Abstract
The MHD simulations described here show that the latitude of the high-altitude cusp decreases as the IMF swings from North to South, that there is a pronounced dawn–dusk asymmetry at high-altitude associated with a dawn–dusk component of the IMF, and that at the same time there is also a pronounced dawn–dusk asymmetry at low-altitude. The simulations generate a feature that represents what has been called the cleft. It appears as a tail (when the IMF has a B y component) attached to the cusp, extending either toward the dawn flank or the dusk flank depending on the dawn–dusk orientation of the IMF. This one-sided cleft connects the cusp to the magnetospheric sash. We compare cusp geometry predicted by MHD simulations against published observations based on Hawkeye and DMSP data. Regarding the high-altitude predictions, the comparisons are not definitive, mainly because the observations are incomplete or mutually inconsistent. Regarding the low-altitude prediction of a strong dawn–dusk asymmetry, the observations are unambiguous and are in good qualitative agreement with the prediction.
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Abbreviations
- DMSP:
-
Defense Meteorological Satellite Program
- GSE:
-
Geocentric Solar Ecliptic
- GSM:
-
Geocentric Solar Magnetic
- HEOS:
-
Highly Eccentric Orbiting Satellite
- IMF:
-
Interplanetary Magnetic Field
- IMP:
-
Interplanetary Monitoring Platform
- ISEE:
-
International Sun–Earth Explorers
- MHD:
-
Magnetohydro-dynamic
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Siscoe, G., Crooker, N., Siebert, K. et al. Cusp geometry in MHD simulations. Surv Geophys 26, 387–407 (2005). https://doi.org/10.1007/s10712-005-1902-4
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DOI: https://doi.org/10.1007/s10712-005-1902-4