Non-adiabatic response of relativistic radiation belt electrons to GEM magnetic storms

The importance of fully adiabatic effects in the relativistic radiation bel t electron response to magnetic storms is poorly characterized due to many difficulties in calculating adiabatic flux response. Using the adiabatic fl u?; model of Kim and Chan [1997a] and Los Alamos National Laboratory geosyn chronous satellite data, we examine the relative timing of the adiabatic an d non-adiabatic flux responses. In the three storms identified by the GEM c ommunity for in depth study, the non-adiabatic energization occurs hours ea rlier than the adiabatic re-energization. The adiabatic energization can ac count for only 10-20% of the flux increases in the first recovery stages, a nd only 1% of the Aux increase if there is continuing activity.