The strange density of Mercury - Theoretical considerationsTwo classes of models which have been advanced to explain the high density of Mercury are reviewed and contrasted. These models invoke either the differing volatilities of iron and silicates or disruptive collisions to fractionate the two phases. Also contrasted are equilibrium condensation and planetary vaporization models, both of which fall within the first broad class considered. Results indicate that equilibrium condensation models are unable to account for the observed high density of Mercury without invoking special mechanisms such as unrealistically narrow planetary accretion zones. However, it is found that distinctive chemical differences, which are potentially testable by spacecraft experiments, provide means for distinguishing between planetary vaporization and large impact scenarios.
Document ID
19890056403
Acquisition Source
Legacy CDMS
Document Type
Conference Proceedings
Authors
Cameron, A. G. W. (Harvard-Smithsonian Center for Astrophysics Cambridge, MA, United States)
Benz, Willy (Harvard-Smithsonian Center for Astrophysics Cambridge, MA, United States)
Fegley, Bruce, Jr. (MIT Cambridge, MA, United States)
Slattery, Wayne L. (Los Alamos National Laboratory NM, United States)