Regions of Enhanced Low-Energy Solar Wind Ion Composition Plasma Inside the Dayside Equatorial Magnetopause

Details Regions of Enhanced Low-Energy Solar Wind Ion Composition Plasma Inside the Dayside Equatorial Magnetopause Regions of Enhanced Low-Energy Solar Wind Ion Composition Plasma Inside the Dayside Equatorial Magnetopause

Dec 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001agufmsm41b0795e&link_type=abstract

American Geophysical Union, Fall Meeting 2001, abstract #SM41B-0795

Physics

2728 Magnetosheath, 2731 Magnetosphere: Outer, 2740 Magnetospheric Configuration And Dynamics, 2784 Solar Wind/Magnetosphere Interactions

Scientific paper

Spatial/temporal regions were observed in the dayside magnetosphere with the AMPTE/CCE/CHEM mass spectrometer during which the average fluxes of ~1-5 keV/amu solar wind ions (e.g., H+, He+2, and 0+6) were enhanced over their nominal magnetospheric values by a factor of ~10 at ~1 keV/amu and merged smoothly into the nominal magnetospheric spectral form at energies _ 10 keV/amu. The 1-5 keV/amu average flux levels at these times were lower than those in the magnetospheric boundary layer or the magnetosheath by a factor of _ 20. Fluxes of ionospheric ions (e.g., 0+1 and He+l) were not similarly enhanced. These regions were often broad in spatial/temporal extent, observed throughout CCE's 4 year lifetime (1984-1989) at a wide range of local times, and frequently, but not always, observed in association with CCE's traversal of the boundary layer. In an effort to ascertain unique characteristics related to the entry, transport, and energization history of these ions, we examine the energy spectra, anisotropies, and composition for a few representative intervals, focusing on their relation to global aspects such as current and recent observation location, solar wind parameters, and geomagnetic disturbance indices.

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