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The moon as a high temperature condensate.The accretion during condensation mechanism, if it occurs during the early over-luminous stage of the sun, can explain the differences in composition of the terrestrial planets and the moon. An important factor is the variation of pressure and temperature with distance from the sun, and in the case of the moon and captured satellites of other planets, with distance from the median plane. Current estimates of the temperature and pressure in the solar nebula suggest that condensation will not be complete in the vicinity of the terrestrial planets, and that depending on location, iron, magnesium silicates and the volatiles will be at least partially held in the gaseous phase and subject to separation from the dust by solar wind and magnetic effects associated with the transfer of angular momentum just before the sun joins the Main Sequence. Many of the properties of the moon, including the 'enrichment' in Ca, Al, Ti, U, Th, Ba, Sr and the REE and the 'depletion' in Fe, Rb, K, Na and other volatiles can be understood if the moon represents a high temperature condensate from the solar nebula.
Document ID
19730058958
Acquisition Source
Legacy CDMS
Document Type
Reprint (Version printed in journal)
Authors
Anderson, D. L.
(California Institute of Technology Pasadena, Calif., United States)
Date Acquired
August 7, 2013
Publication Date
August 1, 1973
Subject Category
Space Sciences
Accession Number
73A43760
Funding Number(s)
CONTRACT_GRANT: NGL-05-002-069
Distribution Limits
Public
Copyright
Other

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