The angular distribution of solar wind ∼20-200 keV superhalo electrons at quiet times Available to Purchase

We present a comprehensive study of the angular distribution of ∼20-200 keV superhalo electrons measured at 1 AU by the WIND 3DP instrument during quiet times from 1995 January through 2005 December. According to the interplanetary magnetic field, we re-bin the observed electron pitch angle distributions to obtain the differential flux, J_out (J_in), of electrons traveling outward from (inward toward) the Sun, and define the anisotropy of superhalo electrons as $A=2(Jout−Jin)Jout+Jin$ at a given energy. We found that for out in ∼96% of the selected quiet-time samples, superhalo electrons have isotropic angular distributions, while for ∼3% (∼1%) of quiet-time samples, superhalo electrons are outward-anisotropic (inward-anisotropic). All three groups of angular distributions show no correlation with the local solar wind plasma, interplanetary magnetic field and turbulence. Furthermore, the superhalo electron spectral index shows no correlation with the spectral index of local solar wind turbulence. These quiet-time superhalo electrons may be accelerated by nonthermal processes related to the solar wind source and strongly scattered/ reflected in the interplanetary medium, or could be formed due to the electron acceleration through the interplanetary medium.