Fig. 3: Spectral distributions of Whistler-mode waves and their quantitative scattering impact on Jovian radiation belt energetic electrons.
a, b the time-averaged wave intensities as functions of wave frequency and M-shell (the distance from the magnetic equator to Jupiter’s center, normalized by Jupiter’s radius) for |MLAT| < 20° (MLAT is the magnetic latitude) and |MLAT| = 20–60°. From top to the bottom, the solid line and two dashed lines represent fceq (equatorial electron gyrofrequency), 0.5fceq, and 0.05fceq based on the dipole magnetic field model. c the average wave intensity at M-shell = 9.5 for |MLAT| < 20° and |MLAT| = 20–60°. The shaded region indicates the frequency range of LFWs (low frequency whistler-mode waves), while the unshaded part corresponds to HFWs (high frequency whistler-mode waves). d, e the bounce-averaged pitch angle diffusion coefficient <Dαα> induced by LFWs and HFWs as functions of energy and equatorial pitch angles. f the combined <Dαα> from LFWs and HFWs. g–i Comparison of simulated electron pitch angle distributions (solid lines) with observations (dotted lines) for three energy channels (55, 97, 170 keV) at three simulation intervals (0, 5, and 10 h). The observed PSDs (phase space densities) are from the time interval between UT = 8:00 and UT = 8:30 (UT means universal time) in Fig. 1, excluding the interval of electron injections. Source data are provided as a Source Data file.
