SAHARA 98034

Five fragments of a stony meteorite were found in the Sahara by a French team. These fragments fit together to constitute a single stone weighing 10.345 kg. The stone was subsequently purchased by Astronomical Research Network, and classification was completed at the Institut für Planetologie in Münster (A. Bischoff) as an H5 chondrite (Fa18, Fs17). Sahara 98034 has one of the highest porosities known in an ordinary chondrite (see photo enlargement below). It consists of chondrules and chondrule fragments, along with some hollow chondrules, surrounded by an extremely porous groundmass. FeNi-metal grains are abundant throughout. This meteorite has been shocked to stage S2 and terrestrially weathered to grade W2.

A proposed model for the development of high porosities in meteorites was presented in an article by Przylibski et al. in MAPS, no. 6, 2003. In Petrology of the Baszkówka L5 chondrite: A record of surface-forming processes on the parent body, the authors describe how an early collision of two thinly crusted, molten planetesimals occurred within the first two million years of solar system history. This collision produced a hot cloud of low-density chondritic material, which thereafter slowly accreted onto the surface of the larger body. This homogeneous material was then loosely welded together by hot, plastic, metal and sulfides. Material that remained near the surface of the body developed the highest porosities such as those found in Sahara 98034 and Baszkówka; those meteorites with somewhat less porosity, such as Mt. Tazerzait, were more deeply buried. These meteorites did not experience further recrystallization, and therefore their petrography reflects the conditions that existed during the earliest period of solar system history.

An alternative theory for the formation of porosity throughout the range of meteorite types was proposed by Strait and Consolmagno (2004). They suggest that the decompression that follows the passage of an impact shock wave could have created the observed range of porosities. However, later studies failed to show any correlation between porosity and metamorphic type, shock stage, brecciation, or even terrestrial weathering. In their study of density and porosity utilizing a broad range of meteorite types, Consolmagno et al. (2008) determined the porosity of a significant number of meteorites, including ordinary chondrites (8.6 [±5.4]%), enstatite chondrites (0.3–12.6%), primitive achondrites (11.5 [±3.6]%), and basaltic achondrites (similar to OC and EC), and they found that they all have very similar porosities. Only the carbonaceous chondrites (e.g., Murchison–CM: 22 [±2]%; Murray–CM: 28%; Warrenton–CO: 26%; Allende–CV 23.0 [±3.6]%; Axtell–CV 21 [±2]%) were found to have different, significantly higher porosities than the other meteorite groups. This is likely the result of unique accretion/lithification/compaction histories in their parent bodies at their particular formation regions in the nebula.

In a study by Wilkison et al. (2003), a formula was developed to quantify the microporosity of meteorites:

%porosity = [1-(grain volume ÷ bulk volume)] × 100

In their study of 30 ordinary chondrites, it was determined that typical microporosities range from 0% to 27%, with an average of ~6.4%; 95% of the samples had porosities below 20%. In an earlier study by Consolmagno et al. (1998), which utilized a larger data set representing 130 different chondrite porosity values, they demonstrated that the pre-weathering porosity for ordinary chondrites averaged ~10%. The CI chondrite Orgueil was determined to have the highest porosity at ~35%, and also the lowest measured bulk density (Consolmagno and Britt, 1998).

Although they have different bulk compositions, the bulk density of Orgueil compares well to that of certain asteroids including Phobos, Deimos, and Mathilde. Notably, Wilkison et al. (2003) found that the petrologic type, which corresponds to burial depth, is not correlated with porosity. Likewise, porosity is not correlated with chemical group (e. g., H, L, LL, CM, LUN, AUB, CHA; Strait and Consolmagno, 2004), bulk density, grain density (possibly weakly correlated), brecciation, shock stage (at least not below very strong shock or shock-melt pressure levels), or permeability (Corrigan et al., 1997). Consolmagno et al. (1998) found that terrestrial weathering leads to the filling of the pore spaces on a time scale of hundreds of years, but Coulson et al. (2007) find no relationship between porosity and terrestrial residency time. Furthermore, they found that porosity is not obviously correlated with crystallization age.

An extensive listing of individual meteorite densities and porosities for all chondrite groups, and many achondrite groups, is presented by Britt and Consolmagno in MAPS, no. 8, 2003. Interestingly, they found that porosities of the L chondrites (6%) are significantly different from those of both the H and LL chondrites (10%).

Low-density, porous material should be present in regolith breccias of asteroids, created by impact lithification of disordered material, as well as in deep fractures and fault zones; the S-type asteroids 433 Eros and 243 Ida, with ~10% microporosity plus ~20% macroporosity, are examples that exhibit both environments. The slice of Sahara 98034 pictured above weighs 56.9 g. The magnified image presented below demonstrates the unprecedented porosity of this special meteorite.