Other
Scientific paper
May 2002
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002agusmgp42a..04a&link_type=abstract
American Geophysical Union, Spring Meeting 2002, abstract #GP42A-04
Other
5440 Magnetic Fields And Magnetism, 5443 Magnetospheres (2756), 1517 Magnetic Anomaly Modeling, 1521 Paleointensity, 1545 Spatial Variations (All Harmonics And Anomalies)
Scientific paper
This paper presents the lateral variations in the remnant magnetization of the Martian crust determined using a 50-degree spherical harmonic model of the magnetic potential. The inversion of the magnetic potential to the crustal magnetization is non-unique, arising from two distinctly different sources, the direction and the intensity of the magnetization. For the terrestrial crust, the direction of magnetization is usually assigned, either by assuming induced magnetization in which case the magnetization is in the direction of the present core field, or by rock magnetic measurements that directly provide the direction of the magnetization. The direction of magnetization of the Martian crust is estimated from the paleomagnetic pole positions that are calculated through modeling 10 isolate and small size magnetic anomalies. The model potential is then inverted to determine the vertically averaged magnetization of a nominal 50 km thick crust. Because the major magnetic anomalies of Mars are located in the equatorial zone of the paleomagnetic pole, the resulting crustal magnetization is mainly horizontal. The crust is strongly magnetic, with a magnetization of up to ~20 A/m, which is similar to the magnetization of fresh extrusive basalt at the oceanic ridges of the Earth. The lack of distinct magnetic signatures of the giant impact basins, Hellas, Argyre and Isidis, and the absence of a magnetic anomaly associated with the north-south topographic dichotomy indicate that the upper parts of the crust is low magnetic, and that the pronounced magnetic source bodies are in the lower crust. The other source of non-uniqueness is the conventional one that is associated with the intensity of the magnetization and it arises because of the fundamental non-uniqueness of the integral equation that relates the magnetic potential to the magnetization intensity. Although this non-uniqueness cannot be removed, arguments are made that it may have minor effects on the crustal magnetization contrast that gives rise to the pronounced magnetic anomalies of Mars.
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