Response of outer belt electrons and VLF waves to high-speed streams

Details Response of outer belt electrons and VLF waves to high-speed streams Response of outer belt electrons and VLF waves to high-speed streams

Dec 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010agufmsm13a1789m&link_type=abstract

American Geophysical Union, Fall Meeting 2010, abstract #SM13A-1789

Physics

[2772] Magnetospheric Physics / Plasma Waves And Instabilities, [2774] Magnetospheric Physics / Radiation Belts, [2784] Magnetospheric Physics / Solar Wind/Magnetosphere Interactions, [2788] Magnetospheric Physics / Magnetic Storms And Substorms

Scientific paper

Flux enhancements of relativistic electrons in the outer belt tend to occur associated with high-speed streams, and a large flux enhancement is observed during the predominantly southward interplanetary magnetic field (IMF). Our statistical studies revealed that 90%(50%) of the fast coronal hole streams display a large flux enhancement at GEO when the southward (northward) IMF is dominant. From the standpoint of the internal acceleration by whistler mode chorus waves, this IMF dependence can be understood as follows. The internal acceleration by wave-particle interactions is especially effective when a continuous source of hot electrons can be maintained to produce chorus waves for the several day periods. Continuous hot electron injections are enhanced during a prolonged period of intense convection and/or substorms, which are driven by the southward IMF in high-speed streams. Here we statistically investigate the VLF wave data of Akebono satellite to test the model for the flux enhancement of the outer belt by VLF waves associated with high-speed streams. We show clear differences of hot electrons, whistler mode chorus waves, and convection/substorms between the southward and northward dominant IMF in high-speed streams, which is consistent with the internal acceleration process.

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