Impact Plasma Amplification of the Ancient Mercury Magnetic Field

Abstract Spacecraft measurements of Mercury indicate that it has a core dynamo with a surface field of 200–800 nT. These data also indicate that the northern hemisphere crust contains remanent magnetization likely produced by an ancient magnetic field. The inferred magnetization intensity is consistent with a wide range of paleofield strengths (0.2–50 μT), possibly indicating that Mercury once had a dynamo field much stronger than today. Recent modeling of ancient impacts on the Moon has demonstrated that plasma generated during basin‐formation can transiently amplify a planetary dynamo field near the surface. Simultaneously, impact‐induced pressure waves can then record these fields as a crustal shock remanent magnetization (SRM). Here, we present impact hydrocode and magnetohydrodynamic simulations of a Caloris‐sized basin (∼1,550 km diameter) formation event. Our results demonstrate that the ancient magnetospheric field (∼0.5–0.9 μT) created by the interaction of the ancient interplanetary magnetic field and Mercury's dynamo field can be amplified by the plasma up to ∼13 μT and, via impact pressure waves, recorded as SRM at the basin antipode. Such magnetization could produce ∼5 nT crustal fields at 20‐km altitude antipodal to Caloris detectable by future spacecraft like BepiColombo. Furthermore, impacts in the southern hemisphere that formed ∼1,000 km diameter basins (e.g., Andal‐Coleridge, Matisse‐Repin, Eitkou‐Milton, and Sadi‐Scopus) could impart crustal magnetization in the northern hemisphere, contributing to the overall remanent field measured by MESSENGER. Overall, the impact plasma amplification process can contribute to crustal magnetization on airless bodies and should be considered when reconstructing dynamo history from crustal anomaly measurements.