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Dynamics of the plasmasphere and the outer radiation belt

During geomagnetic disturbances, the plasmapause and the outer radiation belt exhibit very dynamic behavior in terms of radial location and particle populations. These behaviors have been shown to be correlated as a result of wave-particle interactions contributing to outer radiation belt particle energization and loss. Efforts to model this relationship have been hampered by the limited temporal coverage of available plasmapause observations. We identify the signature of the plasmapause in the ionosphere, i.e. the light ion trough, from DMSP RPA observations, then map these locations along magnetic field lines to the equatorial plasmapause. This can offer over 10 years of plasmapause observations from multiple DMSP satellites. Our identifications compare well with those from IMAGE EUV observations. DMSP light ion measurements often show indications of plasmaspheric structure, e.g. notches and plumes, with such structure tending to account for differences between DMSP and IMAGE identifications. The DMSP-derived plasmapause is found to correlate with outer radiation belt dynamics, including locations of SAMPEX-observed precipitating particle microbursts. Plasmapause-ionosphere interactions Fig. 1. Schematic of proposed mechanisms for outer radiation belt energization and loss associated with the plasmasphere. [From Reeves, 2007, after Summers et al., 1998.] Conclusions and future work • Our method of identifying the plasmapause using DMSP data compares well to IMAGE plasmapause observations; review of DMSP-IMAGE mismatch cases reveals that DMSP often observes plasmaspheric structure (e.g. notches, plumes) that account for mismatches. • Comparison of locations for DMSP-identified plasmapause and SAMPEX-observed microbursts shows microbursts are consistently outside the plasmasphere, with correlations between locations of innermost microbursts and outermost plasmapause detections. • During plasmasphere erosion, microburst locations move into emptied regions on short timescales; data suggests microbursts follow last plasmasphere detection by as little as ~3 hours. This method is being applied to ~10 years of DMSP data, potentially providing ~100,000 plasmapause detections spanning a full solar cycle. Combined with SAMPEX data, the resulting database will be used to examine the relationship of the plasmasphere and radiation belt energization and loss.