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1 Natural History Museum of Denmark, Natural History Museum of Denmark, Faculty of Science, Københavns Universitet 2 Natural History Museum of Denmark, Faculty of Science, Københavns Universitet 3 Geological Museum, Natural History Museum of Denmark, Faculty of Science, Københavns Universitet 4 University of Copenhagen 5 Natural History Museum of Denmark, Faculty of Science, Københavns Universitet 6 Geological Museum, Natural History Museum of Denmark, Faculty of Science, Københavns Universitet 7 Natural History Museum of Denmark, Natural History Museum of Denmark, Faculty of Science, Københavns Universitet
Chondrules are igneous spherical objects preserved in chondritic meteorites and believed to have formed during transient heating events in the solar protoplanetary disk. Chondrules present in the metal-rich CB chondrites show unusual chemical and petrologic features not observed in other chondrite groups, implying a markedly distinct formation mechanism. Here, we report high-precision Mg-isotope data for 10 skeletal olivine chondrules from the Hammadah al Hamra 237 (HH237) chondrite to probe the formation history of CB chondrules. The Al/Mg ratios of individual chondrules are positively correlated to their stable Mg-isotope composition (μMg), indicating that the correlated variability was imparted by a volatility-controlled process (evaporation/condensation). The mass-independent Mg composition (μMg*) of chondrules is consistent with single stage formation from an initially homogeneous magnesium reservoir if the observed μMg variability was generated by non-ideal Rayleigh-type evaporative fractionation characterized by a β value of 0.5142, in agreement with experimental work. The magnitude of the mass-dependent fractionation (∼300 ppm) is significantly lower than that suggested by the increase in Al/Mg values, indicating substantial suppression of isotopic fractionation during evaporative loss of Mg, possibly due to evaporation at high Mg partial pressure. Thus, the Mg-isotope data of skeletal chondrules from HH237 are consistent with their origin as melts produced in the impact-generated plume of colliding planetesimals. The inferred μMg* value of -3.87 ± 0.93 ppm for the CB parent body is significantly lower than the bulk solar system value of 4.5 ± 1.1 ppm inferred from CI chondrites, suggesting that CB chondrites accreted material comprising an early formed Al-free component. © 2013. The American Astronomical Society. All rights reserved.
Astrophysical Journal. Letters, 2013, Vol 776, Issue 1
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