
Contents
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8.1 Introductory Remarks 8.1 Introductory Remarks
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8.2 Bursts of Energetic Electrons and Ions Near the Magnetopause 8.2 Bursts of Energetic Electrons and Ions Near the Magnetopause
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8.3 Flux Transfer Events 8.3 Flux Transfer Events
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1318.4 Locations of Reconnection Events Generating FTEs 1318.4 Locations of Reconnection Events Generating FTEs
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8.5 The FTE Contribution to the Overall Convection Potential 8.5 The FTE Contribution to the Overall Convection Potential
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8.6 Ionospheric Signatures of Impulsive Magnetopause Reconnection 8.6 Ionospheric Signatures of Impulsive Magnetopause Reconnection
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1358.7 Cusp-Region ULF Waves 1358.7 Cusp-Region ULF Waves
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8.8 Alfven Waves at the Equatorward Boundary of the Active Cusp 8.8 Alfven Waves at the Equatorward Boundary of the Active Cusp
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8.9 Ion Energy-Latitude Dispersion on Polar Cusp Field Lines 8.9 Ion Energy-Latitude Dispersion on Polar Cusp Field Lines
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8.10 Bursty Ionospheric Flow Events 8.10 Bursty Ionospheric Flow Events
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8.11 Transient Dayside Aurora 8.11 Transient Dayside Aurora
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8.12 F-Region Density Patches 8.12 F-Region Density Patches
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8.13 Summary 8.13 Summary
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1278 Bursty Magnetopause Reconnection and its Consequences
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Published:April 1996
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Abstract
There is at least one way in which the reconnection model of substorms is unrealistic. Rarely if ever will the interplanetary field rotate southward, stay southward, and remain constant. Even on those infrequent occasions when it does do so, steady reconnection may not be established on the dayside: We will see that dayside reconnection proceeds in bursts even then. How likely is it then that steady convection will be established on the nightside? In the next two chapters, we will fit together observations of bursty convection at the magnetopause, in the polar cap and auroral ionosphere, at various distances downtail in the plasma sheet, and beyond the average position of the neutral line in the deep tail. In this chapter, we deal with unsteady magnetopause reconnection. We start with one simple observation: The magnetopause is a source of escaping particles with energies higher than can be generated by the average convection potential across the ionosphere (Section 8.2). This, together with the fact that high-speed magnetopause flows can turn on and off between successive magnetopause crossings only minutes apart, suggests that the rate of reconnection is high for short periods of time and low for longer intervals. When the reconnection events are shorter than or comparable to MHD wave propagation times to the ionosphere, we call the reconnection “bursty.” We then let observation define the properties of bursty magnetopause reconnection. First, we discuss “flux transfer events” (FTEs), the traveling magnetic perturbations near the magnetopause (Section 8.3) that are signatures of bursty reconnection elsewhere on the magnetopause (Section 8.4). The magnitudes of the fluxes reconnected in FTEs are estimated in Section 8.5. Next, we discuss some of the ionospheric signatures of flux transfer events that might be expected on general theoretical grounds (Section 8.6). Variable dayside reconnection could be responsible for ULF magnetic activity in the polar cusp region (Section 8.7). We expect sudden magnetopause reconnection events to send Alfven waves (Section 8.8) and velocity-dispersed ions along field lines towards the polar cusp ionosphere (Section 8.9).
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