Multisatellite observations of the outer zone electron variation during the November 3–4, 1993, magnetic storm

TitleMultisatellite observations of the outer zone electron variation during the November 3–4, 1993, magnetic storm
Publication TypeJournal Article
Year of Publication1997
AuthorsLi, X, Baker, DN, Temerin, M, Cayton, TE, Reeves, EGD, Christensen, RA, Blake, JB, Looper, MD, Nakamura, R, Kanekal, SG
JournalJournal of Geophysical Research
Volume102
IssueA7
Pagination14123 - 14140
Date Published01/1997
ISSN0148-0227
KeywordsMagnetopause Losses
AbstractThe disappearance and reappearance of outer zone energetic electrons during the November 3–4, 1993, magnetic storm is examined utilizing data from the Solar, Anomalous, and Magnetospheric Particle Explorer (SAMPEX), the Global Positioning System (GPS) series, and the Los Alamos National Laboratory (LANL) sensors onboard geosynchronous satellites. The relativistic electron flux drops during the main phase of the magnetic storm in association with the large negative interplanetary Bz and rapid solar wind pressure increase late on November 3. Outer zone electrons with E > 3 MeV measured by SAMPEX disappear for over 12 hours at the beginning of November 4. This represents a 3 orders of magnitude decrease down to the cosmic ray background of the detector. GPS and LANL sensors show similar effects, confirming that the flux drop of the energetic electrons occurs near the magnetic equator and at all pitch angles. Enhanced electron precipitation was measured by SAMPEX at L ≥ 3.5. The outer zone electron fluxes then recover and exceed prestorm levels within one day of the storm onset and the inner boundary of the outer zone moves inward to smaller L (<3). These multiple-satellite measurements provide a data set which is examined in detail and used to determine the mechanisms contributing to the loss and recovery of the outer zone electron flux. The loss of the inner part of the outer zone electrons is partly due to the adiabatic effects associated with the decrease of Dst, while the loss of most of the outer part (those electrons initially at L ≥ 4.0) are due to either precipitation into the atmosphere or drift to the magnetopause because of the strong compression of the magnetosphere by the solar wind. The recovery of the energetic electron flux is due to the adiabatic effects associated with the increase in Dst, and at lower energies (<0.5 MeV) due to rapid radial diffusion driven by the strong magnetic activity during the recovery phase of the storm. Heating of the electrons by waves may contribute to the energization of the more energetic part (>1.0 MeV) of the outer zone electrons.
URLhttp://onlinelibrary.wiley.com/doi/10.1029/97JA01101/abstract
DOI10.1029/97JA01101


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