A strongly hydrated microclast in the Rumuruti chondrite <scp>NWA</scp> 6828: Implications for the distribution of hydrous material in the solar system

• Published in: Meteoritics & Planetary Science
• Main Author: Greshake, Ansgar
• Format: Article in Journal/Newspaper
• Language: English
• Published: Wiley 2014
• Subjects: Space and Planetary Science; Geophysics; Tagish; Tagish Lake
• Online Access: http://dx.doi.org/10.1111/maps.12295; https://api.wiley.com/onlinelibrary/tdm/v1/articles/10.1111%2Fmaps.12295; https://onlinelibrary.wiley.com/doi/pdf/10.1111/maps.12295

Abstract Hydrous carbonaceous microclasts are by far the most abundant foreign fragments in stony meteorites and mostly resemble CI 1‐, CM 2‐, or CR 2‐like material. Their occurrence is of great importance for understanding the distribution and migration of water‐bearing volatile‐rich matter in the solar system. This paper reports the first finding of a strongly hydrated microclast in a Rumuruti chondrite. The R3‐6 chondrite Northwest Africa 6828 contains a 420 × 325 μm sized angular foreign fragment exhibiting sharp boundaries to the surrounding R‐type matrix. The clast is dominantly composed of magnetite, pyrrhotite, rare Ca‐carbonate, and very rare Mg‐rich olivine set in an abundant fine‐grained phyllosilicate‐rich matrix. Phyllosilicates are serpentine and saponite. One region of the clast is dominated by forsteritic olivine (Fa &lt;2 ) supported by a network of interstitial Ca‐carbonate. The clast is crosscut by Ca‐carbonate‐filled veins and lacks any chondrules, calcium‐aluminum‐rich inclusions, or their respective pseudomorphs. The hydrous clast contains also a single grain of the very rare phosphide andreyivanovite. Comparison with CI 1, CM 2, and CR 2 chondrites as well as with the ungrouped C2 chondrite Tagish Lake shows no positive match with any of these types of meteorites. The clast may, thus, either represent a fragment of an unsampled lithology of the hydrous carbonaceous chondrite parent asteroids or constitute a sample from an as yet unknown parent body, maybe even a comet. Rumuruti chondrites are a unique group of highly oxidized meteorites that probably accreted at a heliocentric distance &gt;1 AU between the formation regions of ordinary and carbonaceous chondrites. The occurrence of a hydrous microclast in an R chondrite attests to the presence of such material also in this region at least at some point in time and documents the wide distribution of water‐bearing (possibly zodiacal cloud) material in the solar system.