Predicted and observed magnetic signatures of Martian (de)magnetized impact craters

The current morphology of the Martian lithospheric magnetic field results from magnetization and demagnetization processes, both of which shaped the planet. The largest Martian impact craters, Hellas, Argyre, Isidis and Utopia, are not associated with intense magnetic fields at spacecraft altitude. This is usually interpreted as locally nonor de-magnetized areas, as large impactors may have reset the magnetization of the pre-impact material. W e study the effects of impacts on the magnetic field. First, a careful analysis is performed to compute the impact demagnetization effects. W e assume that the pre-impact lithosphere acquired its magnetization while cooling in the presence of a global, centered and mainly dipolar magnetic field, and that the subsequent demagnetization is restricted to the excavation area created by large craters, between 50and 500-km diameter. Depth-to-diameter ratio of the transient craters is set to 0.1, consistent with observed telluric bodies. Associated magnetic field is computed between 100and 500-km altitude. For a single-impact event, the maximum magnetic field anomaly associated with a crater located over the magnetic pole is maximum above the crater. A 200-km diameter crater presents a close-to-1-nT magnetic field anomaly at 400-km altitude, while a 100-km diameter crater has a similar signature at 200-km altitude. Second, we statistically study the 400-km altitude Mars Global Surveyor magnetic measurements modelled locally over the visible impact craters. This approach offers a local estimate of the confidence to which the magnetic field can be computed from real measurements. W e conclude that currently craters down to a diameter of 200 km can be characterized. There is a slight anti correlation of -0.23 between magnetic field intensity and impact crater diameters, although we show that this result may be fortuitous. A complete low-altitude