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Determination of the radial profile of phase space density of relativisticelectrons at constant adiabatic invariants is crucial for identifying thesource for them within the outer radiation belt. The commonly used method isto convert flux observed at fixed energy to phase space density at constantfirst, second and third adiabatic invariants, which requires an empiricalglobal magnetic field model and thus might produce some uncertainties in thefinal results. From a different perspective, in this paper we indirectlyinfer the shape of the radial profile of phase space density of relativisticelectrons near the geosynchronous region by statistically examining thegeosynchronous energetic flux response to 128 solar wind dynamic pressureenhancements during the years 2000 to 2003. We thus avoid the disadvantageof using empirical magnetic field models. Our results show that the fluxresponse is species and energy dependent. For protons and low-energyelectrons, the primary response to magnetospheric compression is an increasein flux at geosynchronous orbit. For relativistic electrons, the dominantresponse is a decrease in flux, which implies that the phase space densitydecreases toward increasing radial distance at geosynchronous orbit andleads to a local peak inside of geosynchronous orbit. The flux response ofprotons and non-relativistic electrons could result from a phase densitythat increases toward increasing radial distance, but this cannot bedetermined for sure due to the particle energization associated withpressure enhancements. Our results for relativistic electrons are consistentwith previous results obtained using magnetic field models, thus providingadditional confirmation that these results are correct and indicating thatthey are not the result of errors in their selected magnetic fieldmodel

Features of energetic particle radial profiles inferred from geosynchronous responses to solar wind dynamic pressure enhancements