Dec 2001
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001agufmsm41b0813w&link_type=abstract
American Geophysical Union, Fall Meeting 2001, abstract #SM41B-0813
Physics
2431 Ionosphere/Magnetosphere Interactions (2736), 2447 Modeling And Forecasting, 2455 Particle Precipitation, 2724 Magnetopause, Cusp, And Boundary Layers, 2784 Solar Wind/Magnetosphere Interactions
Scientific paper
When IMF is strongly duskward/dawnward and weakly southward, the open-field line particle precipitation model predicts the occurrence of a double cusp near noon: one cusp at lower latitude and one at higher latitude. The lower latitude cusp ions originate from low-latitude magnetosheath whereas the higher latitude ions originate from the high-latitude magnetosheath. The lower latitude cusp is located in the region of weak azimuthal E x B drift, resulting in a dispersionless cusp, as would be observed from a typical meridional trajectory of a polar orbiting satellite. The higher latitude cusp is located in the region of strong azimuthal and poleward E x B drift. Because of a significant poleward drift, the higher latitude cusp dispersion has some resemblance to that of the typical southward IMF cusp. This prediction was subsequently confirmed in a large case study with DMSP data. Occasionally, the two parts of the double cusp have such narrow latitudinal separation that they give the appearance of just one cusp with extended latitudinal width. From the 40 DMSP passes selected during periods of large (positive or negative) IMF By and small negative IMF Bz, 30 (75%) of the passes exhibit double cusps or cusps with extended latitudinal width. The double cusp result is consistent with the following new statistical results: (1) the cusp latitudinal width increases with |IMF By| and (2) the cusp equatorward boundary moves to lower latitude with increasing |IMF By|.
Newell Patrick
Ruohoniemi Michael J.
Wing Simon
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