Internal and tectonic evolution of Mercury

Details Internal and tectonic evolution of Mercury Internal and tectonic evolution of Mercury

Apr 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003eaeja....11092h&link_type=abstract

EGS - AGU - EUG Joint Assembly, Abstracts from the meeting held in Nice, France, 6 - 11 April 2003, abstract #11092

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Mercury's geologic and internal evolution presents an interesting question: what are the conditions that both allow for apparently limited radial contraction (as recorded in the lobate scarps observed by Mariner 10) over the last 4 billion years and yet permit the core to cool at a sufficiently rapid rate to drive the present-day internal magnetic field? We simulate the coupled thermal, magmatic, and tectonic evolution of Mercury for a range of parameters (e.g., mantle rheology, internal heat production, core sulfur content) in order to explore the set of model characteristics most consistent with these dual observational constraints. We find that a strong (dry) mantle rheology combined with a core containing moderate amounts of sulfur may be consistent with ~1-2 km of radial contraction since 4 Ga and a present-day core dynamo-generated magnetic field. In cases where the core is presently entirely liquid, heat extraction from the core by the mantle is too small to drive convection in the core. Inner core growth, with its attendant release of latent heat and gravitational energy as well as compositional buoyancy induced mixing, is therefore a critical element for maintaining a core dynamo should Mercury's magnetic field be of non-crustal origin. Future observations of Mercury by the MESSENGER and BepiColombo spacecraft will elucidate further the internal structure and evolution of the planet.

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