Analytical representation of the plasmasphere electron temperature distribution based on Akebono data

Details Analytical representation of the plasmasphere electron temperature distribution based on Akebono data Analytical representation of the plasmasphere electron temperature distribution based on Akebono data

Dec 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002jgra..107.1459k&link_type=abstract

Journal of Geophysical Research (Space Physics), Volume 107, Issue A12, pp. SMP 24-1, CiteID 1459, DOI 10.1029/2002JA009494

Physics

4

Magnetospheric Physics: Plasmasphere, Ionosphere: Plasma Temperature And Density, Magnetospheric Physics: Magnetosphere-Inner, Ionosphere: Ionospheric Dynamics

Scientific paper

A new approach is used to reveal the average thermal structure of plasmasphere at altitudes between 1000 and 10,000 km. This paper only considers the plasmasphere inside L = 3, and this region of space is sliced at L = 2 to one internal (denoted as equatorial) and one external (denoted as midlatitude) part. Each of these parts is divided into four altitude/local time zones: northern and southern daytime and northern and southern nighttime. Electron temperature (Te) distribution measured along every individual orbit within each zone is approximated by simple expressions that are functions of the geomagnetic latitude or L. The fitting is performed independently to each zone, and two coefficients are extracted from the individual fits: Te value at the equatorward border and the coefficient scaling the latitudinal shape. These coefficients are accumulated in each zone in order to obtain its average Te structure as a function of altitude. The fitting coefficients exhibit large scatter, which reflects the large day-to-day variability of plasmasphere Te. The fitting error is estimated at 6% and 12% for the equatorial and midlatitude zones, respectively. The average fit coefficients are used to check for seasonal variations in each zone and for a possible hemispheric asymmetry. It is determined that the winter sunlit plasmasphere is hotter than the summer one; the case for nighttime is reverse. The day/night amplitude is larger in the winter than in the summer, and the seasonal differences are more pronounced in the Southern Hemisphere. The latitude gradients of Te reveal a hemispheric asymmetry, which is largest during northern daytime winter. Solar activity is found to affect the plasmasphere Te. During the day at 3000 km and L = 2, Te increases by ~2000°K when F10.7 changes from 70 to 300. The nighttime increase is ~1000°K. At the equator, Te shows weaker dependence on solar activity. The average heat flux through 3000 km altitude is estimated at 3.7 × 109 (eV cm-2 s-1) during the day and 1.6 × 108 (eV cm-2 s-1) during the night.

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