DAR AL GANI 084


Ureilite
Monomict/Unbrecciated
Olivine–pigeonite

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Found 1995
27° 02.44' N., 16° 24.26' E.

Two paired stones of this ureilite were found on the Dar al Gani plateau in the Sahara Desert, which have a total weight of 277 g. The brecciated, highly-shocked DaG 084 exhibits mosaicism in its olivines and has experienced heavy terrestrial weathering consistent with grade W3. The meteorite belongs to Berkley's fayalite-rich subgroup I, having a Mg# in the range of Fo76–87. This ureilite is probably paired with DaG 164 (57 g) and DaG 165 (32 g), and possibly with numerous other monomict and polymict named masses that were found in close proximity. All of these individual stones might represent the breakup of a >7 kg polymict regolith fragment (Downes et al., 2010).

A Mn–Cr isotopic study was conducted by Shukolykov and Lugmair (2006) on the possibly paired polymict ureilite DaG 165 and some others. Their results indicate that DaG 165 last equilibrated very early in Solar System history, ~4.562 b.y. ago, which is much earlier than Kenna.

In an attempt to identify possible common ejection events among the ureilites, Beard and Swindle (2017) conducted a comparative study of 39 different samples utilizing three parameters: CRE age, Fo content in olivine (Mg#), and Δ17O value. They resolved ten potential clusters, several of which show concordance in their CRE age and Mg# but not in Δ17O value (heterogeneous), and three that are concordant in all three parameters (homogeneous). One of the homogeneous clusters reflects an ejection event that occurred 20.1 (±1.2) m.y. ago and comprises DaG 084, DaG 319, Goalpara, and Haverö; however, the Δ17O values for DaG 084 and DaG 319 have not yet been determined. The CRE age of this cluster is consistent with the average of all CRE age results obtained to date of 19.7 (±2.8) m.y. (Riebe et al., 2017).

Current theories of ureilite formation are presented on the Kenna and Almahata Sitta pages. The photo above shows the cut face of this 15.6 g DaG 084 specimen. The photo below shows the outer surface where remnant fusion crust has been affected by desert varnish, while light-colored desert soil still adheres to the part of the stone that laid beneath the surface.

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