Energetic Electron Scattering due to Whistler Mode Chorus Waves Using Realistic Magnetic Field and Density Models in Jupiter's Magnetosphere.

We evaluate energetic electron scattering in pitch angle and energy using realistic magnetic field and density models due to whistler mode chorus waves in Jupiter's magnetosphere and study their dependences on various wave and background parameters. We calculate the bounce‐averaged diffusion coefficients by considering the latitudinal variation of total electron density and ambient magnetic field intensity, using the VIP4 internal magnetic field and CAN current sheet model. The electron phase space density evolution due to chorus waves is simulated at M shell of 10, using the central wave frequency at 0.1fce and wave amplitude of 30 pT. Under the typical values of the ratio between the plasma frequency and electron cyclotron frequency, chorus waves could cause fast pitch angle scattering loss of energetic electrons from tens to several hundred keV in several hours, and gradual acceleration of relativistic electrons at several MeV in several days. The electron pitch angle scattering at ~500 keV and the acceleration at several MeV are both enhanced using the latitudinally varying density and VIP4 + CAN magnetic field model compared to the electron evolution using the constant density and dipole magnetic field model. Our sensitivity study indicates that the electron scattering at higher energy is caused by waves at lower frequencies or in a lower‐density background plasma, and the scattering is faster for waves at smaller wave normal angles. The electron diffusion is mainly caused by waves at lower latitudes, but the waves at higher latitudes (>30°) contribute to the electron loss at higher energies (>2 MeV). Plain Language Summary: Whistler mode chorus waves are capable of causing the flux decay of energetic electrons and acceleration of relativistic electrons in Jupiter's magnetosphere. We evaluate the efficiency of the electron flux decay and acceleration due to chorus waves using more realistic magnetic field and total electron density profiles. The decay of energetic electrons and the acceleration of relativistic electrons are both more significant in our simulation than the results using the constant density and dipolar magnetic field model. The chorus waves at higher wave frequency or in a lower density condition can cause the electron flux acceleration at higher energies, and the waves at lower frequency or in a lower density condition can cause the flux decay at higher energies. The waves propagating closer to the magnetic field line lead to the more efficient electron precipitation than the waves propagating at larger angles with respect to the field line. Although most of the electron flux decay and precipitation into Jupiter's atmosphere is caused by the waves at low latitudes, the waves at higher latitudes can affect the electrons at higher energies than the waves at lower latitudes. Key Points: We calculate the bounce‐averaged diffusion coefficients using realistic magnetic field and density modelsThe scattering at 100 s keV and acceleration at several MeV are enhanced using a realistic magnetic field and density modelsChorus waves at high latitudes can cause relativistic electron precipitation, which can potentially be confirmed by Juno observations [ABSTRACT FROM AUTHOR]