JpGU-AGU Joint Meeting 2017

Presentation information

[JJ] Poster

P (Space and Planetary Sciences) » P-PS Planetary Sciences

[P-PS10] [JJ] Formation and evolution of planetary materials in the solar system

Mon. May 22, 2017 5:15 PM - 6:30 PM Poster Hall (International Exhibition Hall HALL7)

[PPS10-P05] Chondrule-cored aggregates (ChCAs): A new rock-type in CV chondrites with implications for timing of high-T crystallization events in the solar nebula

*Toshiki Yasuda1, Timothy Fagan1, Alexander N. Krot2, Kazu Nagashima2 (1.Waseda University, 2.University of Hawai'i)

Keywords:chondrules, solar nebula, oxygen isotopes

Introduction: Ca-Al-rich inclusions (CAIs) and amoeboid olivine aggregates (AOAs) formed by high-temperature reactions between gas and solids, and in some cases liquids, in a hot (ambient temperature > 1400K) region of the protoplanetary disk during initial stages of its evolution [1]. CAIs and AOAs in chondrites of petrologic types < 3.0 tend to be 16O-rich (Δ17O ≤ -20‰). In contrast, chondrules formed at lower ambient temperatures (<900K) and tend to be 16O-poor compared to CAIs (Δ17O ≥ -10‰). Most chondrules appear to have postdated formation of CAIs and AOAs, though initial stages of chondrule formation might have overlapped with CAIs and AOAs [2,3]. Because of the later formation age of many chondrules, relict CAIs may be found included within chondrules [4], but chondrule fragments included in CAIs are very rare [5].
In this project, we describe minerals, textures and oxygen isotopes of three unusual objects from the CV3 chondrites Allende and Vigarano in which relict chondrule phenocrysts are partially enclosed by granular olivine texturally similar to AOAs. We refer to these objects as chondrule-cored aggregates (ChCAs). They are significant because their textures suggest the opposite of the conventionally accepted timing; namely, in ChCAs, an early stage of chondrule formation was apparently followed by a later stage of olivine condensation.
Methods: Two ChCAs (called NE-27 and SW-7) were identified in Allende, and one (NW-30) was found in Vigarano. Minerals and textures were characterized using petrographic microscopes, a scanning electron microscope (Hitachi S-3400N) and a JEOL JXA 8900 electron probe micro-analyzer (EPMA) at Waseda University. Oxygen isotopic compositions of olivine in the Allende ChCAs were collected using the Cameca ims-1280 SIMS at University of Hawai‘i using conditions similar to those described in [6]. Typical uncertainty including internal and external errors is ~0.6‰ in both d17O and d18O.
Results: In Allende ChCA NE-27, a large (>200 µm across), low-Ca pyroxene (En98Wo1) similar to a chondrule phenocryst occurs in the core. The relict phenocryst is rimmed by granular olivine grains approximately < 20 µm across. The olivine grains are zoned with cores as Mg-rich as Fo95 and rims of approximately Fo60. Olivines with compositions near Fo60 also occur in veins that cut across relict pyroxene. ChCA SW-7 has similar low-Ca pyroxene, granular olivine and vein olivine, but is composed of several nodules and has a more diffuse boundary with the Allende matrix. Vigarano ChCA NW-30 also has a core of low-Ca pyroxene. The granular olivine layer is not as complete as in the Allende ChCAs, but granular olivine does appear to replace low-Ca pyroxene near margins of ChCA NW-30.
SIMS oxygen isotope analyses of granular olivine from the Allende ChCAs fall near the Carbonaceous Chondrite Anhydrous Mineral and Primary Chondrule Mineral reference lines (see [7]) and form a spread of Δ17O values from -8 to -3‰. All measurements are from MgO-rich cores and avoid FeO-rich olivine rims. The 16O-poor isotopic composition indicates that the olivine rims of ChCAs did not form in a typical AOA-like setting. Regardless of O-isotopic setting, the ChCAs indicate (1) an early episode of chondrule formation, followed subsequently by (2) fragmentation or some process that released pyroxene phenocrysts from their host chondrules, (3) crystallization of granular olivine grains on the margins of relict phenocrysts, and (4) formation of Fe-rich olivine on rims of grains and in veins during metamorphism.
References: [1] Krot et al. (2009) GCA 73, 4963-4997. [2] Kita N.T. et al. (2005) in Krot et al. (eds) Chondrites and the Protoplanetary Disk, p. 558- 587. [3] Connelly et al. (2012) Science 338, 651-655. [4] Krot A.N. et al. (2007) MaPS 42, 1197-1219. [5] Itoh and Yurimoto. (2003) Nature 423, 728-731. [6] Nagashima K. et al. (2014) GCA 151, 49-67. [7] Ushikubo T. et al. (2012) GCA 90, 242-264.