Petrology and origin of amoeboid olivine aggregates in CR chondrites
Article first published online: 26 JAN 2010
2004 The Meteoritical Society
Meteoritics & Planetary Science
Volume 39, Issue 10, pages 1741–1753, October 2004
How to Cite
WEISBERG, M. K., CONNOLLY, H. C. and EBEL, D. S. (2004), Petrology and origin of amoeboid olivine aggregates in CR chondrites. Meteoritics & Planetary Science, 39: 1741–1753. doi: 10.1111/j.1945-5100.2004.tb00070.x
- Issue published online: 26 JAN 2010
- Article first published online: 26 JAN 2010
- Received 18 September 2003; revision accepted 28 July 2004
Abstract— Amoeboid olivine aggregates (AOAs) are irregularly shaped, fine-grained aggregates of olivine and Ca, Al-rich minerals and are important primitive components of CR chondrites. The AOAs in CR chondrites contain FeNi metal, and some AOAs contain Mn-rich forsterite with up to 0.7 MnO and Mn:Fe ratios greater than one. Additionally, AOAs in the CR chondrites do not contain secondary phases (nepheline and fayalitic olivine) that are found in AOAs in some CV chondrites. The AOAs in CR chondrites record a complex petrogenetic history that included nebular gas-solid condensation, reaction of minerals with the nebular gas, small degrees of melting, and sintering of the assemblage. A condensation origin for the Mn-rich forsterite is proposed. The Mn-rich forsterite found in IDPs, unequilibrated ordinary chondrite matrix, and AOAs in CR chondrites may have had a similar origin.
A type A calcium, aluminum-rich inclusion (CAI) with an AOA attached to its Wark-Lovering rim is also described. This discovery reveals a temporal relationship between AOAs and type A inclusions. Additionally, a thin layer of forsterite is present as part of the Wark-Lovering rim, revealing the crystallization of olivine at the end stages of Wark-Lovering rim formation. The Ca, Al-rich nodules in the AOAs may be petrogenetically related to the Ca, Al-rich minerals in Wark-Lovering rims on type A CAIs. AOAs are chondrite components that condensed during the final stage of Wark-Lovering rim formation but, in general, were temporally, spatially, or kinetically isolated from reacting with the nebula vapor during condensation of the lower temperature minerals that were commonly present as chondrule precursors.