Functional Description of Magnetospheric Effective Terrestrial Outflows

Details Functional Description of Magnetospheric Effective Terrestrial Outflows Functional Description of Magnetospheric Effective Terrestrial Outflows

May 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001agusm..sm51a08g&link_type=abstract

American Geophysical Union, Spring Meeting 2001, abstract #SM51A-08

Physics

2431 Ionosphere/Magnetosphere Interactions (2736), 2736 Magnetosphere/Ionosphere Interactions

Scientific paper

Applying results from the many published terrestrial outflow studies to the broader problem of globally modeling the flow's impact on magnetosphere dynamics is complicated by several factors. Not all studies apply corrections to derived fluxes for convection drifts or for the effects of spacecraft potential. The distinction between various outflowing ion distribution types is not sharp. And, because outflow acceleration takes place along a distributed altitude range, it is not clear which portions of the reported flows will reach escape velocity and therefore reach the inner boundary of global magnetospheric models. This presentation seeks taddress this issue by providing an empirical model specifically describing the terrestrial outflows capable of populating and influencing the magnetosphere outside of 3 RE altitude. A description is given, both statistical and functional, of the terrestrial ion outflow, for energies below 300 eV, associated with auroral and polar latitude processes. The Polar spacecraft has been immersed within solar cycle 23 for a period of time sufficient to define outflow occurrences for a wide range minimum and maximum conditions. The statistical description of H+ and O+ outflow is determined by binning the parallel ion flux and density in spatial bins of magnetic local time and invariant latitude. Previously published solar maximum data from the Dynamics Explorer RIMS instrument contributes to the species dependent description. The statistical flux and density profiles at any MLT consistently have smoothly varying peaks over auroral and polar latitudes, allowing a functional description to be constructed for a variety of solar input conditions. The functional description for increasing solar wind ram pressure conditions will be shown. Calculated trajectory patterns show that the effective terrestrial contribution to the plasma sheet is both mass- and local-time dependent under stretched and compressed magnetic field configurations.

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