Solar Wind Energy Input and the Response of the Magnetotail During Geomagnetically Disturbed Times

Details Solar Wind Energy Input and the Response of the Magnetotail During Geomagnetically Disturbed Times Solar Wind Energy Input and the Response of the Magnetotail During Geomagnetically Disturbed Times

Dec 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009agufmsm31b1539l&link_type=abstract

American Geophysical Union, Fall Meeting 2009, abstract #SM31B-1539

Physics

[2744] Magnetospheric Physics / Magnetotail, [2784] Magnetospheric Physics / Solar Wind/Magnetosphere Interactions, [2788] Magnetospheric Physics / Magnetic Storms And Substorms, [2790] Magnetospheric Physics / Substorms

Scientific paper

The energy input from the solar wind into the magnetosphere and the response of the magnetotail magnetic field and plasma are examined during geomagnetically disturbed days. The solar wind energy input is estimated using Akasofu’s empirical energy coupling parameter, ɛ = VB^2(sin^4(θ/2))L^2, where V and B is the solar wind speed and IMF magnetic field magnitude, respectively, and θ is the polar angle of IMF projected onto the dawn-dusk plane, while L2 is a rough estimation of the area through which the energy flux passes. The magnetotail field and plasma variations are detected by THEMIS spacecraft. It is found that the growth phase signatures in the tail, which include prolonged increase in |Bx| and small Bz component often occurred during periods of enhanced solar wind energy input. Dipolarizations and sudden intensification of magnetic field disturbances following the growth phase, which are associated with substorm auroral onsets observed on the ground, are often observed when or after the reduction of the ɛ parameter. The observations suggest that the release of the solar wind energy in the tail is associated with the decrease of the solar wind energy and momentum input to the magnetosphere.

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