Statistical Properties of Exohiss Waves and Associated Scattering Losses of Radiation Belt Electrons

Exohiss waves are a type of structureless whistler-mode waves that exist in the low density plasmatrough outside the plasmapause and may potentially perturb the motions of electrons in the radiation belt and ring current. Using data from Van Allen Probe A, we analyze the distribution of magnetic power spectral density (PSD) of exohiss waves in different magnetic local time (MLT) and L-shell regions near the geomagnetic equator. The results reveal that the peak magnetic PSD of exohiss waves is the weakest at MLT = 0-6 and the strongest at MLT = 12-18. The magnetic PSDs of exohiss waves are much lower than those of chorus and hiss waves except for the MLT = 12-18 sector. In addition, we calculated the quasi-linear bounce-averaged pitch angle and momentum diffusion coefficients (< D alpha alpha > and < Dpp >) of electrons caused by exohiss waves. The diffusion coefficients are then compared with those caused by chorus and hiss waves. The peak < D alpha alpha > of electrons driven by exohiss waves becomes stronger as L-shell increases at all MLTs and is the greatest on the dayside, especially in the sector of MLT = 12-18. Exohiss waves have more significant effect on the loss of radiation belt electrons with specific energy levels related to MLT and L-shell region compared to chorus and hiss waves. On the other hand, < Dpp > of electrons caused by exohiss waves is very small, which illustrates that exohiss waves have almost no acceleration effect on electrons. The peak power spectral density of exohiss waves is the weakest at MLT = 0-6 and the strongest at MLT = 12-18 The power spectral density of exohiss waves is much lower than that of chorus and hiss waves except for the MLT = 12-18 sector The effect of exohiss waves on radiation belt electrons with specific energy levels related to MLT and L-shell region cannot be ignored