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

The importance of fully adiabatic effects in the relativistic radiation belt electron response to magnetic storms is poorly characterized due to many difficulties in calculating adiabatic flux response. Using the adiabatic flux model of Kim and Chan [1997a] and Los Alamos National Laboratory geosynchronous satellite data, we examine the relative timing of the adiabatic and non‐adiabatic flux responses. In the three storms identified by the GEM community for in depth study, the non‐adiabatic energization occurs hours earlier than the adiabatic re‐energization. The adiabatic energization can account for only 10–20% of the flux increases in the first recovery stages, and only 1% of the flux increase if there is continuing activity.