Windows on Martian dynamo history: electron reflection (ER) magnetic signatures and crater retention ages of basins and volcanoes

Details Windows on Martian dynamo history: electron reflection (ER) magnetic signatures and crater retention ages of basins and volcanoes Windows on Martian dynamo history: electron reflection (ER) magnetic signatures and crater retention ages of basins and volcanoes

Dec 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006agufmgp23a..05l&link_type=abstract

American Geophysical Union, Fall Meeting 2006, abstract #GP23A-05

Physics

5420 Impact Phenomena, Cratering (6022, 8136), 5430 Interiors (8147), 5440 Magnetic Fields And Magnetism, 5443 Magnetospheres (2756), 5480 Volcanism (6063, 8148, 8450)

Scientific paper

A picture continues to emerge of a Martian dynamo that began extremely early in the planet's history. After reversing polarity at least once and possibly varying significantly in strength, it permanently ceased operating prior to 4 billion years ago (using the Hartmann-Neukum chronology), when the core could no longer sustain the required convective motion. By combining ER magnetometry and MOLA topography, we use the derived magnetic signatures and crater retention ages (CRAs) of large basins and volcanoes to constrain the ambient magnetic conditions present during their formation. Here we present results that support the above picture; in particular case studies involving several large visible and buried basins and highland volcanoes, implying that Mars' last dynamo activity likely ceased prior to 4.07 ± 0.04 Gyr ago and later than 4.15 ± 0.05 Gyr ago and that this cessation was, within uncertainties, coincident with the formation of the 3 giant northern lowland basins Acidalia, Chryse and Utopia. We also present a statistical study of the magnetic signatures and CRAs of the ~500 largest basins on Mars which tentatively suggests that the dynamo may have weakened considerably for a period during its active lifetime.

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