Energetic Electron Precipitation Driven by Whistler-Mode Waves: A Comparative Study at Earth and Jupiter

Within the magnetospheres of both Earth and Jupiter, a variety of whistler-mode waves are observed, including chorus and hiss waves. At Earth, chorus waves are predominantly found outside the plasmapause, whereas hiss waves are typically confined to the plasmasphere or associated plumes. In contrast, Jupiter's magnetospheric environment is distinctive, as chorus and hiss waves frequently coexist due to the lack of a well-defined plasmapause boundary beyond the Io plasma torus. These waves play crucial roles in influencing energetic electron dynamics at both planets by facilitating the precipitation of energetic electrons into the upper atmosphere and accelerating energetic electrons to relativistic and ultrarelativistic energies.

The impact of chorus and hiss waves on energetic electron precipitation has been extensively quantified at Earth, yet their contributions at Jupiter remain largely unexplored. To address this gap, we perform a comparative analysis of energetic electron precipitation driven by whistler-mode waves at Earth and Jupiter. For Earth, we utilize recently developed empirical models of chorus and hiss waves, informed by data from the Van Allen Probes and THEMIS, covering a broad range of L-shells and Magnetic Local Times (MLTs). At Jupiter, we construct a novel statistical dataset of chorus and hiss wave properties using seven years of observations from Juno. The wave properties derived from these datasets are integrated with updated plasma and magnetic field models to compute pitch angle diffusion coefficients caused by chorus and hiss waves. A quasilinear theory-based physics model is then applied to simulate global electron precipitation driven by these waves at both planets. This comprehensive comparison quantitatively evaluates the roles of chorus and hiss waves in energetic electron precipitation on a global scale at Earth and Jupiter. Our results provide new insights into the dynamic processes governing magnetosphere-atmosphere coupling at these planets, providing broader implications for understanding similar processes at other magnetized planets within the solar system and beyond.