Inclusion MS-MU-002

(ELb3/4 in Weyrauch et al., 2018)
standby for ms-mu-002 photo
Fell October 7, 2008
20° 43.04' N., 32° 30.58' E.

In 2008, October 6 at 5:46 A.M., asteroid 2008 TC3 fell to Earth in northern Sudan. See the Almahata Sitta webpage for the complete story of the discovery of this meteorite, results of the consortium analyses, and new models for the petrogenetic history of the ureilite parent body.

The 2008 TC3 meteorite was sent to NASA's Johnson Space Center in Houston (Zolensky) and Carnegie Institution of Washington (Steele) for analysis and classification, and Almahata Sitta was determined to be a polymict ureilite fragmental breccia composed of three main ureilite lithologies, along with a wide range of xenolithic clasts representing many different chondritic and achondritic lithologies in an assemblage similar to the polymict breccia Kaidun (Bischoff et al., 2010). Results of the analyses indicate that all of the clasts came from the Almahata Sitta fall; e.g., detection of short-lived cosmogenic nuclides, very low weathering grade (W0–W0/1), multiple lithologies among fragments delimiting a strewn field, a high number of rare E-chondrite rock types found together, diffusion of PAHs among clasts [Sabbah et al., 2010], and the finding of new and unique meteorite fragments within a small area.

The heterogeneous composition of Almahata Sitta could reflect an assemblage derived from a catastrophic collision(s) between ureilite and chondrite objects (Kohout et al., 2010). Alternatively, it is considered likely that these diverse clasts could have become gravitationally bound within a common debris disk composed of a disrupted ureilite asteroid, and that this disk then re-accreted into one or more smaller second-generation asteroids. This second-generation asteroid later became lightly sintered together through subsequent low-energy impacts, resulting in a bulk porosity of ~50%. This fine-grained, highly-porous, weakly-consolidated matrix material is possibly represented by the recovered specimen MS-168 and/or the C1+URE+OC+EH regolith breccia clasts AhS 91/91A and 671; this would be consistent with the reflectance spectra obtained for the asteroid (Goodrich et al., 2015, 2019).

Inclusion MS-MU-002 was analyzed and classified at the University in Münster, Germany (A. Bischoff), and it was determined to be a very rare and uniquely pristine EL3 chondrite associated with the Almahata Sitta fall. The entire MS-MU-002 inclusion had dimensions of 1.28 × 1.15 × 1.07 cm, and weighed only 3.0 g before it was sectioned into several slices. Other EL3 clasts recovered from the Almahata Sitta strewn field include MS-17 and MS-177, initially characterized by Goresy et al. (2012).

Although classification of MS-MU-002 by magnetic susceptibility alone (5.26; Hoffmann et al., 2016) cannot discriminate between EH and EL chondrite groups, the observed values for a variety of parameters can help resolve the genetic relationship. For example, FeNi-metal in MS-MU-002 contains kamacite with ~1.4 wt% Si (EL: 0.3–2.1 wt%; EH: 1.9–3.8 wt%). Also, the sulfides that are present include troilite, oldhamite, and keilitic alabandite. Keilitic alabandite is representative of the Fe,Mn-rich end member of the solid solution series ([Mg,Mn,Fe]S) which occurs only in EL chondrites, in contrast to the Mg-rich end member (niningerite) found in EH chondrites. Inclusion MS-MU-002 contains chondrules with diameters of 0.2–0.5 mm (no average available), a size which overlaps the averages for both E-chondrite groups (EL3: ave. 0.55 mm; EH3: ave. 0.22 mm). A more complete list of EL/EH discriminators can be found on the NWA 3132 page.

Weyrauch et al. (2018) analyzed the mineral and chemical data from 80 enstatite chondrites representing both EH and EL groups and spanning the full range of petrologic types for each group. They found that a bimodality exists in each of these groups with respect to both the Cr content in troilite and the Fe concentration in niningerite and alabandite. In addition, both the presence or absence of daubréelite and the content of Ni in kamacite were demonstrated to be consistent factors for the resolution of four distinct E chondrite groups: EHa, EHb, ELa, and ELb (see table below).

Weyrauch et al., 2018
  EHa EHb ELa ELb
Troilite Cr <2 wt% Cr >2 wt% Cr <2 wt% Cr >2 wt%
(Mn,Mg,Fe)S Fe <20 wt% Fe >20 wt% Fe <20 wt% Fe >20 wt%
Daubréelite Abundant Missing Abundant Missing
Kamacite Ni <6.5 wt% Ni >6.5 wt% Ni <6.5 wt% Ni >6.5 wt%

A few other E chondrites with intermediate mineralogy have been identified, including LAP 031220 (EH4), QUE 94204 (EH7), Y-793225 (E-an), LEW 87223 [EL3-an; abs], and PCA 91020 (possibly related to LEW 87223). Studies have determined that these meteorites were not derived from the EH or EL source through any metamorphic processes, and some or all of them could represent separate E chondrite asteroids. The revised E chondrite classification scheme of Weyrauch et al. (2018) including selected examples from their 80-sample study can be found here. It was determined that MS-MU-002 is a member of the ELb subgroup.

Petrographic and isotopic evidence indicate that the EL parent body accreted hot silicate and metal components that were formed through repeated nebular condensation processes rather than by impact-heating events on a parent body (Weisberg et al., 2013). Observations consistent with a nebular condensation origin include the absence of shock-induced features, the lack of high-pressure polymorphs, the presence of metal–sinoite–oldhamite–graphite assemblages composed of crystalline sinoite and poorly graphitized carbon, and the pristine texture of discrete chondrules and metal nodules, while the isotopic inventory is inconsistent with a large-scale impact-heating event. A high abundance of metal in the final agglomeration is also expected with the presumed nebular condensation sequence.

The broad diversity of lithologic types present in 2008 TC3 constituted <30% of all material recovered. However, given that the vast bulk of 2008 TC3 is thought to have been lost as fine dust (≥99.9% of the estimated 42–83 ton pre-atmospheric mass), the asteroid was likely composed predominantly of very fine-grained, highly-porous, weakly-consolidated matrix material, possibly represented by the recovered specimen MS-168 and/or the C1+URE+OC+EH regolith breccia clasts AhS 91/91A and 671; this would be consistent with the reflectance spectra and other data obtained for the asteroid (Goodrich et al., 2015, 2019; Bischoff et al., 2022). Examples of some of the diverse samples that have been recovered are listed below (Bischoff et al., 2010, 2015, 2016, 2018, 2019; Horstmann and Bischoff, 2010, 2014; Hoffmann et al., 2016; Fioretti et al., 2017; Goodrich et al., 2018, 2019):

Special thanks to Siegfried Haberer and Stephan Decker for providing specimens of this special meteorite and many of its xenolithic inclusions to the scientific and collector communities. The photo of MS-MU-002 shown above is a 0.350 g full slice. The photo below shows the 3.00 g main mass.

standby for ms-mu-002 photo
Photo courtesy of Stephan Decker—Meteorite Shop and Museum

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