Fluid Flow and Chemical Alteration in Carbonaceous Chondrite Parent Bodies

Details Fluid Flow and Chemical Alteration in Carbonaceous Chondrite Parent Bodies Fluid Flow and Chemical Alteration in Carbonaceous Chondrite Parent Bodies

Dec 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009agufm.p42b..04p&link_type=abstract

American Geophysical Union, Fall Meeting 2009, abstract #P42B-04

Mathematics

Logic

[1009] Geochemistry / Geochemical Modeling, [1028] Geochemistry / Composition Of Meteorites, [6205] Planetary Sciences: Solar System Objects / Asteroids

Scientific paper

Carbonaceous chondrites are a suite of primitive meteorites with bulk chemical compositions that closely resemble solar values for non-volatile elements. On this basis, carbonaceous chondrites are considered among the most primitive materials available for study and, therefore, a critical source of information on the formation and evolution of our planetary system. However, despite carbonaceous chondrites' primitive characteristics, mineralogical and isotopic observations indicate that most have been modified by geochemical processing of their parent bodies (i.e., the asteroidal bodies from which the chondrites are derived). Therefore, although they possess a primitive bulk chemistry, it is clear that carbonaceous chondrites are not pristine samples. Elucidating the complex formation history of aqueously altered chondrite groups has been a principal objective of cosmochemistry. Fulfilling this objective requires understanding the nature of the water-rock interactions involved. Current alteration models are generally founded upon an assumption of uniform alteration in a closed system. In these models, there is no fluid circulation and different chondrite groups must originate on separate parent bodies. Until recently, little work has been done to investigate the consequences of fluid flow and chemical alteration in carbonaceous chondrite parent bodies. However, stability analyses of pore water in permeable, spherical bodies have established that many asteroidal bodies likely experienced a period of convective flow. Contrary to the closed system models, we show, through hydrothermal simulations, that chondrite data are consistent with non-uniform alteration in a convecting (open) system. Our results support the idea that distinct chondrite groups could form at different locations within the same body and are not required to originate on separate parent bodies. On this basis, we re-evaluate the origin of carbonaceous chondrites and the a priori assumption of closed system alteration.

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