Loss Of Relativistic Electrons In The Inner Magnetosphere Via Wave Particle Interactions

Details Loss Of Relativistic Electrons In The Inner Magnetosphere Via Wave Particle Interactions Loss Of Relativistic Electrons In The Inner Magnetosphere Via Wave Particle Interactions

Dec 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010agufmsm13c..02k&link_type=abstract

American Geophysical Union, Fall Meeting 2010, abstract #SM13C-02

Physics

[2716] Magnetospheric Physics / Energetic Particles: Precipitating, [2730] Magnetospheric Physics / Magnetosphere: Inner, [2774] Magnetospheric Physics / Radiation Belts, [2784] Magnetospheric Physics / Solar Wind/Magnetosphere Interactions

Scientific paper

Relativistic electrons in the magnetosphere are both energized and lost via their interaction with plasma waves such as whistler chorus, plasmaspheric hiss and EMIC waves. These waves are usually localized in different regions of the magnetosphere as well as being located either inside or outside the plasmapause. We examine the systematics of loss time scales of relativistic electrons during geomagnetic storms using data collected by multiple sensors onboard SAMPEX, a low Earth orbiting spacecraft. SAMPEX is in a polar orbit with an orbital period of about 90 minutes and covers all L shells. The sensors on board SAMPEX provide measurements of electrons of energies > 0.6 MeV, > 1 MeV, > 3 MeV, 2-6 MeV, 3-16 MeV and have been collecting data since SAMPEX was launched in 1992. We will compare the low altitude results to those obtained by sensors onboard the HEO spacecraft. The HEO spacecraft are in a Molniya type orbit and we will use measurements made at high altitudes which sample a larger portion of the pitch angle distribution. We will examine the dependence of energization and loss time scales of relativistic electrons over a time period ranging from 1994 to 2005 to investigate the systematics of electron loss as a function of energy and L shell. In particular, we will focus on the relationship between plasmapause location and flux decay time scales. We will also examine the dependence of loss time scales as a function of geomagnetic activity and interplanetary drivers.

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