Description of an aerodynamic levitation apparatus with applications in Earth sciences

Pack, Andreas; Kremer, Katrina; Albrecht, Nina; Simon, Klaus; Kronz, Andreas

doi:10.1186/1467-4866-11-4

Cited by 24 publications

(23 citation statements)

References 44 publications

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“…No loss of Ca or Al--and most likely any other refractory element, All ratios are given as weighted means with 1r standard error. Literature sources: (S) = Shima (1979) i.e., Zr and Hf--was induced by the spherule production process (see also Pack et al 2010).…”

Section: Calcium and Aluminummentioning

confidence: 60%

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Zirconium and hafnium in meteorites

Patzer¹,

Pack²,

Gerdes

2010

Meteorit & Planetary Scien

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Abstract– The ratio of the two refractory trace elements zirconium (Zr) and hafnium (Hf) in meteorites has been proposed to be uniform. The most precise value available is 34.3 ± 0.2 (1σ). It was obtained by isotope dilution ICP‐MS applied to 15 chondrites, most of which were carbonaceous chondrites, and six achondrites. We reinvestigated the case and determined Zr/Hf ratios of a broad spectrum of meteoritic samples via laser ablation ICP‐MS. Our sample suite comprised 29 chondrites and five achondrites. The main objective of the study was two‐fold: we intended to verify the accuracy and precision of a relatively fast and inexpensive sample preparation method combined with expeditious laser ablation ICP‐MS techniques. Furthermore, we were looking into the possibility of systematic fine‐scale Zr/Hf variations among bulk meteoritic matter of different classes. The applied fusion technique together with laser ablation ICP‐MS turned out to be well suited to determine relative refractory trace element abundances. Absolute Zr/Hf ratios yield uncertainties of approximately 4% (1σ). As opposed to the most recent findings, we observed variable Zr/Hf ratios in different meteorites ranging from approximately 28 to approximately 38. Our value for Orgueil (CI1) is 34.0 ± 0.3 (1σ). Including literature data, we propose a solar system value of 34.1 ± 0.3. Our data also suggest that H chondrites tend to exhibit higher Zr/Hf ratios (average of 35.6 ± 0.5 [1σ]) while EL6 chondrites rather show low values (average of 30.8 ± 0.6 [1σ]). In addition to examining Zr/Hf ratios, we also explored the content of refractory major elements in different meteorite groups. Here, we found that EL6 chondrites often show very low Ca/Al ratios. The CI1 value for CaO/Al2O3 is 0.804. EL6 chondrites, however, display ratios as low as approximately 0.3. While the variation in Zr/Hf can be explained by fractional condensation processes in the early solar nebula, the observed low Ca/Al ratios in EL6 chondrites are probably attributable to deficits in oldhamite (CaS).

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Section: Calcium and Aluminummentioning

confidence: 60%

“…Overall, 100 melt spherules were subdivided onto four sample mounts. Further details of the technique are given by Pack et al. (2010).…”

Section: Sample Preparationmentioning

confidence: 99%

Zirconium and hafnium in meteorites

Patzer¹,

Pack²,

Gerdes

2010

Meteorit & Planetary Scien

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“…6). Donaldson (1979); Tsuchiyama et al (1981), Hashimoto (1983); Nagahara and Kushiro (1989); Richter et al (2002); O'Neill and Eggins (2002); Pack et al (2010).…”

Section: Kinetic Evaporation Experimental Techniquesmentioning

confidence: 99%

Thermodynamics of Element Volatility and its Application to Planetary Processes

Sossi

Fegley

2018

Reviews in Mineralogy and Geochemistry

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3) Evaporation on small planetary bodies (section 4.0.) 4) Evaporation during giant impacts (section 4.0.)To constrain the conditions under which these processes occur necessitates thermodynamic data of gaseous-and condensed species. Therefore, a review of our knowledge and lack thereof, is also presented (section 2.0.). Much of our information on thermodynamic quantities of gaseous species comes from spectrometric measurements, undertaken from the 1950s onwards, largely on simple (binary and ternary) systems (e.g., see Brewer 1953;Margrave 1967;Lamoreaux et al. 1987, and section 2.0.). This information is now readily available in compilations of thermodynamic data such as JANAF (Chase 1998) or IVTAN (Glushko et al. 1999). However, the application of these data to more complex, natural geological systems is less straightforward.Instead, for lack of any other comprehensive volatility scale, 50% nebular condensation temperatures, Tc, (Grossman and Larimer 1974;Lodders 2003), which describe the temperature at which half of the abundance of an element is condensed in the solar nebula, are frequently used to discuss elemental volatility in planetary environments. However, these Tc are strictly relevant only at the pressure and temperature conditions of a solar-composition protoplanetary accretion disk (e.g., the solar nebula). Namely, at low total pressures (PT ≲10 -2 bar), solar or close to solar metallicity 2 (i.e., PT ~ PH2 + PH + PHe), oxygen fugacities ~ 6 log bar units below the Iron -Wüstite (IW) buffer (due to the low H2O/H2 ratios, 5 × 10 -4 ; Rubin et al. 1988;Grossman et al., 2008). Boss (1998) and Woolum and Cassen (1999), to give two examples, used astronomical observations to model midplane temperatures in protoplanetary accretion disks in the planet-forming region and found temperatures <1600 K.Petrological observations of Calcium, Al-rich inclusions (CAI) with the highly fractionated group II rare-earth element (REE) pattern 3 (Boynton 1975) indicate they formed by fractional condensation (Boynton 1975;Davis and Grossman 1979) at temperatures between 1676 K, 1463 K, 1296 K at total pressures (PT) of 10 -3 bar, 10 -6 bar, and 10 -9 bar, respectively (Kornacki and Fegley 1986). At total pressures above ≈10 -2 bar, liquids condense in place of solids (Ebel, 2004) and departures from solar composition (e.g., by changes in metallicity or H-loss on a planetary body) lead to condensation temperatures different to those in a solar-composition system (Larimer and Bartholomay 1979; Lodders and Fegley 1999; Schaefer and Fegley 2010). Thus, the complexity of evaporation and condensation reactions are such that, at conditions outside this range, the relevant gas species, their equilibrium partial pressures and mechanisms driving their escape diverge greatly. Potentially powerful tracers of the conditions under which these gas-liquid/solid processes occur are the moderately volatile elements (MVEs), defined as those that condense from a solar composition nebular condensation and evaporation of silicates under post-n...

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“…) and melting using a levitation apparatus (Pack et al . ) have been developed. However, homogeneous glasses are easily obtained for low SiO 2 and fine‐grained rocks (e.g., basalt), but not for SiO 2 ‐rich and/or coarse‐grained rocks (e.g., granitoid; Nehring et al .…”

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confidence: 99%

“…The fusion glass technique has been widely accepted as an alternative to powder pellets for LA-ICP-MS bulk analysis (Fedorowich et al 1993, Eggins 2003. Flux-free fusion techniques to produce glasses from rock powders using tungsten strips (Fedorowich et al 1993), iridium strips (Norman et al 1996, Stoll et al 2008, molybdenum strips (He et al 2016), boron nitride vessels (Zhu et al 2013), platinum capsules (Kurosawa et al 2006), infrared laser heating and melting using a levitation apparatus (Pack et al 2010) have been developed.…”

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confidence: 99%

Comparison of Ultrafine Powder Pellet and Flux‐free Fusion Glass for Bulk Analysis of Granitoids by Laser Ablation‐Inductively Coupled Plasma‐Mass Spectrometry

Karius²,

Schmidt³

et al. 2018

Geostandard Geoanalytic Res

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Two sample preparation techniques (ultrafine powder pellet and flux‐free fusion glass) for LA‐ICP‐MS bulk analysis of granitoids were compared. Ultrafine powder particles produced by wet milling were characterised as d50: ~ 1.0 μm, d90: ~ 5.0 μm. Agate abrasion (balls and vial) during wet milling affects only SiO2 measurements and is negligible for other elements. For the flux‐free fusion glass, a second grinding of the initial fused glass and re‐melting were necessary to produce compositionally homogeneous glasses. Nickel and Cu can be contaminated during the fusion procedure, and Sn and Pb were depleted after the melting process. The homogeneity of fusion glasses was comparable to that of MPI‐DING glasses, while the powder pellets were less homogeneous. This heterogeneity is ascribed to large (up to 10 μm) crystal fragments (e.g., biotite) persisting in powders even after 45 min of milling. For most elements of interest, both preparation techniques give reliable LA‐ICP‐MS results of granitoid reference materials within 10% of the reference values. Thus, we can recommend both techniques to avoid common problems associated with acid dissolution ICP‐MS. For high‐precision measurements (especially Zr, Hf, Th and U), the flux‐free fusion glass technique is a better choice than ultrafine powder pellets.

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Description of an aerodynamic levitation apparatus with applications in Earth sciences

Cited by 24 publications

References 44 publications

Zirconium and hafnium in meteorites

Zirconium and hafnium in meteorites

Thermodynamics of Element Volatility and its Application to Planetary Processes

Comparison of Ultrafine Powder Pellet and Flux‐free Fusion Glass for Bulk Analysis of Granitoids by Laser Ablation‐Inductively Coupled Plasma‐Mass Spectrometry

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