Rapid enhancements of relativistic electrons deep in the magnetosphere during the May 15, 1997, magnetic storm

Variations in 0.2-3.2 MeV electron flux in the magnetosphere during the May 15, 1997, magnetic storm (the largest magnetic storm of 1997) arc examined . After over an order of magnitude initial decrease of the 0.2-3.2 MeV elec tron fluxes, the 0.2-0.8 MeV electron flux at L < 4.5 increased and surpass ed the prestorm level in an hour. This increase was followed by increases o f the more energetic 0.8-3.2 MeV electron fluxes. These energetic electron variations are examined utilizing data from the Solar, Anomalous, and Magne tospheric Particle Explorer (SAMPEX), the Global Positioning System (GPS) s eries of satellites, and the Los Alamos National Laboratory (LANL) sensors on board geosynchronous satellites. During the main phase of the storm, flu xes of >0.4-MeV electrons from SAMPEX decreased at L > 4.5 following the D- st drop but increased somewhat at L < 4. GPS satellite data also show that the electron flux decreased in the energy range 0.2-3.2 MeV for all L value s above the minimum detectable L value of similar to 4.2 simultaneously wit h the decrease in D-st, which is consistent with an adiabatic process. Howe ver, the recovery of the electron flux was different at different energies, with an earlier recovery of the less energetic electrons and a later recov ery of the more energetic electrons. The recovery of the electron fluxes st arted before the recovery of D-st, indicating that nonadiabatic processes w ere involved. The 0.2- to 0.8-MeV electrons appeared in the low-L region (4 .2-4.5) at about the same time that the GOES 9 spacecraft measured a strong dipolarization of the Earth's stretched magnetic field. Outer zone electro n fluxes continued to increase across a wide L range (L = 3-8) though the e lectron flux exhibited a strong spatial gradient, with the peak flux below L = 4.2 in the equatorial plane. These data are used to test the idea if ra dial transport from larger L can account for all of the increase in the flu x in the heart of the outer zone electron radiation belt at L = 4-5. Howeve r, the radial gradient of the phase space density for a given first adiabat ic invariant was estimated to be: negative as a function of radial distance during the time that the electron flux was increasing. This estimate is so mewhat uncertain because of rapid temporal variations and sparse data. Howe ver, if this estimate is correct, the usual theory of radial transport from larger radial distances cannot account fur all of the increase in the elec tron flux. The analysis thus suggests that another process, such as local h eating, which does not conserve mu, may be required to explain the subseque nt enhancement of the more energetic (0.8- to 3.2-MeV) electrons but that a dditional data are required to answer this question definitely.