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球粒陨石母体中的流体流动:解读小行星的成分。

Fluid flow in chondritic parent bodies: deciphering the compositions of planetesimals.

作者信息

Young ED, Ash RD, England P, Rumble D

机构信息

Department of Earth Sciences, University of Oxford, Parks Road, Oxford, OX1 3PR, UK. Geophysical Laboratory, Carnegie Institution of Washington, 5251 Broad Branch Road NW, Washington DC, 20015, USA.

出版信息

Science. 1999 Nov 12;286(5443):1331-5. doi: 10.1126/science.286.5443.1331.

Abstract

Alteration of the Allende meteorite caused shifts in oxygen isotope ratios along a single mass fractionation line. If alteration was caused by aqueous fluid, the pattern of oxygen isotope fractionation can be explained only by flow of reactive water down a temperature gradient. Down-temperature flow of aqueous fluid within planetesimals is sufficient to explain the mineralogical and oxygen isotopic diversity among CV, CM, and CI carbonaceous chondrites and displacement of the terrestrial planets from the primordial slope 1. 00 line on the oxygen three-isotope plot.

摘要

阿连德陨石的蚀变导致氧同位素比值沿单一质量分馏线发生变化。如果蚀变是由含水流体引起的,那么氧同位素分馏模式只能通过活性水沿温度梯度向下流动来解释。小行星体内含水流体的向下温度流动足以解释CV、CM和CI碳质球粒陨石之间的矿物学和氧同位素多样性,以及类地行星在氧三同位素图上相对于原始斜率1.00线的位移。

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