^1,2Jangmi Han,²Lindsay P.Keller,³Ming-Chang Liu,^1,2Andrew W.Needham,³Andreas T.Hertwig,² Scott Messenger,²Justin I.Simon
Geochimica et Cosmochimica Acta (in Press) Link to Article [https://doi.org/10.1016/j.gca.2019.10.042]
¹Lunar and Planetary Institute, USRA, 3600 Bay Area Boulevard, Houston, TX 77058, USA
²Astromaterials Research and Exploration Science, NASA Johnson Space Center, Houston, TX 77058, USA
³Department of Earth, Planetary, and Space Sciences, University of California, Los Angeles, Los Angeles, CA 90095, USA
Copyright Elsevier

We carried out a coordinated mineralogical and isotopic study of a Wark-Lovering (WL) rim on a Ca,Al-rich inclusion (CAI) from the reduced CV3 chondrite Vigarano. The outermost edge of the CAI mantle is mineralogically and texturally distinct compared to the underlying mantle that is composed of coarse, zoned melilite (Åk_∼10-60) grains. The mantle edge contains fine-grained gehlenite with hibonite and rare grossite that likely formed by rapid crystallization from a melt enriched in Ca and Al. These gehlenite and hibonite layers are surrounded by successive layers of spinel, zoned melilite (Åk_∼0-10), zoned diopside that grades outwards from Al,Ti-rich to Al,Ti-poor, and forsteritic olivine intergrown with diopside. These layered textures are indicative of sequential condensation of spinel, melilite, diopside, and forsterite onto hibonite. Anorthite occurs as a discontinuous layer that corrodes adjacent melilite and Al-diopside, and appears to have replaced them, probably even later than the forsterite layer formation. Based on these observations, we conclude that the WL rim formation was initiated by flash melting and extensive evaporation of the original inclusion edge, followed by subsequent gas-solid reactions under highly dynamic conditions.

All the WL rim minerals are ¹⁶O-rich (Δ¹⁷O = ∼−23‰), indicating their formation in an ¹⁶O-rich nebular reservoir. Our Al-Mg measurements of hibonite, spinel, and diopside from the WL rim, as well as spinel and Al,Ti-diopside in the core, define a single, well-correlated isochron with an inferred initial ²⁶Al/²⁷Al ratio of (4.94 ± 0.12) × 10⁻⁵. This indicates that the WL rim formed shortly after the host CAI. In contrast, the lack of ²⁶Mg excesses in the WL rim anorthite suggest its later formation or later isotopic disturbance in the solar nebula, after ²⁶Al had decayed.

^1,2Bucurica, I.A.,^1,3Radulescu, C.,⁴Poinescu, A.A.,^1,3,5Popescu, I.V.,¹Nicolescu, C.M.,¹Teodorescu, S.,³Bumbac, M.,⁶Pehoiu, G.,⁶Murarescu, O.
Romanian Journal of Physics 64, 906 Link to Article [http://www.nipne.ro/rjp/2019_64_7-8.html]
¹Valahia University of Targoviste, Institute of Multidisciplinary Research for Science and Technology, Targoviste, 130004, Romania
²University of Bucharest, Faculty of Physics, Doctoral School of Physics, Bucharest, 050107, Romania
³Valahia University of Targoviste, Faculty of Sciences and Arts, Targoviste, 130004, Romania
⁴Valahia University of Targoviste, Faculty of Materials Engineering and Mechanics, Targoviste, 130004, Romania
⁵Academy of Romanian Scientists, Bucharest, 050094, Romania
⁶Valahia University of Targoviste, Faculty of Humanities, Targoviste, 130105, Romania

We currently do not have a copyright agreement with this publisher and cannot display the abstract here

¹Johnson, B.C.,²Sori, M.M.,³Evans, A.J.
Nature Astronomy (in Press) Link to Article [DOI: 10.1038/s41550-019-0885-x]
¹Department of Earth, Atmospheric, and Planetary Sciences, Purdue University, West Lafayette, IN, United States
²Lunar and Planetary Laboratory, University of Arizona, Tucson, AZ, United States
³Department of Earth, Environmental and Planetary Sciences, Brown University, Providence, RI, United States

We currently do not have a copyright agreement with this publisher and cannot display the abstract here