ARISPE


Iron, IC, octahedrite
High Re, Os, and Ir subgroup
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Found 1896
30° 20' N., 109° 59' W.

Two masses of 116 pounds and 20 pounds were found about 25 miles NW of Arispe, Sonora, Mexico. In 1898, another mass weighing 272 pounds was discovered 15 miles NW of Arispe and was sectioned and distributed to several museums. In the years following, many more masses were recovered along a 12-mile line from Mount San Antonio to Arispe. At least sixteen individuals with a total weight of over 1,500 pounds show that the Arispe shower was a significant one.

Arispe is a polycrystalline iron meteorite with distinctly oriented austenite crystals up to 25 cm in diameter. Troilite inclusions occur throughout, enveloped by schreibersite. The compositional trends are most consistent with formation from a residue of equilibrium partial melting. While distantly related to group IA irons, its lower Ni content of 6.1%–6.8% led to the establishment of a new group, IC. A unique feature present among group IC members is the occurrence of abundant cohenite and other carbon inclusions. Due to a high iridium content, Arispe is considered an anomalous member of the diverse IC group.

Radioisotope chronometry indicates an unusually long terrestrial age for the Arispe masses of 240,000 (±50,000) years. Based on corrected Hf–W isotope systematics, Kruijer et al. (2017) calculated the model age for core formation on the IC iron parent body at 0.3 (±0.5) m.y. after CAIs. This age overlaps within uncertainty the time of CAI formation and is the earliest differentiation, and thus the earliest accretion, of any parent body studied to date. Tornabene et al. (2021 #1531) revealed that isotopic data for most IC irons support a Re–Os isochron age of 4.57 b.y., which substantiates such an early accretion of the parent body.

W Isotope Dichotomy and Age Relative to CAIs
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Diagrams credit: Kruijer et al., PNAS, vol. 114, #26, p. 6713 (2017 open access link)
'Age of Jupiter inferred from the distinct genetics and formation times of meteorites'
(http://dx.doi.org/10.1073/pnas.1704461114)

Highly siderophile element (HSE) data was obtained by Tornabene et al. (2020 #2391) for each of the IC irons. In addition, W and Mo isotopic data was acquired by Tornabene et al. (2021 #1531). It was demonstrated that the members of this group are related through varying degrees of fractional crystallization from a common parental melt, with Arispe being the first to crystallize after ~7% fractional crystallization (see #1531 for the fractionation/mixing scenario of other IC members; see also the Santa Rosa page). Based on the disparate HSE data, µ182W isotope values, and µ94,95,97Mo isotope values obtained for the two anomalous IC irons, Nocoleche and Winburg, Tornabene et al. (2021) contend that these two meteorites are not members of the IC group and should be reclassified as ungrouped irons.

Tornabene et al. (2020, 2021) further determined that IC irons can be divided into two subgroups according to whether they have high or low abundances of Re, Os, and Ir (see diagrams below). It was proposed by Tornabene et al. (2020, 2021 and references therein) that the two subgroups represent mixing between solids and liquids in various stages of evolution following a severe collision. The "high abundance" subgroup could represent mixtures of contemporaneously evolved solids and liquids, while the "low abundance" subgroup could represent mixtures of early-formed solids (after ~1% crystallization) and more evolved liquids persisting after ~13% fractional crystallization, with the assumption that these meteorites are composed of >99% evolved liquid component.

Highly Siderophile Element Data for IC Iron Subgroups
High abundance subgroup: Arispe, Union County, Mount Dooling
Low abundance subgroup: Bendego, Chihuahua City, NWA 2743, St. Francois County, Santa Rosa

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Diagrams credit: Tornabene et al., 51st LPSC, #2391 (2020)

To learn more about the relationship between this and other iron chemical groups, click here. The specimen of Arispe shown above is a 39.6 g etched partial slice. A photo of the complete 1898 mass weighing 272 pounds is shown below.

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