Other
Scientific paper
Dec 2006
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006agufmgp11b0076r&link_type=abstract
American Geophysical Union, Fall Meeting 2006, abstract #GP11B-0076
Other
1517 Magnetic Anomalies: Modeling And Interpretation, 1545 Spatial Variations: All Harmonics And Anomalies, 1595 Planetary Magnetism: All Frequencies And Wavelengths, 5440 Magnetic Fields And Magnetism, 6225 Mars
Scientific paper
Martian magnetization vectors and paleopole locations determined by different investigators using different methodologies are contradictory. I suggest that one of the reasons for this is that the anomalies that are assumed to be caused by a homogeneously magnetized source may actually be due to coalescence of multiple crustal sources that may be magnetically coherently or incoherently magnetized and whose coalescence effects at higher observation altitudes lead to derived magnetization directions that are completely different than the ones perceived from lower altitudes. To demonstrate the deleterious effect of the anomaly coalescence, I chose marine magnetic anomalies over a small 4 degree by 4 degree area gridded at 0.1 degree spacing in the NW Atlantic Ocean and computed by inverse techniques magnetization vectors at surface, 10 km, 20 km, and 50 km altitudes. The analysis considered many indicators of the numerical stability in the inversion of magnetization through the equivalent source method, namely the source spacing, the source to observation distance, the mathematical condition number and the rank of the matrix, and also visual characteristics of the observed field and the derived magnetization intensity, inclination, and declination. A comparison of the stable solutions at each altitude shows that the derived solutions are completely different from one another. The lowest altitude Mars magnetic data are at close to 100 km elevation, but has many gaps, and the cleanest and the most complete magnetic data are at close to 400 km elevation. Since it was not even possible to recover similar magnetic directions from the surface and 10 km altitude anomalies, it should be clear that, unless the Martian anomalies are all created by homogeneously magnetized contiguous sources whose geometries are known a priori (as in the well-known seamount magnetization problem), deriving meaningful magnetization directions from the coalesced observed anomalies is impossible. While the prospect of understanding the tectonic framework of Mars through the paleomagnetism of its tectonic terranes is tantalizing, the impossibility obtaining meaningful magnetic directions from coalesced anomalies is reflected in the scattered magnetic pole locations obtained by different researchers using different methods.
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