Simulating plasmaspheric field-aligned density profiles measured with IMAGE/RPI: Effects of plasmasphere refilling and ion heating

Details Simulating plasmaspheric field-aligned density profiles measured with IMAGE/RPI: Effects of plasmasphere refilling and ion heating Simulating plasmaspheric field-aligned density profiles measured with IMAGE/RPI: Effects of plasmasphere refilling and ion heating

Jan 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003jgra..108.1017t&link_type=abstract

Journal of Geophysical Research (Space Physics), Volume 108, Issue A1, pp. SMP 12-1, CiteID 1017, DOI 10.1029/2002JA009468

Physics

10

Magnetospheric Physics: Plasmasphere, Magnetospheric Physics: Magnetosphere/Ionosphere Interactions, Magnetospheric Physics: Magnetospheric Configuration And Dynamics, Magnetospheric Physics: Numerical Modeling

Scientific paper

The radio plasma imager (RPI) on board the IMAGE satellite measures electron density profiles along magnetic lines through radio sounding techniques. We simulate three density profiles measured by the RPI on 8 June 2001 using the field line interhemispheric plasma (FLIP) model and compare the modeled density profiles with observed profiles. While careful consideration of depletion of flux tubes followed by refilling over several days allows fair agreement between simulated and measured densities around the equator, the simulated densities in the off-equator regions remain significantly lower than those measured for all simulated flux tubes. It is shown that direct heating of ions in the plasmasphere during the plasmasphere refilling, in addition to heating through Coulomb collisions with hotter plasmaspheric electrons, can improve the agreement in the off-equator regions. The enhanced ion pressure in the high altitude part of magnetic field line due to the ion heating impedes the ionospheric inflow from both hemispheres toward the equator, giving rise to decreased transport of ionospheric ions into the equatorial region and thus increased density gradient along the magnetic field line.

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