Abstract
Predicting of the location of the maximum in high-energy electron fluxes filling a new radiation belt is an endeavor being carried out by physicists studying the magnetosphere. We analyzed the data from the Defense Meteorological Satellite Program (DMSP) satellites and ground-based magnetometers obtained during geomagnetic storm on 8–9 October 2012. The minimum value of the disturbance storm time (Dst) was −111 nT, and the maximum in high-energy electron fluxes that appeared during the recovery phase was observed at L = 4 Re. At the same time, we analyzed the motion of the auroral oval toward lower latitudes and related substorm activity using the data of the low-orbiting DMSP satellites and the IMAGE magnetic meridian network. It was found from the DMSP satellites’ measurements that the maximum of the energy density of precipitating ions, the maximum of the plasma pressure, and the most equatorial part of the westward auroral electrojet are all located at the 60° geomagnetic latitude. This value corresponds to L = 4 Re, i.e., it coincides with the location of the maximum in high-energy electron fluxes. This L-value also agrees with the predictions of the Tverskaya relation between the minimum in Dst variation and the location of the maximum of the energetic electron fluxes, filling a new radiation belt. The obtained results show that the location of this maximum could be predicted solely from the data of the auroral particle precipitations and/or ground-based magnetic observations.
Highlights
Large fluxes of relativistic electrons in the magnetosphere of the Earth fill the outer radiation belt (ORB)
We analyze the position of the auroral oval and the westward auroral electrojet for the 8–9 October 2012 magnetic storm, using the data of the Defense Meteorological Satellite Program (DMSP) satellites and the International Monitor Geomagnetic Effects (IMAGE) magnetometer network, and show that the analysis of such observations can be very important with regard to solving of the problem of the acceleration of electrons in the ORB
A relation between the minimum value of the disturbance storm time (Dst) variation, maximum of partial ion pressure, and the location of the peak intensity of the relativistic electron fluxes Analysis of the data of high apogee satellites during storms of different intensity showed that the location of the peak intensity of the relativistic electron fluxes appearing during the storm recovery phase (Lmax where Lmax is the McIlwain parameter) depends on the amplitude of the Dst variation (∣Dst∣max) according to the Tverskaya relation (Tverskaya 1986; Tverskaya et al 2005): ∣Dst∣max = c(Lmax)−4 where c is the coefficient of proportionality c = 2.75 ⋅ 104
Summary
Large fluxes of relativistic electrons in the magnetosphere of the Earth fill the outer radiation belt (ORB). Reeves et al (2003) showed that geomagnetic storms can either increase or decrease the fluxes of relativistic electrons in the radiation belt.
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