Abstract Magnetic reconnection occurring between the interplanetary magnetic field (IMF) and the dayside magnetopause causes a circulation of magnetic flux and plasma within the magnetosphere, known as the Dungey cycle. This circulation is transmitted to the ionosphere via field‐aligned currents (FACs). The magnetic flux transport within the Dungey cycle is quantified by the cross‐polar cap potential (CPCP or transpolar voltage). Previous studies have suggested that under strong driving conditions the CPCP can saturate near a value of 250 kV. In this study we investigate whether an analogous saturation occurs in the magnitudes of the FACs, using observations from the Active Magnetosphere and Planetary Electrodynamics Response Experiment. The solar wind speed, density and pressure, theBzcomponent of the IMF, and combinations of these, were compared to the concurrent integrated current magnitude, across each hemisphere. We find that FAC magnitudes are controlled most strongly by solar wind speed and the orientation and strength of the IMF. FAC magnitude increases monotonically with solar wind driving but there is a distinct knee in the variation around IMFBz = −10 nT, above which the increase slows.
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Magnetosheath Control of the Cross Polar Cap Potential: Correcting for Measurement Uncertainty in Space Weather
Abstract This study quantifies the variation and apparent saturation of the cross polar cap potential with respect to the motional electric field in the solar wind and magnetosheath. The electric potential across the polar cap is often observed to respond linearly to solar wind driving during weak driving and nonlinearly during strong driving, with eventually responding less and less to increased driving. This effect is called “polar cap potential saturation” and has been observed in many studies that correlate some measure of solar wind driving (typically the motional electric field ) with . In this study, it is shown that measurement error in the solar wind driver creates a nonlinear bias in its variation relative to . This is accomplished by associating a decade of radar measurements of with simultaneous probabilistic predictions of in the solar wind just upstream of the bow shock and in the magnetosheath. After correcting for the bias in the solar wind and magnetosheath caused by measurement uncertainty, the extent of saturation between and the corrected solar wind is reduced. More importantly, saturates with respect to the solar wind but not the magnetosheath . This effect is caused by the magnetosheath being reduced relative to the solar wind when the solar wind Alfvén Mach number is low. Both of these findings support the theory that the saturation is due to the magnetosheath flow being magnetically dominated for large solar wind magnetic field magnitudes.
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- Award ID(s):
- 1934997
- PAR ID:
- 10683418
- Publisher / Repository:
- Journal of Geophysical Research: Space Physics
- Date Published:
- Journal Name:
- Journal of Geophysical Research: Space Physics
- Volume:
- 130
- Issue:
- 3
- ISSN:
- 2169-9380
- Format(s):
- Medium: X
- Sponsoring Org:
- National Science Foundation
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