Shock-induced isotope evolution of hydrogen and carbon in meteorites

Details Shock-induced isotope evolution of hydrogen and carbon in meteorites Shock-induced isotope evolution of hydrogen and carbon in meteorites

Jun 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005georl..3211201m&link_type=abstract

Geophysical Research Letters, Volume 32, Issue 11, CiteID L11201

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2

Geochemistry: Stable Isotope Geochemistry (0454, 4870), Geochemistry: Composition Of Meteorites (3662, 6240), Geochemistry: Planetary Geochemistry (5405, 5410, 5704, 5709, 6005, 6008), Planetary Sciences: Comets And Small Bodies: Impact Phenomena (5420, 8136), Planetary Sciences: Solar System Objects: Meteorites And Tektites (1028, 3662)

Scientific paper

Single- and multiple-shock recovery experiments on Murchison meteorite samples were performed, to examine the shock-induced isotope behavior of their hydrogen and carbon contents. δD values of the shocked Murchison showed an initial increase from +10.6‰ to +59.1‰ before declining to -87.6‰, as the dehydrogenation progressed. Isotope behavior of δD can be controlled by dehydrogenation involving extremely large isotope fractionation and is attributed to the composition of organic matter in the Murchison. On the other hand, the behavior of δ13C simply decreased from -5.15‰ to -17.65‰ and is explainable by decarbonization only. The plot of those isotope data collected along devolatilization shows a variation curve that suggests the evolution of those isotopes in the meteorites. Shock is one of the processes effectively controlling the isotope features of the solar system.

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