Spatial structure of the electron flux in an energy range of several MeV and its variations in the outer radiation belt

Abstract

The results from analyzing high energy (4–6 MeV) electron flux variations in the region of the outer radiation belt (L = 3–7) associated with magnetospheric disturbances during active processes on the Sun (flares, coronal mass ejections, and so on) are presented. Data from the low–Earth orbit ARINA experiment on board the Resurs-DK1 satellite (2006–2016) and the VSPLESK experiment on board the International Space Station (2008–2013) are used. The multilayered ARINA and VSPLESK scintillation spectrometers allow us to identify and record electrons in the energy range of 3–30 MeV, and to determine their energies and pitch angles. It is shown that in a period of strong solar magnetospheric disturbances, the high energy electron flux can vary strongly in the outer radiation belt, growing or falling to background values typical of the electron flux of atmospheric albedo. The amplitude and time evolution of such electron flux variations depends largely on the L shell.