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At auroral zone highly irregular magnetic field disturbances are commonly observed.
This may be due to the large and slow magnetic field disturbances at TIX and KTN.
Magnetic field disturbances are analysed for field-aligned currents (FACs) during different IMF conditions.
The intensity of the geomagnetic field disturbances reached maximum values during 9 26 to 10 07 UT.
The beam becomes much more intense in the narrower region associated with the small magnetic field disturbances.
In addition, Gulyaev and Gulyaeva (1992) reported increases in the geomagnetic field disturbances during the full Moon at the solar activity minimum using the auroral electrojet index.
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A distinct pattern of the flow and field disturbance near the plasma boundaries was found.
This phase of field positive disturbance lasted until the Forbush effect maximum depth, then a longer negative phase of field disturbance began.
The field disturbance was observed to propagate faster than the local Alfven speed and was identified as a kinetic Alfvén wave (KAW) disturbance (Duan et al. 2016).
For typical at high latitudes ΣH/ΣP ~ 1.6, and sin I ~ 0.9, the magnetic field disturbance in the ionosphere is b 2 ~ 290 nT.
We next discuss the mechanism by which the dynamo generates the magnetic field disturbance on the ground via the magnetosphere-ionosphere current system.
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