Inferring the energy density in the tail as a function of the interplanetary conditions during the growth phase of substorms

Details Inferring the energy density in the tail as a function of the interplanetary conditions during the growth phase of substorms Inferring the energy density in the tail as a function of the interplanetary conditions during the growth phase of substorms

Dec 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006agufmsm31a0312j&link_type=abstract

American Geophysical Union, Fall Meeting 2006, abstract #SM31A-0312

Astronomy and Astrophysics

Astrophysics

7500 Solar Physics, Astrophysics, And Astronomy

Scientific paper

The expansion phase corresponds to the dissipative phase of substorm and typically lasts for 30~45 minutes. During the expansion phase, a large amount of energy is explosively dissipated into the inner magnetosphere and the ionosphere. This energy originally coming from the solar wind via its electromagnetic coupling with the magnetosphere is firstly stored in the tail during the growth phase lasting for 1~3 hours.In this paper, we present case studies and preliminary statistical analysis based on the simultaneous measurements obtained both in the solar wind by IMP-8 and in the tail lobes by the pair of the ISEE 1/2 probes. We show that the tail energy density temporal profiles can be reproduced with the help of a model taking into account the pressure balance at the magnetopause and the storage of input energy from the solar wind. We analyse the changes of the values of the model parameters in regards of the interplanetary conditions, the geomagnetic activity and the observation location. We also study the radial gradient of the tail energy density by comparing the results obtained by the model and by the multi-point analysis of the ISEE 1/2 measurements. The implications of these results in substorm and magnetospheric field models are discussed. We finally present the methodology envisioned for extending in a semi-automated way this study to a vast database including the data obtained in the tail by ISEE 1/2, AMPTE-IRM, GEOTAIL, INTERBALL, CLUSTER and the up-coming THEMIS mission and in the solar wind by IMP-8, WIND and ACE.

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