¹Yasuhito Sekine et al. (>10*)
¹Department of Earth and Planetary Science, University of Tokyo, Bunkyo 113-0033, Japan
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Reference
Sekine Y et al. (2015) High-temperature water–rock interactions and hydrothermal environments in the chondrite-like core of Enceladus. Nature Communications 6, 8604 Link to Article [doi:10.1038/ncomms9604]

^1,2Kathryn H. McDermott, ¹Richard C. Greenwood, ³Edward R.D. Scott, ¹Ian A. Franchi, ⁴Mahesh Anand
¹Planetary and Space Sciences, The Open University, Walton Hall, Milton Keynes, MK7 6AA
²School of Physical Sciences, University of Kent, Canterbury, CT2 7NH
³Hawaii Institute of Geophysics and Planetology, University of Hawaii, Honolulu, HI 96822, USA
⁴Department of Earth Sciences, The Natural History Museum, London, SW7 5BD

The origin of silicate-bearing irons, especially those in groups IAB, IIICD, and IIE, is poorly understood as silicate should have separated rapidly from molten metal. Here we report the results of high precision oxygen isotope analysis of silicate inclusions in eleven group IIE meteorites and a petrological study of silicate inclusions in ten IIE irons including those in Garhi Yasin and Tarahumara, which have not been described in detail before. Oxygen isotopes have also been analysed in 20 H chondrites to investigate their possible relationship with the IIE irons.

Based on petrographic observations and mineral analysis, the silicate-bearing IIE meteorites have been divided into four types according to the nature of their silicate inclusions: 1) primitive chondritic, 2) evolved chondritic, 3) differentiated with >10 vol.% orthopyroxene, and 4) differentiated with

Our data suggest that the IIE meteorites formed on an internally heated H/HH chondrite-like body that experienced the initial stages of differentiation in response to radiogenic heating. However, prior to full differentiation the IIE parent body experienced a major hit-and-run style collision that resulted in silicate-metal mixing. The initial stages of this event involved a phase of rapid cooling that prevented unmixing of metal and silicates. Reassembly of the IIE parent body produced a large regolith blanket that facilitated subsequent slow cooling. The IIE parent body has probably experienced numerous subsequent less catastrophic collisions. The development of alkali glass textures in some differentiated inclusions is probably the result of one of these later events.

Reference
McDermott KH, Greenwood RC, Scott ERD, Franchi IA, Anand M (2015) Oxygen isotope and petrological study of silicate inclusions in IIE iron meteorites and their relationship with H chondrites. Geochimica et Cosmochimica Acta (in Presss)
Link to Article [doi:10.1016/j.gca.2015.10.014]
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