Energetic Electron Flux Predictions in the Near-Earth Plasma Sheet From Solar Wind Driving

Suprathermal electrons in the near-Earth plasma sheet are important for inner magnetosphere considerations. They are the source population for outer radiation belt electrons and they pose risks to geosynchronous satellites through their contribution to surface charging. We use empirical modeling to address relationships between solar driving parameters and plasma sheet electron flux. Using Time History of Events and Macroscale Interactions during Substorms, OMNI, and Flare Irradiance Spectral Model Version 2 data, we develop a neural network model to predict differential electron flux from 0.08 to 93 keV in the plasma sheet, at distances from 6 to 12 R-E. Driving parameters include solar wind (SW) density and speed, interplanetary magnetic field (IMF) B-Z and B-Y, solar extreme ultraviolet flux, IMF B-Z ultra-low frequency (ULF) wave power, SW-magnetosphere coupling functions P-alpha 1 and NXCF, and the 4-hr time history of these parameters. Our model predicts overall plasma sheet electron flux variations with correlation coefficients of between 0.59 and 0.77, and median symmetric accuracy in the 41%-140% range (depending on energy). We find that short time-scale electron flux variations are not reproduced using short time-scale inputs. Using a recently published technique to extract information from neural networks, we determine the most important drivers impacting model prediction are V-SW, VBS, and IMF B-Z. SW-magnetosphere coupling functions that include IMF clock angle, IMF B-Z ULF wave power, and IMF B-Y have little impact in our model of electron flux in the near-Earth plasma sheet. The new model, built directly on differential flux, outperforms an existing model that derives fluxes from plasma moments, with the performance improvement increasing with increasing energy.