Dependence of the Maximum Static Pressure in the Inner Magnetosphere on the Solar Wind Dynamic Pressure and Different Coupling Functions

Details Dependence of the Maximum Static Pressure in the Inner Magnetosphere on the Solar Wind Dynamic Pressure and Different Coupling Functions Dependence of the Maximum Static Pressure in the Inner Magnetosphere on the Solar Wind Dynamic Pressure and Different Coupling Functions

Dec 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009agufmsm11a1539g&link_type=abstract

American Geophysical Union, Fall Meeting 2009, abstract #SM11A-1539

Physics

[2730] Magnetospheric Physics / Magnetosphere: Inner, [2784] Magnetospheric Physics / Solar Wind/Magnetosphere Interactions, [2788] Magnetospheric Physics / Magnetic Storms And Substorms

Scientific paper

Knowledge about distribution of plasma pressure is crucial for the evaluation of the stability of any plasma configuration. Nevertheless, this distribution should be affected by the solar wind-magnetosphere interaction, generally expressed as a series of coupling functions of Dungey, Akasofu, Newell, among others, as well as different characteristics of the solar wind like velocity, interplanetary magnetic field and dynamic pressure. In this study we used the precipitating particles flux data obtained by Aureol-3 satellite to reconstruct the radial plasma pressure profiles in the night-side inner magnetosphere with high space and time resolution. The instantaneous radial profiles of plasma pressure have been obtained using the THEMIS mission satellites. The dynamics of these profiles has been compared with the main parameters of the solar wind, inferred from the NSSDC date base. In particular, it was found that the maximum value of static pressure in the night-side inner magnetosphere correlates with the value of dynamic pressure of the solar wind. The position of the maximum is also affected by the solar wind dynamic pressure, being closer to the Earth in case of high dynamic pressure. The fact that the inner pressure in the magnetosphere and the relation with the dynamic pressure of the solar wind is important for understanding the dynamics of geomagnetic substorms and storms. Finally we compare these results with the analysis of THEMIS data.

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