Ionospheric density depletions around crustal fields at Mars and their connection to ion frictional heating

Mars' ionosphere is formed through ionization of the neutral atmosphere by solar irradiance, charge exchange, and electron impact. Observations by the Mars Atmosphere and Volatile EvolutioN (MAVEN) spacecraft have shown a highly dynamic ionospheric layer at Mars impacted by loss processes including ion escape, transport, and electron recombination. The crustal fields at Mars can also significantly modulate the ionosphere. We use MAVEN data to perform a statistical analysis of density depletions of ionospheric species (Oinline-formula⁺, Oinline-formula $M2inlinescrollmathml{}_{\mathrm{normal\; 2}}^{+}$ 8pt15ptsvg-formulamathimg0e2c4a09676df1e15858f52da73e71b7 angeo-42-69-2024-ie00001.svg8pt15ptangeo-42-69-2024-ie00001.png , and electrons) around crustal fields. Events mostly occur when the crustal magnetic fields are radial, outward, and with a mild preference towards east in the planetocentric coordinates. We show that events near crustal fields are typically accompanied by an increase in suprathermal electrons within the depletion, either throughout the event or as a short-lived electron beam. However, no correlation between the changes in the bulk electron densities and suprathermal electron density variations is observed. Our analysis indicates that the temperature of the major ionospheric species, Oinline-formula $M3inlinescrollmathml{}_{\mathrm{normal\; 2}}^{+}$ 8pt15ptsvg-formulamathimg0e87d75f2896f63c49da39d14255593e angeo-42-69-2024-ie00002.svg8pt15ptangeo-42-69-2024-ie00002.png , increases during most of the density depletion events, which could indicate that some ionospheric density depletions around crustal fields are a result of ion frictional heating.