Statistical Analysis of Locally Generated Magnetosonic Waves in the Martian Magnetosheath and Magnetosphere Using MAVEN Observations

Abstract Magnetosonic (MS) waves, a type of plasma wave with frequencies between the proton gyrofrequency and the lower hybrid frequency, play a critical role in the dynamics of space plasma environments. This study presents a comprehensive statistical analysis of locally generated MS waves in the Martian magnetosheath and magnetosphere, based on nearly nine years of MAVEN observations (October 2014–May 2023). Using wavelet transform and singular value decomposition techniques, we identify MS wave events and investigate their spatial distribution, occurrence rates, and dependence on solar wind and solar EUV conditions. Our results reveal that locally generated MS waves predominantly occur in the nightside magnetic pileup region and magnetotail (with a northern preference), with occurrence rates reaching ∼8%. These waves exhibit dawn‐dusk asymmetry, with higher rates on the dawn side. The occurrence rates increase with altitude, from ∼0% below 200 km to over 5% at 400–500 km. Solar wind dynamic pressure and solar EUV radiation strongly influence the spatial distribution and amplitude of MS waves, with high‐pressure and high‐EUV conditions favoring higher occurrence rates and larger wave amplitudes in the magnetotail. This study highlights the potential role of MS waves in ionospheric particle heating and escape, particularly through resonant interactions with ions. These findings underscore the complexity of MS wave dynamics in the Martian magnetosphere and their sensitivity to solar activity, providing critical insights for future studies of the plasma environment of Mars and its interaction with the solar wind.