Physical characterization of a suite of Buzzard Coulee H4 chondrite fragments

Fry, Christopher S.; Melanson, Denis; Samson, C.; McCausland, P. J. A.; Herd, R. K.; Ernst, Richard E.; Umoh, J.; Holdsworth, David W.

doi:10.1111/maps.12130

Cited by 11 publications

(7 citation statements)

References 21 publications

(28 reference statements)

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“…Further evidence for homogenization is seen among the physical properties of Buzzard Coulee as corresponding measurements were found to have low variation coefficients (Fry et al. ). Buzzard Coulee is clearly an anomalous type‐4 EOC that is homogenous on the scale of cm.…”

Section: Resultsmentioning

confidence: 99%

In situ analysis of platinum group elements in equilibrated ordinary chondrite kamacite and taenite

Gilmour

Herd

2020

Meteorit & Planetary Scien

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Platinum group element (PGE) concentrations have been determined in situ in ordinary chondrite kamacite and taenite grains via laser ablation inductively coupled plasma mass spectrometry (LA-ICP-MS). Results demonstrate that PGE concentrations in ordinary chondrite metal (kamacite and taenite) are similar among the three ordinary chondrite groups, in contrast to previous bulk metal studies in which PGE concentrations vary in the order H < L < LL. PGE concentrations are higher in taenite than kamacite, consistent with preferential PGE partitioning into taenite. PGE concentrations vary between and within metal grains, although average concentrations in kamacite broadly agree with results from bulk studies. The variability of PGE concentrations in metal decreases with increasing petrologic type; however, variability is still evident in most type six ordinary chondrites, suggesting that equilibration of PGEs does not occur between metal grains, but rather within individual metal grains via self-diffusion during metamorphism. The constant average PGE concentrations within metal grains across different ordinary chondrite groups are consistent with the formation of metal via nebular condensation prior to the accretion of ordinary chondrite parent bodies. Post-condensation effects, including heating during chondrule-formation events, may have affected some element ratios, but have not significantly affected average metal PGE concentrations. H chondrites Buzzard*Specimens provided by the Smithsonian National Museum of Natural History. All other specimens are from the University of Alberta Meteorite Collection. Provided with the meteorite name is its classification and specimen number.

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Section: Resultsmentioning

confidence: 99%

In situ analysis of platinum group elements in equilibrated ordinary chondrite kamacite and taenite

Gilmour

Herd

2020

Meteorit & Planetary Scien

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“…; Fry et al. ), including frozen pristine fragments of the Tagish Lake meteorite (Ralchenko et al. ), tektites (Fry et al.…”

Section: Introductionmentioning

confidence: 99%

Iron meteorite bulk densities determined via 3‐D laser imaging

Fry

Samson

McCausland

et al. 2018

Meteorit & Planetary Scien

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This study tested the feasibility of using 3‐D laser imaging to measure the bulk density of iron meteorites. 3‐D laser imaging is a technique in which a 3‐D model of an object is built after aligning and merging individual detailed images of its surface. Assuming that the mass of the object is known, the volume of the model is calculated by software and an estimate of bulk density can be obtained by dividing mass by volume. The 3‐D laser imaging technique was used to determine the density of 46 fragments from 11 different iron meteorites. The technique proved to be robust and was applied successfully to study samples ranging close to four orders of magnitude in mass (8 g to 156 kg) and exhibiting a variety of surface textures (e.g., cracks, regmaglypts), reflectivities (e.g., polished surfaces, fusion crust, rust), and morphologies (e.g., sharp angular edges, shrapnel tendrils). Three metrics were considered to estimate the error associated with density measurements: the range accuracy of the laser camera, image alignment error, and inter‐operator variability during model building. Inter‐operator variability was the largest source of error and was highest when assembling models of samples which either lacked distinctive features or were very complex in shape. Excluding two anomalous Zagora samples where silicate inclusions might have lowered density, the densities measured using 3‐D laser imaging ranged from 6.98 to 7.93 g cm−3, consistent with previous studies. There is overlap between bulk density and iron meteorite class, and therefore bulk density cannot be used in isolation as a classification criterion. It is a good indicator, however, of weathering effects and of the potential presence of low‐density inclusions.

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“…The principles and procedure of this method are fully described in Section 2.1. The technique is easily scalable for a range of sizes, and has produced results that are consistent with other methods (Smith et al 2006b;McCausland et al, 2011;Fry et al, 2013a). There is a significant time commitment with this method, at least 2-3 hours, to achieve a single measurement.…”

Section: 32: Measuring Densitymentioning

confidence: 53%

“…There is now a database of 18 stony meteorites (Fry et al, 2013), 28 iron meteorites (this study), and 9 tektites (this study) for which a comparison between the two density measurement methods can be done (in all these cases, the same laser camera (VIVID 9i noncontact 3D digitizer) was used). This includes the results presented in this thesis and those of Fry et al (2013a).The average coefficient of correlation between both methods is 1.07% for the stony meteorites and 2.79% for iron meteorites. For tektites, the coefficient of correlation is much higher, at 3.73%, even when excluding outliers.…”

Section: Dmentioning

confidence: 73%

“…P-and S-wave velocity, Poisson's ratio), to name a few. The measurement of physical properties has been extended from terrestrial material to astromaterial, such as meteorites, for density (Consolmagno and Britt, 1998;Smith et al, 2006b;Macke et al, 2010), magnetic properties (bulk susceptibility, frequency dependence, degree and shape of anisotropy) (Rochette et al, 2003;Smith et al, 2006a), porosity (Consolmagno et al, 1998;Wilkison et al, 2003;Fry et al, 2013a;Ralchenko, 2013), and thermal conductivity (Consolmagno et al, 2013).…”

Section: 31: Introduction To Physical Propertiesmentioning

confidence: 99%

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3D Laser Imaging and Modeling of Iron Meteorites and Tektites

Fry¹

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3D laser imaging is a non-destructive method devised to calculate bulk density by creating volumetrically accurate computer models of hand samples. The focus of this research was to streamline the imaging process and to mitigate any potential errors. 3D laser imaging captured with great detail (30 voxel/mm 2 ) surficial features of the samples, such as regmaglypts, pits and cut faces. Densities from 41 iron meteorites and 9 splash-form Australasian tektites are reported here. The laser-derived densities of iron meteorites range from 6.98 to 7.93 g/cm 3 .Several suites of meteorites were studied and are somewhat heterogeneous based on an average 2.7% variation in inter-fragment density. Density decreases with terrestrial age due to weathering. The tektites have an average laser-derived density of 2.41+0.11g/cm 3 . For comparison purposes, the Archimedean bead method was also used to determine density. This method was more effective for tektites than for iron meteorites.iii Acknowledgements

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Physical characterization of a suite of Buzzard Coulee H4 chondrite fragments

Cited by 11 publications

References 21 publications

In situ analysis of platinum group elements in equilibrated ordinary chondrite kamacite and taenite

In situ analysis of platinum group elements in equilibrated ordinary chondrite kamacite and taenite

Iron meteorite bulk densities determined via 3‐D laser imaging

3D Laser Imaging and Modeling of Iron Meteorites and Tektites

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