt has a strong dependence on the solar activity, i.e. the outer belt approaches toward the Earth during the solar maximum periods. (2) Correlation between the peak position of the outer radiation belt and the magnitude of Dst index is quite good, i.e. large Dst causes a new outer belt closer to the Earth. (3) Sufficient supply of intermediate-energy electrons is made during and after storm main phase. These seed electrons are accelerated internally up to the high energy range during the storm recovery phase. (4) Increase in the intensity of outer belt electrons strongly depends on the magnetic activity during the storm recovery phase. Sector structure of high speed solar wind as well as CME stricture, i.e N-S type or S-N type with respect to the magnetic field, are key parameters for the large increase of relativistic electrons in the outer radiation belt.

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