Ingo Leya's research while affiliated with Planetary Science Institute and other places

... Based on our data (Fig. 1) (Greenwood et al., 2017;Torrano et al., 2021) and Meteoritical Bulletin, e 54 Cr (Qin et al., 2010a;Trinquier et al., 2007;Zhu et al., 2019b;Zhu et al., 2021a;Zhu et al., 2021b;Zhu et al., 2021c;Zhu et al., 2020b;Zhu et al., 2022), e 50 Ti (Torrano et al., 2021;Trinquier et al., 2009;Zhang et al., 2012) and e 48 Ca (Dauphas et al., 2014;Schiller et al., 2018;Schiller et al., 2015b). Note: we use grey circles to represent the e 48 Ca data of CO chondrites in Dauphas et al. (2014), due to the relatively large data uncertainty of the TIMS measurements. ...

... Fine-grained troilite and chromite distribute pervasively in the orthopyroxene crystals (Figure 1a), indicating that the orthopyroxenetroilite-chromite symplectite-like intergrowth probably formed simultaneously. Such a symplectite-like structure has been previously found in various meteorite groups, including acapulcoites (El Goresy et al., 2005), brachinites (Goodrich et al., 2011(Goodrich et al., , 2017Irving et al., 2013;Rumble et al., 2008), ungrouped achondrites (Petaev & Brearley, 1994), HEDs (Patzer & McSween, 2012;Zhang et al., 2018Zhang et al., , 2020, mesosiderites (Lorenz et al., 2010;Ruzicka et al., 1994), Apollo lunar sample (Lindstrom & Salpas, 1983;Norman, 1981), and ordinary chondrites (Li et al., 2021). ...

... This demonstrates that the model of Leya and Masarik (2009) cannot be directly applied to compute CRE exposure ages of HEDs, most likely due to marked differences in the matrix effects. The next generation of model calculations for cosmogenic production rates in planetary objects has been recently developed (Leya et al., 2021a) and will be soon applied to achondrites (Leya et al., 2021b), making it possible, for the first time, to apply model calculations for cosmogenic production rates in HEDs. Due to the high C-content (∼2 wt% on average and up to 7 wt%; Downes et al., 2015;Grady et al., 1985;Vdovykin, 1970) and moderate Fe abundance of ureilites, the physical model of cosmogenic nuclide production in carbonaceous chondrites constitutes a more reasonable approximation for the matrix effects in ureilites (Leya & Stephenson, 2019;Meier et al., 2012;Riebe et al., 2017;Welten et al., 2010). ...

... However, few desert meteorites have been collected until the discovery of two LL5 ordinary chondrites in Alaer area, Xinjiang, in 2007, which were named Alaer 001 and Alaer 002 (Weisberg et al., 2010). Thereafter, an increasing number of studies on desert meteorites in China were reported (Du et al., 2021;Li & Hsu, 2014;Li et al., 2017Li et al., , 2021Zeng et al., 2018). Four meteorite dense collection areas (Xingdi, Argan, Loulan Yizhi, and Lop Nur) in the east of the Taklamakan Desert have been reported by Li and Hsu (2014). ...

... The abundance and isotopic ratios of noble gases were measured at the Institute of Geology and Geophysics, Chinese Academy of Sciences (Beijing, China), using a multicollector Noblesse mass spectrometer from Nu Instruments. The technical details of Noblesse mass spectrometer and measurement procedures have been given in some of the previous studies [25][26][27][28][29]. Briefly, samples of Clast1 (3.76 mg), Clast2 (0.87 mg), Clast3 (0.94 mg), Matrix (2.33 mg), and Bulk (2.30 mg) were loaded into a laser sample chamber and preheated in vacuum at 120 • C for 3 days to remove absorbed atmospheric noble gases. ...

... Laser-induced fluorescence making use of a capillary electrophoresis microfluidic suite could reach the 1-100 picomolar limit of detection, well below our proposed threshold (Skelley et al. 2005;Creamer et al. 2017;Mathies et al. 2017;Casto-Boggess et al. 2021). Alternatively, mass-spectrometry-based methods of detection and analysis might also reach our proposed threshold (Ligterink et al. 2020). To conclude, while it might be hard to interpret a measure of [Gly] > 2 × 10 −7 mol L −1 unless organics enhancement (such as bubble scrubbing) can be confidently constrained, it seems quite feasible to reach sufficiently high detection capability (less than 2 × 10 −7 mol L −1 ) for which the probability of false negatives is low. ...

... Thus, the K, Cu, and Zn isotopic compositions show coupled elemental depletions and isotopic enrichments in planetary materials such as lunar samples, relative to CI chondrites. Similar trends are also seen in other volatile elements such as Cl, Rb, Se, Ga, and Sn (e.g., Sharp et al., 2010;Kato and Moynier, 2017;Pringle and Moynier, 2017;Wang et al., 2019;Nie and Dauphas, 2019;Vollstaedt et al., 2020). Fig. 1 summarizes current knowledge on the K, Cu, and Zn isotopic compositions for planetary bodies and materials. ...

... ± 0.030) x 10 -12 , SMD-Al-11 with 26 Al/ 27 Al = (9.66 ± 0.14) x 10 -12 , SMD-Ca-11 with 41 Ca/ 40 Ca = (9.944 ± 0.092) x 10 -12 , and inhouse 60 Fe/Fe material (known to ~10%), which is based on material provided by the TU Munich and on material from recent meteorite studies (Leya et al., 2020). They had been previously cross-calibrated against material from PSI with a well-known 60 Fe/Fe ratio of (1.234 ± 0.007) x 10 -12 (Schumann et al., 2019). ...

... Figures S1 to S3 Tables S1 to S5 Data file S1 (20,22,53), updated with recent publications (9,23,42,47,52,(54)(55)(56)(57)(58)(59)(60)(61)(62). ...

... This strongly suggests that mass-dependent fractionation dominates over mixing with stratospheric oxygen, even once particles achieve a molten state. (Zhang et al., 2020b) and spinels in aqueously altered FgMMs (Kurat et al., 1994a;Hoppe et al., 1995;Engrand et al., 1999) are shown. N.G. ...