Energy transfer from the solar wind to the magnetosheath and into the magnetosphere

Details Energy transfer from the solar wind to the magnetosheath and into the magnetosphere Energy transfer from the solar wind to the magnetosheath and into the magnetosphere

May 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001agusm..sm41a03p&link_type=abstract

American Geophysical Union, Spring Meeting 2001, abstract #SM41A-03

Physics

2736 Magnetosphere/Ionosphere Interactions, 2740 Magnetospheric Configuration And Dynamics, 2784 Solar Wind/Magnetosphere Interactions

Scientific paper

Energy input from the solar wind into the magnetosphere is usually evaluated using coupling functions such as epsilon or VBsouth as measured in the upstream solar wind. Especially, the epsilon parameter was originally scaled such that it gave values comparable to the energy dissipation in the inner magnetosphere and ionosphere. Statistically, the energy input during the expansion phase as evaluated from the epsilon parameter is well-correlated with the energy dissipated in the ionosphere. Here we use Cluster II and ISTP observations to examine events during which measurements were available from the solar wind, from the magnetosheath, and from the magnetosphere. The energy coupling functions are compared with those evaluated in the magnetosheath, to examine the scatter in the energy input-output analysis introduced by the shocked solar wind in the magnetosheath. Furthermore, the results are compared with those predicted by a global MHD simulation, where the magnetosheath and solar wind can be evaluated at any point in space and time. Both storm-time and isolated substorms are examined; we discuss the differences and similarities of energy transfer during stormtime andisolated substorms.

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