Physics – Geophysics
Scientific paper
Apr 1994
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994jgr....99.5793p&link_type=abstract
Journal of Geophysical Research (ISSN 0148-0227), vol. 99, no. A4, p. 5793-5803
Physics
Geophysics
49
Current Sheets, Geomagnetic Tail, Magnetic Field Configurations, Magnetic Fields, Magnetic Storms, Geophysics, Ionospheric Electron Density, Mathematical Models, Solar Terrestrial Interactions
Scientific paper
The global magnetic field configuration during the growth phase of the Coordinated Data Analysis Workshop (CDAW) 6 substorm (March 22, 1979, 1054 UT) is modeled using data from two suitably located spacecraft and temporally evolving variations of the Tsyganenko magnetic field model. These results are compared with a local calculation of the current sheet location and thickness carried out by McPherron et al. (1987) and Sanny et al. (this issue). Both models suggest that during the growth phase the current sheet rotated away from its nominal location, and simultaneously thinned strongly. The locations and thickness obtained from the two models are in good agreement. The global model suggests that the peak current density is approximately 120 nA/sq m and that the cross-tail current almost doubled its intensity during this very strong growth phase. The global model predicts a field configuration that is sufficiently stretched to scatter thermal electrons, which may be conducive to the onset of ion tearing in the tail. The electron plasma data further support this scenario, as the anisotropy present in the low-energy electrons disappears close to the substorm onset. The electron contribution to the intensifying current in this case is of the order of 10% before the isotropization of the distribution.
Baker Daniel N.
Frank Louis A.
Huang Chang-Yin
McPherron Robert L.
Mitchell Donald G.
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