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Multiple discrete-energy ion features in the inner magnetosphere: 9 February 1998, event

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Figure

Fig. 1. From top to bottom, energy vs. L spectra of pitch-angle averaged proton differential flux measured by POLAR/CAMMICE/MICS on 9 February 1998 (panels 1 and 2), energy spectra of locally mirroring proton flux calculated with the Volland-Stern type con
Fig. 2. From top to bottom, the solar wind density (SW N), the solar wind velocity (SW V), the intensity of the IMF (IMF B), the clock angle of IMF and D st on 8–9 February 1998.
Fig. 3. Same as panels 9 and 10 of Fig. 1, except that time is fixed to 11:00 UT on 9 February 1998.
Fig. 4. Possible explanation for the ion gaps observed by Po- Po-lar/MICS on 9 February 1998

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