Low‐frequency hiss is known to play an important role in the precipitation of radiation belt electrons by cyclotron, Landau, and bounce resonances. To investigate the potential combined scattering effect caused by these resonant processes, we analyze the resonant conditions and develop a full relativistic test particle code to quantify the net pitch angle scattering efficiency. It is indicated that the three resonance processes can coexist to scatter electrons at different energies and pitch angles, with the net pitch angle scattering rates up to ~10−3 s−1 for low‐frequency hiss ~175 pT at L = 4.5. Comparisons with the quasi‐linear theory results demonstrate that the cyclotron resonance is mainly responsible for the pitch angle scattering of electrons < ~ 80°, while both Landau and bounce resonances can affect the scattering of near‐equatorially mirroring electrons and their combined diffusion produces smaller scattering coefficients compared to quasi‐linear theory calculations.

The loss mechanisms of radiation belt dropout during the 12 September 2014 storm were investigated using satellite measurements q During the initial phase of the storm, magnetopause shadowing was the dominant loss mechanism, supported by energyindependent decay and butterfly pitch angle distributions (PADs) q The wave-particle interactions played an important role in >1 MeV electron loss during the main phase of the storm and produced 90-peaked PADs at L < 4

A neural network model is constructed based on Van Allen Probes observations to predict the dynamic plasmapause location. The model parameterized by AE or Kp without inclusion of other parameters shows good accuracy to predict the plasmapause location. Our neural network model is capable of predicting the global plasmapause location with low RMSE.

Plasmaspheric hiss can be regarded as an incoherent, broadband electromagnetic whistler mode emission with frequencies ranging from ∼20 to ∼2 kHz (e.g.,

The major energy source of the Jovian system is derived from its fast rotation, and its major particle source is from volcanic activities from Io (Bolton et al., 2015). In addition to being plasma sources, large moons embedded within the Jovian magnetosphere can act as candidates responsible for losses of magnetospheric energetic particles as well (Paonessa & Cheng, 1985). The net effect of how moons affect radiation intensities in their environment is determined by the balance of loss processes (such as the moon absorption time scale) and sources (such as how fast new particles are provided by radial transport or local acceleration). Therefore, the moon absorption of radially diffusing energetic particles is recognized as an important physical process that needs to be considered when evaluating the particle dynamics in the Jovian magnetosphere (e.g.,

Whistler mode chorus waves are electromagnetic emissions, which are typically observed in the low-density region near the geomagnetic equator outside the plasmapause (e.g., Koons & Roeder, 1990;Tsurutani & Smith, 1974). Characteristically, they occur in two separate frequency bands: the lower band (0.1where 𝐴𝐴 𝐴𝐴𝑐𝑐𝑐𝑐 is the equatorial electron gyrofrequency) and the upper band (0.5 𝐴𝐴 𝐴𝐴𝑐𝑐𝑐𝑐 < f < 𝐴𝐴 𝐴𝐴𝑐𝑐𝑐𝑐 ) (

Whistler-mode chorus waves are one of the most important and common waves in the Earth's magnetosphere with the frequencies generally ranging from 0.1 f ce to 0.8 f ce (f ce is the electron gyro-frequency). By the gap around 0.5 f ce , chorus waves are divided into upper band (0.5 f ce < f < 0.8 f ce ) and lower band (0.1 f ce < f < 0.5 f ce ) (W.

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