Fell March 24, 1933
36° 13′ N., 103° 24′ W. At 5:00 on a March morning, ~100 stones totaling 3–4 kg were heard and seen to fall in New Mexico, after putting on a display for observers in New Mexico, Colorado, Kansas, Oklahoma, and as far away as Texas and Wyoming. The fireball left a thick, twisting dust trail, perhaps a mile wide and hundreds of miles long, comprising perhaps thousands of tons of material. Grabbing his Kodak Brownie camera, a rare photo of the actual fireball in flight was taken by the quick-acting Charles M. Brown as it spiralled towards Earth (see below), and other images of the remnant twisted dust cloud were captured. Information was recorded in a note by Harvey Nininger describing the scene as photographed by Charles Brown: Great meteor of Mar. 24 1933. Photo by Chas. M. Brown and copyrighted by him. Nininger survey demonstrated that meteor was visible for 15 to 22 seconds. Cloud remained visible 3 hrs. or more. Diameter of luminous sphere was about 6 miles. Diameter of spiral train was about 1 mile. Meteorites from this fall were strewn along a path of 28 miles having a width of about 2 to 3 miles wide. The fall was in an E.N.E. to W.S.W. direction beginning about 25 mi. W.S.W. from Clayton New Mexico. Meteorites were preserved in America Meteorite Museum, U.S. 66, west of Winslow Arizona. The small stones were collected by ranchers along a distance of 28 miles near the Pasamonte Ranch, and these were subsequently identified as meteorites by Harvey Nininger, who had independently located the strewnfield after spending many months conducting eyewitness interviews.
- Main Group (primary basalt): Mg# ~ 0.38–0.41; Ti ~ 3–4 mg/g
- Stannern trend (primary partial melt): Mg# similar to main series; Ti up to 5.7 mg/g
- Nuevo Laredo trend (fractional crystallization): Mg# extends from Main Group to 0.32; Ti = 5.7 mg/g
A plot of the three subgroups shows a convergence at the center of the Main Group, implying that a genetic relationship (i.e., same parent body) exists among them, and a possible derivation of the two trends from the primary melts of the Main Group. Currently, the Main Group is combined with the Nuevo Laredo Trend to form a single series, while the Stannern Trend represents Main Group magma that has been contaminated by a crustal partial melt.It has been demonstrated that the HED parent body was relatively homogenous in its O-isotopic composition. In a study of a number of eucrites having anomalous O-isotopic ratios and/or anomalous chemical compositions, textures, or ages, evidence was presented indicating that Pasamonte must have originated on a parent body distinct from that of the other HED meteorites (Scott et al., 2008, 2009). For example, its significant displacement from the Eucrite Fractionation Line (EFL)—plotting ~4.7 standard deviations from the eucrite/diogenite mean Δ17O value—cannot be reasonably explained by the admixture of foreign impactor contaminates, by terrestrial weathering processes, or by an isotopically heterogeneous parent body. Pasamonte has a pyroxene Fe/Mn ratio of 29, which is at the lower range (28–40) of typical eucrites. Moreover, its chromites have compositions which are much more Al-rich and Ti-poor than in other eucrites. It is reasonable to assume that Pasamonte was derived from one of many Vesta-sized asteroids that likely existed early in Solar System history, prior to the Late Heavy Bombardment period ~3.5–4.1 b.y. ago. Notably, the paired brecciated, vesiculated basalts PCA 82502 and PCA 91007 have O-isotopic compositions which are virtually identical to Pasamonte (see diagram below), and they have similar anomalously high abundances of certain siderophile elements (Ni, Ir, Os) as well; it could be inferred that they formed in a common nebular region (Scott et al., 2009).
Diagram credit: Mittlefehldt et al., 47th LPSC, #1240 (2016) As presented by Sanborn and Yin (2014) [#2018], a Δ17O vs. ε54Cr diagram is one of the best available diagnostic tools for determining genetic (parent body) relationships among meteorites, constrained by the degree to which isotopic homogenization occurred on their respective parent bodies. Moreover, Sanborn et al. (2015) demonstrated that ε54Cr values are not affected by aqueous alteration. Currently, a number of anomalous eucritic meteorites are known, including Ibitira, Pasamonte, NWA 1240, PCA 82502/91007, Bunburra Rockhole, A-881394, EET 92023, and Emmaville, each of which are resolved from typical eucrites and the HED parent body both isotopically and compositionally; notably, the latter four anomalous eucritic meteorites share close similarities in their O-isotopes and might be genetically related (Barrett et al., 2017; see O-isotopic diagram). However, a high-resolution Δ17O diagram presented by Mittlefehldt et al. (2018) appears to distinguish many of these meteorites from each other, with two couples—Pasamonte with PCA 91007 and Bunburra Rockhole with EET 92023—showing overlapping values (see diagram below). Asuka 881394 is exceptional in having the oldest measured U–Pb age of any achondrite. Employing the precise 238U/235U value of 137.768, 2015), Wimpenny et al. (2019) determined the most precise and accurate Pb–Pb isochron age for A-881394 of 4.56495 (± 0.00053) b.y. By comparison, the ungrouped NWA 11119 (likely related to NWA 7325) has an Al–Mg age relative to D’Orbigny of 4.5648 (± 0.0003) b.y. (Srinivasan et al., 2018).
Diagram credit: Mittlefehldt et al., 49th LPSC, #2700 (2018) Another useful tool to help resolve potential genetic relationships among meteorites is the pyroxene Fe/Mn ratio. While Fe and Mn do experience nebular fractionations, they are not readily fractionated during parent body igneous processing, and therefore different Fe/Mn values are inherent in different parent objects. Mittlefehldt et al. (2017) utilized a number of eucrites and anomalous eucrite meteorites, including A-881394, EET 92023, Ibitira, and Emmaville, to compare the Fe/Mn and Fe/Mg ratios in low-Ca pyroxenes. Consistent with the O-isotopic results, these four meteorites plot in separate locations on an Fe/Mn vs. Fe/Mg coupled diagram, which suggests that they derive from separate parent bodies (see top two diagram below). Moreover, despite the fact that Pasamonte and PCA 82502/91007 are similar with respect to both Δ17O and ε54Cr values (see Sanborn et al., 2016, #2256), these two meteorites are resolved on an Fe/Mn vs. Fe/Mg coupled diagram, which suggests that they derive from separate parent bodies as well (see bottom diagram below).
Diagram adapted from Mittlefehldt et al., 47th LPSC, #1240 (2016)
Diagram credit: Greenwood et al., 48th LPSC, #1194 (2017) It is known that ureilites, generally considered to originate from a common parent body, have a relatively wide degree of variability in Δ17O, but a relatively narrow degree of variability in ε54Cr. By comparison, Sanborn et al. (2014) inferred that the similar degrees of variability that exist among these anomalous eucritic meteorites could likewise reflect a common origin from a single Vesta-like parent body distinct from typical eucrites (see diagram below). Several exceptions to this hypothesis have since been identified including the following: NWA 1240 plots away from the common HED field; PCA 82502/91007 is resolved from the other anomalous eucrites by both O-isotopes and pyroxene Fe/Mn ratio; A-881394 has significantly different oxygen isotopes, Ti/Al and Fe/Mn values, and bulk composition compared to HEDs (Mittlefehldt et al. (2015); and EET 92023 exhibits significant differences in O-isotopes, Cr-isotopes (Sanborn et al., 2016, #2256), and pyroxene composition compared to HEDs and other anomalous achondrites. EET 92023 shares similar O- and Cr-isotopes to A-881394 and Bunburra Rockhole indicating that they each formed within a common isotopic reservoir. Under the hypothesis that Δ17O values serve equally well as a discriminator compared to ε54Cr values, all of these anomalous meteorites could derive from numerous unique parent bodies distinct from Vesta (see diagram below). Furthermore, although Bunburra Rockhole and A-881394 have the same oxygen and chromium isotope compositions, new in-depth analyses of Bunburra Rockhole conducted by Benedix et al. (2017, and references therein) have revealed that these two meteorites have very different textures and mineral chemistries; e.g., Bunburra Rockhole has plagioclase with An87–90, while A-881394 has plagioclase with An98. Based on their results, they consider it likely that these two meteorites also derive from separate parent bodies.
Diagram adapted from Sanborn and Yin, 45th LPSC, #2018 (2014) One more anomalous eucrite-like achondrite, classified as NWA 12338, has joined this disparate group. This unbrecciated basaltic meteorite is geochemically similar to eucrites but has some differences in its texture and mineralogy, and it has O-isotopic values that plot in a distinct space above the HED trend (see diagram below).
Diagram credit: Guo et al., 50th LPSC, #1583 (2019) Because there are now a number of eucrite-like meteorites that are not grouped with normal eucrites for various reasons, it was proposed that the term ‘eucrite’ be used as a description of a rock type rather than to imply an origin on the presumed HED parent body Vesta. The photo above shows a partially fusion-crusted 18.93 g specimen of Pasamonte acquired from the Robert Haag Collection.
The left photo above captures the shock-generated condensation cloud at the moment when a jet breaks the sound barrier. Compare this to the Pasamonte fireball photo on the right. The corkscrew appearance of the dust train attests to the spinning motion of the incoming object over an extended period of time. The photo below shows the persistent dust cloud of the Pasamonte meteorite showing the effects of adiabatic processes.