AbstractAn empirical formula relating the strength of a storm given by its |Dst|max with the L-coordinate of the peak of storm-injected relativistic electrons is one of a few well-confirmed quantitative relations found in the magneto-spheric physics. We successively extended a dataset of the formula’s basic storms with several events of high Dst-amplitude up to the highest observed |Dst|max=600 nT. Possible applying of the formula to the predicting of the ring-current plasma-pressure distribution and the lowest westward electrojet position for a storm are discussed. We have also analyzed the 2000–2001 years’ data on relativistic electrons from our instruments installed on EXPRESS-A (geosynchronous orbit; Ee=0.8–6 MeV), Molniya-3 (h=500×40000 km, i=63°; Ee=0.8–5.5 MeV) and GLONASS (h=20000 km, i=64°; Ee∼l MeV) along with other correlated measurements: GOES series (Ee>2 MeV), geomagnetic indices (Dst, AE, AL) and interplanetary parameters (solar wind, IMF). The goal is to investigate which outer conditions are most responsible for the high/low output of the storm-injected relativistic electrons. For the geosynchronous orbit, two factors are found as the necessary condition of the highest electron output: high and long-lasting substorm activity on a storm recovery phase and high velocity of solar wind. On the contrary, extremely low substorm activity surely observed during whole the storm recovery phase constitutes a sufficient condition of the non-increased after-storm electron intensity. For the first time found cases of the increased after-storm electron intensity observed at the inner L-shells with no simultaneously seen increase in the geosynchronous distances are presented.
Storm-time formation of a relativistic electron belt and some relevant phenomena in other magnetospheric plasma domains
Advances in Space Research ; 36 , 12 ; 2392-2400
2003-09-19
9 pages
Article (Journal)
Electronic Resource
English
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