An Akasofu's Epsilon Parameter Corrected By The Solar Wind Dynamic Pressure As A Guide For The Energy Balance Estimate During Geomagnetic Storms

Details An Akasofu's Epsilon Parameter Corrected By The Solar Wind Dynamic Pressure As A Guide For The Energy Balance Estimate During Geomagnetic Storms An Akasofu's Epsilon Parameter Corrected By The Solar Wind Dynamic Pressure As A Guide For The Energy Balance Estimate During Geomagnetic Storms

Dec 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006agufmsm31a0289d&link_type=abstract

American Geophysical Union, Fall Meeting 2006, abstract #SM31A-0289

Physics

2784 Solar Wind/Magnetosphere Interactions, 2788 Magnetic Storms And Substorms (7954), 7954 Magnetic Storms (2788)

Scientific paper

Geomagnetic storms are large disturbances in the Earth's magnetosphere caused by an enhanced solar wind- magnetosphere energy transfer. One of the main manifestations of a geomagnetic storm is the ring current enhancement. It is responsible for the decrease in the geomagnetic field observed at the ground stations. In this work we have studied the ring current dynamics during two different types of magnetic storms. Thirty-three events were selected during the period 1981-2004. Eighteen out of 30 events are very intense (or super- intense) magnetic storms (Dst ≤ -250 nT) and the remaining are intense magnetic storms (-250 < Dst ≤ -100 nT). Interplanetary data from spacecraft in the solar wind near Earth's orbit (ACE, IMP-8, ISEE3), and geomagnetic indices (Dst, AE, Sym, and Kp) were analyzed. Our aim is to consider what are the interplanetary characteristics (interplanetary dawn-dusk electric field, interplanetary magnetic field component B_S), the e parameter, and the total energy input into the magnetosphere (Wɛ), for these two classes of magnetic storms. Two corrections on the e coupling function were used: the first one is an already known correction in the magnetopause radius to take into account the changed solar wind pressure. The second correction is by the first time proposed in this work, and it accounts for the reconnection efficiency. Geomagnetic data/indices were also employed to study the ring current dynamics and to search the differences in the storm evolution during these events. Corrected parameters are shown to be more adequate to explain storm energy balance. Further, the energy during the main phase using corrected can be considered as a threshold value to separate intense from very intense storms.

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