Physics
Scientific paper
Mar 2003
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003jastp..65..429f&link_type=abstract
Journal of Atmospheric and Solar-Terrestrial Physics, Volume 65, Issue 4, p. 429-446.
Physics
9
Scientific paper
The most detailed studies of the energetic budget of the magnetosphere during the magnetic storms were done on the basis of the paraboloid model using the November 23-27, 1986 and May 6-8, 1988 magnetic storms. Calculations have shown that the energy injected in the course of the magnetic storms into the inner magnetosphere and ionosphere of both hemispheres amounts to ~0.9-2.2% of the solar wind kinetic energy on the magnetospheric cross section. The total energy injected into the magnetosphere from a distance of 60RE in the tail down to the ionosphere is /~4.0-7.5% of the solar wind kinetic energy during the main phase of the two magnetic storms. The injected energy into the tail ETL is 1.03-1.18 of the total energy input into the inner magnetosphere and ionosphere of both hemispheres at the main phase of the two storms. The decay parameter for the energy stored in the magnetospheric tail is ~5h.
The total energy dissipated in the ionosphere of both hemispheres, in the inner magnetosphere and in the tail during the two storms, is 1.85×1017 and 3.24×1017J, respectively. The total energy input into the magnetosphere is calculated to be 1.77×1017 and 3.16×1017J. The discrepancies of 0.08×1017 and 0.10×1017J amount to 4.3% and 3.1% of the total energy input and characterize the accuracy of the magnetospheric energy budget calculation. In the magnetotail the balance between the injected and dissipated energy of ~1.09×1017J for one storm and ~1.7×1017J for the other is preserved as well. We conclude that one-half of the energy which is injected into the magnetosphere from the solar wind during the storms enters the magnetotail and dissipates there.
The coupling parameter ɛPA is widely considered to be a measure of the energy dissipation in the inner magnetosphere. The dissipation energy in the inner magnetosphere UT=UJ+UA+UDR is defined as the sum of the contributions of the Joule dissipation UJ, the energy of auroral particle precipitation UA, and the energy injection into the ring current UDR. In this paper, we find that ɛPA in the two storms investigated is substantially different from UT. The energy injected into the ring current region at the main phase of the storm amounts to ~1016J. It is nearly 3 or 4 times smaller than the energy input into the magnetosphere via the field-aligned currents or the energy dissipated in the ionosphere by Joule dissipation. The energy injected into the magnetosphere is transferred mainly into processes different from the ring current generation.
During the development of intensive auroral electrojets, the energy dissipation in the magnetotail and the increase in the energy of the tail current system occur simultaneously. The energy dissipation in the inner magnetosphere and ionosphere US occurs not only at the expense of energy previously stored in the magnetotail, but rather at the expense of energy that is injected into the near-Earth tail. This energy transfer from the solar wind into the magnetotail and the energy dissipation in the ionosphere increased simultaneously. Thus, during disturbances in the magnetosphere, simultaneously loading-unloading and directly driven processes occur. Loading- and unloading processes manifest themselves both in the storage of the solar wind energy in the magnetotail and the ring current, and subsequent dissipation. The directly driven processes become manifest in the direct dissipation of the energy which enters into the ionosphere through large-scale field-aligned current systems.
Alexeev Igor I.
Dremukhina L. A.
Feldstein Ya. I.
Kalegaev Vladimir V.
Levitin A. E.
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