Volatile Evolution and Loss

作者: A. M. Davis

DOI:

关键词:

摘要: Relative to bulk solar system composition, most meteorites and the terrestrial planets are depleted in volatile elements. This abundance pattern likely arose nebula rather than during planet formation. The record of element abundances is reviewed constraints on its origin from isotopic compositions presolar grains primitive explored. Major models for volatility fractionations described.

参考文章(87)
John T. Wasson, Byeon-Gak Choi, Main-group pallasites: chemical composition, relationship to IIIAB irons, and origin Geochimica et Cosmochimica Acta. ,vol. 67, pp. 3079- 3096 ,(2003) , 10.1016/S0016-7037(03)00306-5
M. I. Petaev, J. A. Wood, Meteoritic Constraints on Temperatures, Pressures, Cooling Rates, Chemical Compositions and Modes of Condensation in the Solar Nebula Chondrites and the Protoplanetary Disk. ,vol. 341, pp. 373- ,(2005)
John W. Larimer, The cosmochemical classification of the elements. Meteorites and the Early Solar System. pp. 375- 389 ,(1988)
Kazuhito Ozawa, Hiroko Nagahara, Chemical and isotopic fractionations by evaporation and their cosmochemical implications Geochimica et Cosmochimica Acta. ,vol. 65, pp. 2171- 2199 ,(2001) , 10.1016/S0016-7037(01)00578-6