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The evolution of the moon and the terrestrial planetsThe thermal evolutions of the Moon, Mars, Venus and Mercury are calculated theoretically starting from cosmochemical condensation models. An assortment of geological, geochemical and geophysical data are used to constrain both the present day temperatures and the thermal histories of the planets' interiors. Such data imply that the planets were heated during or shortly after formation and that all the terrestrial planets started their differentiations early in their history. The moon, smallest in size, is characterized as a differentiated body with a crust, a thick solid mantle and an interior region which may be partially molten. Mars, intermediate in size, is assumed to have differentiated an Fe-FeS core. Venus is characterized as a planet not unlike the earth in many respects. Core formation has occurred probably during the first billion years after the formation. Mercury, which probably has a large core, may have a 500 km thick solid lithosphere and a partially molten core if it is assumed that some heat sources exist in the core.
Document ID
19750006618
Acquisition Source
Legacy CDMS
Document Type
Conference Paper
Authors
Toksoez, M. N.
(Massachusetts Inst. of Tech. Cambridge, MA, United States)
Johnston, D. H.
(Massachusetts Inst. of Tech. Cambridge, MA, United States)
Date Acquired
September 3, 2013
Publication Date
April 1, 1974
Publication Information
Publisher: NASA
Subject Category
Lunar And Planetary Exploration
Report/Patent Number
NASA-CR-141252
REPT-223
Meeting Information
Meeting: Sov.-Am. Conf. on the Cosmochem. of the Moon and Planets
Location: Moscow
Country: Soviet Union
Start Date: June 4, 1974
End Date: June 8, 1974
Accession Number
75N14690
Funding Number(s)
CONTRACT_GRANT: NGL-22-009-187
CONTRACT_GRANT: NAS1-9703
CONTRACT_GRANT: NSG-7081
Distribution Limits
Public
Copyright
Work of the US Gov. Public Use Permitted.
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