HR: 10:50h
AN: SM42A-03    [Abstracts]
TI: The Spatial Variation of Polar Rain Electrons and its Cause
AU: * Fairfield, D H
EM: Donald.H.Fairfield@nasa.gov
AF: NASA Goddard Space Flight Center, Code 674, Greenbelt, MD 20771, United States
AU: Wing, S
AF: Johns Hopkins University, Applied Physics Laboratory, Laurel, MD 20723, United States
AU: Ruohoniemi, J M
AF: Johns Hopkins University, Applied Physics Laboratory, Laurel, MD 20723, United States
AU: Newell, P T
AF: Johns Hopkins University, Applied Physics Laboratory, Laurel, MD 20723, United States
AU: Gosling, J T
AF: University of Colorado, Laboratory for Atmospheric and Space Physics, Boulder, CO 80303, United States
AU: Skoug, R M
AF: Los Alamos National Laboratory, Los Alamos National Laboratory, Los Alamos, NM 87545, United States
AB: It is generally accepted that field aligned electrons in the solar wind can follow field lines connected to Earth and precipitate in the polar ionosphere where they are known as polar rain. Few-hundred eV, field-aligned electrons of the solar wind "strahl" carry the interplanetary heat flux moving out from the sun and these electrons precipitate in either the northern or southern hemisphere depending on the magnetic field direction. These electrons produce enhanced polar rain in one hemisphere or the other although weaker polar rain is usually produced in the opposite hemisphere by whatever electrons are moving in the opposite direction. Although much evidence exists for this simple free entry mechanism, it has also long been known that there are spatial variations in the energies and intensities of the precipitating electrons. The present work compares electron distribution functions measured by the ACE spacecraft in the solar wind with those measured by the DMSP spacecraft at 800 km altitude over the polar cap. It is found that shifting the DMSP distribution functions in energy by amounts ranging from 10's to a few hundred eV produces quite good agreement with simultaneous ACE measurements. Over most of the polar cap this DMSP energy shift must be positive to achieve this agreement, suggesting the electrons have been decelerated by a field aligned potential as they move from the solar wind to low altitudes. The largest shifts occur on the nightside and on the dawn or dusk side, with the latter depending on the plasma convection pattern which is controlled by the orientation of the IMF. Nearer the cusp the shift is smaller or even negative. Since more massive tailward flowing magnetosheath ions are unable to follow the field lines into the magnetotail like the electrons, a field aligned potential is expected to develop to exclude low energy electrons and prevent an excessive charge imbalance. Such a potential would also produce the deceleration of those electrons that reach low altitudes. This improved understanding of polar rain should increase the utility of polar rain measurements as a diagnostic of the magnetosphere magnetic field configuration.
DE: 2455 Particle precipitation
DE: 2744 Magnetotail
DE: 2760 Plasma convection (2463)
DE: 2776 Polar cap phenomena
DE: 2784 Solar wind/magnetosphere interactions
SC: SPA-Magnetospheric Physics [SM]
MN: 2007 Fall Meeting