Iron, IAB complex, sLL subgroup
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Found 1776, known earlier
19° 34' N., 99° 34' W.

Many large masses were found near Xiquipilco, Mexico, the largest of which weighed 300 pounds. Recently, a taxonomic revision was proposed by Wasson and Kallemeyn (2002) that includes iron meteorites from the IAB-IIICD group, along with numerous IAB-related meteorites. On a Ni–Au diagram, Toluca and other similar irons resolve a low-Au, low-Ni subgroup (sLL).

The I–Xe closure age of Toluca was determined by Pravdivtseva et al. (2009) for both high-Mg and low-Mg pyroxenes, the two closure times differing by 8.5 (±4.4) m.y. An absolute closure age based on the Shallowater standard was calculated to be 4,560.5 (±2.4) m.y. for high-Mg pyroxenes and 4,552.0 (±3.7) m.y. for low-Mg pyroxenes, a range similar to that of other IAB iron silicates. The earlier closure age is likely commensurate with the catastrophic disruption of the IAB parent body. The research team also determined the cooling rate of Toluca following parent body breakup and reassembly. This was calculated as a function of the difference between the crystallization temperatures and closure ages of the two pyroxenes to be 14.5 (±10.0)°C/m.y.

A comparative study of the IAB iron main group (MG) and sLL subgroup by Worsham et al. (2013, 2016) demonstrated through Mo-isotopic compositions that both groups derive from a common parent body that was initially chondritic. In addition, they verified through HSE data that irons from these two groups crystallized from distinct parental melt pools, one of which could have been the core, and that the observed fractionations were not the result of fractional crystallization, but instead, most likely involved crystal segregation and other processes. Further evidence for formation in distinct melt pools among the IAB iron groups was found through cooling rate studies correlating the cloudy zone particle size with the metallographic cooling rate (Goldstein et al., 2013). Moreover, the slow cooling rates determined for the IAB irons and other meteorite groups containing silicate assemblages (e.g., pallasites and mesosiderites), were found to be inconsistent with the faster cooling rates attributed to those iron groups which underwent fractional crystallization in cores lacking insulating silicate mantles (e.g., IIIAB, IVA, and IVB).

Based on similar silicate textures, reduced mineral chemistry, and O-isotopes, it is presumed that the winonaites and the IAB complex irons originated on a common parent body. Utilizing a Ge/Ni vs. Au/Ni coupled diagram, Hidaka et al. (2015) determined that FeNi-metal in the winonaite Y-8005 plots in the field of the sLL subgroup of the IAB complex irons. In addition, the metal in this winonaite retains a near chondritic composition likely representative of the precursor material of the parent body. In view of these findings, they suggest that the sLL subgroup rather than the main group of the IAB complex represents the primitive metal of the IAB–winonaite parent body, with the main group possibly representing a partial melt of the sLL subgroup.

The silicate ureyite (NaCrSi2O6) has been found as a rare occurrence in Toluca (Frondel and Klein, 1965). Further information on the formation of the IAB iron complex can be found on the Caddo County page. The specimen of Toluca shown above and below is a 2003 Harvey Award—"New Technology Award"—which was presented in recognition of the Meteorite Studies website.

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