Beyond the Electrostatic Approach: Numerical Simulations of Martian Ionospheric Irregularities

Abstract

Numerical simulations play an essential role in the study of ionospheric irregularities. In the past few decades, electrostatic simulations have successfully simulated the nonlinear evolution of terrestrial ionospheric irregularities. However, the Mars Atmosphere and Volatile EvolutioN (MAVEN) observations reveal that the Martian ionospheric irregularities are electromagnetic in nature, in contrast to the electrostatic nature of terrestrial ionosphere. In this study, we develop a non‐electrostatic model to investigate the evolution of Martian ionospheric irregularities under nighttime conditions and predominantly horizontal magnetic fields. Our simulation results indicate that electromagnetic Rayleigh‐Taylor instability (RTI) can induce the formation of Martian ionospheric irregularities. Consistent with MAVEN observations, the simulated Martian ionospheric irregularities exhibit plasma density variations of approximately 10%–70% relative to the background ionospheric density, with maximum magnetic field variations reaching about 2 nT.