Other
Scientific paper
Dec 2001
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001agufmgp32a0191h&link_type=abstract
American Geophysical Union, Fall Meeting 2001, abstract #GP32A-0191
Other
1540 Rock And Mineral Magnetism, 5420 Impact Phenomena (Includes Cratering), 5440 Magnetic Fields And Magnetism, 6250 Moon (1221)
Scientific paper
Experiments have shown that shock can act to magnetize or demagnetize terrestrial and lunar rocks. In the presence of strong magnetic fields shock pressures of tens of kbar have been shown to impart stable magnetic remanence. Meanwhile, in the absence of significant ambient fields, shock pressures of only a few kbar have been found to reduce remanent magnetism. Data from the Apollo missions and Lunar Prospector have made it clear that impacts control the global distribution of remanent crustal magnetism on the Moon. Many of the strongest regions of magnetic field are associated with the antipodes of large impact basins or with discontinuous basin ejecta. On the other hand, the impact basins themselves and their continuous ejecta blankets show weak or nonexistent remanent magnetism. If thermal remanent magnetization were responsible one would expect quite a different signature. This suggests that shock remanent magnetization is the dominant process. Meanwhile, impact basins and craters are generally demagnetized relative to their surroundings. Thermal or shock effects could conceivably be responsible. However, thermal effects should only be effective at relatively small distances from the impact center, while shock pressures sufficient to demagnetize can be generated at distances of at least 1.5-2 crater radii. We observe demagnetization signatures which extend to several crater radii, providing strong evidence that shock demagnetization is responsible.
Acuña Mario Humberto
Binder Alan B.
Halekas Jasper S.
Hood Lon L.
Lin Robert P.
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