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Dayside merging between the interplanetary and terrestrial magnetic fields  couples the\udsolar wind electric field to the Earth's magnetosphere, increases the magnetospheric\udconvection  and results in efficient transport of solar wind energy into the magnetosphere.\udSubsequent reconnection of the lobe magnetic field in the magnetotail transports energy into\udthe closed magnetic field region.   Combining global imaging and ground-based radar\udmeasurements, we estimate the reconnection rate in the magnetotail during two days of an\udEISCAT campaign in November-December 2000.  Global images from the IMAGE FUV system guide us\udto identify ionospheric  signatures of the open-closed field line boundary observed by the\udtwo EISCAT radars in Troms&#248; (VHF) and  on Svalbard (ESR).   Continuous radar and optical\udmonitoring of the open-closed field line  boundary is used to determine the location,\udorientation and velocity of the open-closed  boundary and the ion flow velocity\udperpendicular to this boundary. The magnetotail reconnection electric field is found to be a\udbursty process that oscillates between 0mV/m  and 1mV/m with ~10-15min periods.\udThese ULF oscillations are mainly due to the motion of the open-closed boundary. In situ\udmeasurements earthward of the reconnection site in the magnetotail by Geotail show similar\udoscillations in the duskward electric field.  We also find that bursts of increased\udmagnetotail reconnection do not necessarily have any associated auroral signatures. Finally,\udwe find that the reconnection rate  correlates poorly with the solar wind electric field.\udThis indicates that the magnetotail reconnection is not directly driven, but is an internal\udmagnetospheric process.  Estimates of a coupling efficiency between the solar wind electric\udfield and magnetotail reconnection  only seem to be relevant as averages over long time\udintervals. The oscillation mode at 1mHz corresponds to the internal cavity mode with\udadditional lower frequencies, 0.5 and 0.8mHz, that might be modulated by solar wind\udpressure variations

Estimates of magnetotail reconnection rate based on IMAGE FUV and EISCAT measurements