Shock effects on Martian crustal magnetization near large impact basins

Details Shock effects on Martian crustal magnetization near large impact basins Shock effects on Martian crustal magnetization near large impact basins

Dec 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003agufmgp22a..07k&link_type=abstract

American Geophysical Union, Fall Meeting 2003, abstract #GP22A-07

Physics

1517 Magnetic Anomaly Modeling, 1519 Magnetic Mineralogy And Petrology, 1521 Paleointensity, 5420 Impact Phenomena (Includes Cratering), 5440 Magnetic Fields And Magnetism

Scientific paper

The Martian crust has been subject to several very large meteoroid impacts. Shock pressures associated with these impacts may have demagnetized parts of the Martian crust to an extent determined by the shock resistance of the magnetic materials responsible for crustal sources. Impacts that form large basins generate pressures in excess of 1 GPa that extend several crater radii from the point of impact, beneath the surface. Near the surface, however, wave interference significantly reduces the pressure (1 GPa) experienced by crustal materials. Impact demagnetization experiments indicate that pressures of 1 GPa magnitude are sufficient to demagnetize most of the common magnetic minerals (magnetite, pyrrhotite). Titanohematite with ferrian ilmenite exsolution lamellae is the exception. According to our data, this mineral has the highest coercivity (>300 mT) and largest NRM intensity (~1500 A/m). As such it is a leading candidate for Mars crustal magnetism, particularly in proximity to the large impact basins where pressures > 1 GPa may have been experienced. The presence of this mineral suggests that much of the deep Martian crust was oxidized at the time of acquisition of magnetic remanence. This would be an important constraint for Martian chemical evolution at the time of crustal formation.

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