SOUTH BYRON


Iron, ungrouped
ataxite
(eponymous member of the South Byron Trio)

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Found 1915
43° 2' N., 78° 4' W.

A single terrestrially-weathered (surface loss of a few mm) iron meteorite weighing ~6 kg was found west of South Byron, Genesee County, New York. The meteorite was analyzed at the Chicago Field Museum (Nichols and Farrington) and classified as a nickel-rich (17.8%) ataxite.

As described in the Handbook of Iron Meteorites Volume 3 (Vagn F. Buchwald, 1975), shock-melted mm-scale troilite–daubreelite inclusions, sometimes associated with primary chromite grains, are scattered throughout an otherwise homogeneous FeNi-metal matrix. Under high magnification, µm-scale kamacite platelets and associated schreibersite crystals can be resolved forming a micro-Thomson (Widmanstätten) structure. The presence of daubréelite in South Byron and the similar Babb's Mill (Troost's) iron is attributed by Corrigan et al. (2018) to a late-stage reduction process, possibly related to the exhaustion of water utilized in the oxidation of metallic iron to form FeO.

South Byron is grouped with two other irons, Babb's Mill (Troost's) and Inland Forts (ILD) 83500, and these three together have been termed the South Byron Trio (SBT). The existence of a possible genetic link between the SBT and the Milton pallasite has been investigated by numerous investigators (e.g., Jones et al., 2003 [#1683]; Reynolds et al., 2006 [#5233]; McCoy et al., 2017 [#2241], 2019 [GCA]; Corrigan et al., 2017 [#2556]; Corrigan et al., 2018 [#2527]). All of these irons have significant characteristics in common, including similar metal compositions (siderophile element abundance patterns reflecting oxidizing conditions), similar metal structures (kamacite spindles and associated schreibersite), O-isotope values that plot along a consistent trend line, similar Δ17O-isotopic compositions of chromites, and overlapping Mo-isotopic values. The differences in siderophile element and platinum group element abundances that are observed could be attributed to fractional crystallization processes, or as Hilton et al. (2019) have inferred, to formation on separate parent bodies that accreted from similar precursor materials in a similar isotopic region (CC) of the protoplanetary disk (see respective diagrams below).

Siderophile Element Concentrations for SBT and Milton
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click on image for a magnified view (V, Cr, and Mn not included)

Diagram credit: McCoy et al., 48th LPSC, #2241 (2017)

Oxygen Isotopes for SBT and Milton
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Diagram credit: McCoy et al., 48th LPSC, #2241 (2017)

Oxygen Isotopic Composition of Chromites for SBT and Milton
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Diagram credit: McCoy et al., GCA, vol. 259 (2019)
'The Milton pallasite and South Byron Trio Irons: Evidence for oxidation and core crystallization'
(https://doi.org/10.1016/j.gca.2019.06.005)

Molybdenum Isotopes for SBT and Milton
(µ notation denotes deviation from terrestrial standards in parts per million)
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Diagram credit: Hilton et al., 49th LPSC, #1186 (2018)

HSE Abundances for SBT and Milton
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Diagram credit: Hilton et al., GCA, vol. 251, pp. 217–228 (2019)
'Genetics, crystallization sequence, and age of the South Byron Trio iron meteorites:
New insights to carbonaceous chondrite (CC) type parent bodies'
(https://doi.org/10.1016/j.gca.2019.02.035)

Investigators have explored the possibility of a genetic relationship between IVB irons and other meteorite groups including the South Byron Trio. Based on O-isotopic analyses utilizing chromite grains from the IVB irons Warburton Range and Hoba, Corrigan et al. (2017) found that IVB irons plot close to the Milton–South Byron trio grouping (MSB in diagram below). The O-isotopic compositions of the IVB irons and the MSB grouping also fall within the range of the oxidized CV–CK chondrites. Moreover, Corrigan and McCoy (2018) found that both IVB irons and the MSB grouping show evidence for early oxidation (e.g., both have a similar high Ni content of ~15.5–18 wt% and ~15–18 wt%, respectively), as well as evidence for late reduction (e.g., both contain reduced mineral phases such as troilite, daubréelite, and schreibersite).

standby for o-isotopic relationship between groups diagram
Diagram credit: Corrigan et al., 48h LPSC, #2556 (2017)
Hoba: Δ17O = –3.4 [±0.2] ‰
Warburton Range: Δ17O = –3.4 [±0.4] ‰
Milton–South Byron trio: Δ17O = ~ –3.6 [±0.6] ‰

Further comparative studies of Milton, the South Byron Trio, and IVB irons were published by McCoy et al., 2019). Despite the fact that these meteorites have similarities in their Δ17O values, metallography, and HSE enrichments, the significantly higher depletion of volatile siderophiles among the IVB irons was attributed to parent body devolatilization subsequent to removal of the silicate shell. For such a degassing process to occur unimpeded, core crystallization on the IVB parent body would have proceeded from the center outwards. This is consistent with observations in which the earliest crystallizing, low-Ni irons have the slowest cooling rates due to core–outward crystallization. In contrast, they determined that the Milton–SBT parent body was stripped of its silicate shell prior to crystallization, with rapid cooling and solidification starting at the core–mantle boundary and then proceeding inward in the following sequence: Milton ⇒ South Byron and Babb's Mill (very early solidification) ⇒ ILD 83500 (at ~40% solidification); this crystallization sequence would have prevented a similar volatile degassing process as hypothesized for the IVB parent body (McCoy et al., 2019).

Given a scenario in which the SBT and Milton derive from a common parent body, it was recognized by McCoy et al. (2017, 2019) and others that the inferred sequence of crystallization would be from the core-mantle boundary inwards. This process would be consistent with the formation of an early core dynamo, evidence for which has been demonstrated through paleomagnetic studies of CV meteorites (e.g., Elkins-Tanton and Weiss, 2009; Weiss et al., 2010; Elkins-Tanton et al., 2011; Carporzen et al., 2010, 2011; Gattacceca et al., 2013, 2016).

The CRE age for South Byron based on K systematics was reported to be 210 (±70) m.y. (Voshage, 1967). Further details about the South Byron Trio and its possible relationship to the Milton pallasite can be found on the Milton page. The specimen of South Byron shown above is a 4.5 g polished part slice originally acquired by a fellow collector from the Impactika Meteorite Collection of Anne Black.