A Statistical Investigation of Factors Influencing the Magnetotail Twist at Mars

The Martian magnetotail exhibits a highly twisted configuration, shifting in response to changes in polarity of the interplanetary magnetic field's (IMF) dawn‐dusk (B (Y)) component. Here, we analyze ∼6000 MAVEN orbits to quantify the degree of magnetotail twisting (θ (Twist)) and assess variations as a function of (a) strong planetary crustal field location, (b) Mars season, and (c) downtail distance. The results demonstrate that θ (Twist) is larger for a duskward (+B (Y)) IMF orientation a majority of the time. This preference is likely due to the local orientation of crustal magnetic fields across the surface of Mars, where a +B (Y) IMF orientation presents ideal conditions for magnetic reconnection to occur. Additionally, we observe an increase in θ (Twist) with downtail distance, similar to Earth's magnetotail. These findings suggest that coupling between the IMF and moderate‐to‐weak crustal field regions may play a major role in determining the magnetospheric structure at Mars.