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Journal articles on the topic 'Volatile elements'

Author: Grafiati

Published: 4 June 2021

Last updated: 25 May 2024

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1

Day, James M. D., and Frederic Moynier. "Evaporative fractionation of volatile stable isotopes and their bearing on the origin of the Moon." Philosophical Transactions of the Royal Society A: Mathematical, Physical and Engineering Sciences 372, no. 2024 (September 13, 2014): 20130259. http://dx.doi.org/10.1098/rsta.2013.0259.

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The Moon is depleted in volatile elements relative to the Earth and Mars. Low abundances of volatile elements, fractionated stable isotope ratios of S, Cl, K and Zn, high μ ( 238 U/ 204 Pb) and long-term Rb/Sr depletion are distinguishing features of the Moon, relative to the Earth. These geochemical characteristics indicate both inheritance of volatile-depleted materials that formed the Moon and planets and subsequent evaporative loss of volatile elements that occurred during lunar formation and differentiation. Models of volatile loss through localized eruptive degassing are not consistent with the available S, Cl, Zn and K isotopes and abundance data for the Moon. The most probable cause of volatile depletion is global-scale evaporation resulting from a giant impact or a magma ocean phase where inefficient volatile loss during magmatic convection led to the present distribution of volatile elements within mantle and crustal reservoirs. Problems exist for models of planetary volatile depletion following giant impact. Most critically, in this model, the volatile loss requires preferential delivery and retention of late-accreted volatiles to the Earth compared with the Moon. Different proportions of late-accreted mass are computed to explain present-day distributions of volatile and moderately volatile elements (e.g. Pb, Zn; 5 to >10%) relative to highly siderophile elements (approx. 0.5%) for the Earth. Models of early magma ocean phases may be more effective in explaining the volatile loss. Basaltic materials (e.g. eucrites and angrites) from highly differentiated airless asteroids are volatile-depleted, like the Moon, whereas the Earth and Mars have proportionally greater volatile contents. Parent-body size and the existence of early atmospheres are therefore likely to represent fundamental controls on planetary volatile retention or loss.

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Day, James M. D., Frédéric Moynier, and Charles K. Shearer. "Late-stage magmatic outgassing from a volatile-depleted Moon." Proceedings of the National Academy of Sciences 114, no. 36 (August 21, 2017): 9547–51. http://dx.doi.org/10.1073/pnas.1708236114.

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The abundance of volatile elements and compounds, such as zinc, potassium, chlorine, and water, provide key evidence for how Earth and the Moon formed and evolved. Currently, evidence exists for a Moon depleted in volatile elements, as well as reservoirs within the Moon with volatile abundances like Earth’s depleted upper mantle. Volatile depletion is consistent with catastrophic formation, such as a giant impact, whereas a Moon with Earth-like volatile abundances suggests preservation of these volatiles, or addition through late accretion. We show, using the “Rusty Rock” impact melt breccia, 66095, that volatile enrichment on the lunar surface occurred through vapor condensation. Isotopically light Zn (δ66Zn = −13.7‰), heavy Cl (δ37Cl = +15‰), and high U/Pb supports the origin of condensates from a volatile-poor internal source formed during thermomagmatic evolution of the Moon, with long-term depletion in incompatible Cl and Pb, and lesser depletion of more-compatible Zn. Leaching experiments on mare basalt 14053 demonstrate that isotopically light Zn condensates also occur on some mare basalts after their crystallization, confirming a volatile-depleted lunar interior source with homogeneous δ66Zn ≈ +1.4‰. Our results show that much of the lunar interior must be significantly depleted in volatile elements and compounds and that volatile-rich rocks on the lunar surface formed through vapor condensation. Volatiles detected by remote sensing on the surface of the Moon likely have a partially condensate origin from its interior.

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3

Tian, Zhen, Tomáš Magna, James M. D. Day, Klaus Mezger, Erik E. Scherer, Katharina Lodders, Remco C. Hin, Piers Koefoed, Hannah Bloom, and Kun Wang. "Potassium isotope composition of Mars reveals a mechanism of planetary volatile retention." Proceedings of the National Academy of Sciences 118, no. 39 (September 20, 2021): e2101155118. http://dx.doi.org/10.1073/pnas.2101155118.

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The abundances of water and highly to moderately volatile elements in planets are considered critical to mantle convection, surface evolution processes, and habitability. From the first flyby space probes to the more recent “Perseverance” and “Tianwen-1” missions, “follow the water,” and, more broadly, “volatiles,” has been one of the key themes of martian exploration. Ratios of volatiles relative to refractory elements (e.g., K/Th, Rb/Sr) are consistent with a higher volatile content for Mars than for Earth, despite the contrasting present-day surface conditions of those bodies. This study presents K isotope data from a spectrum of martian lithologies as an isotopic tracer for comparing the inventories of highly and moderately volatile elements and compounds of planetary bodies. Here, we show that meteorites from Mars have systematically heavier K isotopic compositions than the bulk silicate Earth, implying a greater loss of K from Mars than from Earth. The average “bulk silicate” δ41K values of Earth, Moon, Mars, and the asteroid 4-Vesta correlate with surface gravity, the Mn/Na “volatility” ratio, and most notably, bulk planet H2O abundance. These relationships indicate that planetary volatile abundances result from variable volatile loss during accretionary growth in which larger mass bodies preferentially retain volatile elements over lower mass objects. There is likely a threshold on the size requirements of rocky (exo)planets to retain enough H2O to enable habitability and plate tectonics, with mass exceeding that of Mars.

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4

Baker, D. R., and J. Stix. "Volatile elements in magmatic systems." Eos, Transactions American Geophysical Union 73, no. 46 (1992): 493. http://dx.doi.org/10.1029/91eo00364.

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5

Wang, Ming-Sheng, and Michael E. Lipschutz. "Volatile trace elements in Antarctic ureilites." Meteoritics 30, no. 3 (May 1995): 319–24. http://dx.doi.org/10.1111/j.1945-5100.1995.tb01130.x.

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6

Mahan, Brandon, Frédéric Moynier, Julien Siebert, Bleuenn Gueguen, Arnaud Agranier, Emily A. Pringle, Jean Bollard, James N. Connelly, and Martin Bizzarro. "Volatile element evolution of chondrules through time." Proceedings of the National Academy of Sciences 115, no. 34 (August 6, 2018): 8547–52. http://dx.doi.org/10.1073/pnas.1807263115.

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Chondrites and their main components, chondrules, are our guides into the evolution of the Solar System. Investigating the history of chondrules, including their volatile element history and the prevailing conditions of their formation, has implications not only for the understanding of chondrule formation and evolution but for that of larger bodies such as the terrestrial planets. Here we have determined the bulk chemical composition—rare earth, refractory, main group, and volatile element contents—of a suite of chondrules previously dated using the Pb−Pb system. The volatile element contents of chondrules increase with time from ∼1 My after Solar System formation, likely the result of mixing with a volatile-enriched component during chondrule recycling. Variations in the Mn/Na ratios signify changes in redox conditions over time, suggestive of decoupled oxygen and volatile element fugacities, and indicating a decrease in oxygen fugacity and a relative increase in the fugacities of in-fluxing volatiles with time. Within the context of terrestrial planet formation via pebble accretion, these observations corroborate the early formation of Mars under relatively oxidizing conditions and the protracted growth of Earth under more reducing conditions, and further suggest that water and volatile elements in the inner Solar System may not have arrived pairwise.

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7

Marty, Bernard. "Origins and Early Evolution of the Atmosphere and the Oceans." Geochemical Perspectives 9, no. 2 (October 2020): 135–313. http://dx.doi.org/10.7185/geochempersp.9.2.

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My journey in science began with the study of volcanic gases, sparking an interest in the origin, and ultimate fate, of the volatile elements in the interior of our planet. How did these elements, so crucial to life and our surface environment, come to be sequestered within the deepest regions of the Earth, and what can they tell us about the processes occurring there? My approach has been to establish geochemical links between the noble gases, physical tracers par excellence, with major volatile elements of environmental importance, such as water, carbon and nitrogen, in mantle-derived rocks and gases. From these analyses we have learned that the Earth is relatively depleted in volatile elements when compared to its potential cosmochemical ancestors (e.g., ~2 ppm nitrogen compared to several hundreds of ppm in primitive meteorites) and that natural fluxes of carbon are two orders of magnitude lower than those emitted by current anthropogenic activity. Further insights into the origin of terrestrial volatiles have come from space missions that documented the composition of the proto-solar nebula and the outer solar system. The consensus behind the origin of the atmosphere and the oceans is evolving constantly, although recently a general picture has started to emerge. At the dawn of the solar system, the volatile-forming elements (H, C, N, noble gases) that form the majority of our atmosphere and oceans were trapped in solid dusty phases (mostly in ice beyond the snowline and organics everywhere). These phases condensed from the proto-solar nebula gas, and/or were inherited from the interstellar medium. These accreted together within the next few million years to form the first planetesimals, some of which underwent differentiation very early on. The isotopic signatures of volatiles were also fixed very early and may even have preceded the first episodes of condensation and accretion. Throughout the accretion of the Earth, volatile elements were delivered by material from both the inner (dry, volatile-poor) and outer (volatile-rich) solar system. This delivery was concomitant with the metals and silicates that form the bulk of the planet. The contribution of bodies that formed in the far outer solar system, a region now populated by comets, is likely to have been very limited. In that sense, volatile elements were contributed continuously throughout Earth’s accretion from inner solar system reservoirs, which also provided the silicates and metal building blocks of the inner planets. Following accretion, it likely took a few hundred million years for the Earth’s atmosphere and oceans to stabilise. Luckily, we have been able to access a compositional record of the early atmosphere and oceans through the analysis of palaeo-atmospheric fluids trapped in Archean hydrothermal quartz. From these analyses, it appears that the surface reservoirs of the Earth evolved due to interactions between the early Sun and the top of the atmosphere, as well as the development of an early biosphere that progressively altered its chemistry.

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8

Ming-sheng, Wang, Rick L. Paul, and Michael E. Lipschutz. "Volatile/mobile trace elements in Bholghati howardite." Geochimica et Cosmochimica Acta 54, no. 8 (August 1990): 2177–81. http://dx.doi.org/10.1016/0016-7037(90)90043-k.

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9

Steenstra, E. S., C. J. Renggli, J. Berndt, and S. Klemme. "Evaporation of moderately volatile elements from metal and sulfide melts: Implications for volatile element abundances in magmatic iron meteorites." Earth and Planetary Science Letters 622 (November 2023): 118406. http://dx.doi.org/10.1016/j.epsl.2023.118406.

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10

Zhang, Youxue. "Review of melt inclusions in lunar rocks: constraints on melt and mantle composition and magmatic processes." European Journal of Mineralogy 36, no. 1 (January 26, 2024): 123–38. http://dx.doi.org/10.5194/ejm-36-123-2024.

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Abstract. Mineral-hosted melt inclusions provide a window into magmatic processes and pre-eruptive liquid compositions. Because melt inclusions are small (typically < 100 µm), the study of lunar melt inclusions is enabled by advancements of microbeam instrumental techniques. In the 1970s immediately following the Apollo and Luna missions, major and minor oxide concentrations of lunar melt inclusions were measured using electron microprobes. The data were used to understand magma evolution, and they revealed the immiscibility of two silicate liquids in the late stage of lunar magma evolution. More recently, the development of secondary ion mass spectrometry as well as laser ablation–inductively coupled plasma–mass spectrometry has enabled the measurement of key volatile elements and other trace elements in lunar melt inclusions, down to about the 0.1 ppm level. The applications of these instruments have ushered in a new wave of lunar melt inclusion studies. Recent advances have gone hand in hand with improved understanding of post-entrapment loss of volatiles. These studies have provided deep insights into pre-eruptive volatiles in lunar basalts, the abundance of volatiles in the lunar mantle, the isotopic ratios of some volatile elements, and the partition of trace elements between host olivine and melt inclusions. The recent studies of lunar melt inclusions have played a critical role in establishing a new paradigm of a fairly wet Moon with about 100 ppm H2O in the bulk silicate Moon (rather than a “bone-dry” Moon) and have been instrumental in developing an improved understanding of the origin and evolution of the Moon.

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11

Fenske, Myles P., Kristen D. Hewett Hazelton, Andrew K. Hempton, Jae Sung Shim, Breanne M. Yamamoto, Jeffrey A. Riffell, and Takato Imaizumi. "Circadian clock gene LATE ELONGATED HYPOCOTYL directly regulates the timing of floral scent emission in Petunia." Proceedings of the National Academy of Sciences 112, no. 31 (June 29, 2015): 9775–80. http://dx.doi.org/10.1073/pnas.1422875112.

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Flowers present a complex display of signals to attract pollinators, including the emission of floral volatiles. Volatile emission is highly regulated, and many species restrict emissions to specific times of the day. This rhythmic emission of scent is regulated by the circadian clock; however, the mechanisms have remained unknown. In Petunia hybrida, volatile emissions are dominated by products of the floral volatile benzenoid/phenylpropanoid (FVBP) metabolic pathway. Here we demonstrate that the circadian clock gene P. hybrida LATE ELONGATED HYPOCOTYL (LHY; PhLHY) regulates the daily expression patterns of the FVBP pathway genes and floral volatile production. PhLHY expression peaks in the morning, antiphasic to the expression of P. hybrida GIGANTEA (PhGI), the master scent regulator ODORANT1 (ODO1), and many other evening-expressed FVBP genes. Overexpression phenotypes of PhLHY in Arabidopsis caused an arrhythmic clock phenotype, which resembles those of LHY overexpressors. In Petunia, constitutive expression of PhLHY depressed the expression levels of PhGI, ODO1, evening-expressed FVBP pathway genes, and FVBP emission in flowers. Additionally, in the Petunia lines in which PhLHY expression was reduced, the timing of peak expression of PhGI, ODO1, and the FVBP pathway genes advanced to the morning. Moreover, PhLHY protein binds to cis-regulatory elements called evening elements that exist in promoters of ODO1 and other FVBP genes. Thus, our results imply that PhLHY directly sets the timing of floral volatile emission by restricting the expression of ODO1 and other FVBP genes to the evening in Petunia.

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12

Chen, Zuxing, Landry Soh Tamehe, Haiyan Qi, Yuxiang Zhang, Zhigang Zeng, and Mingjiang Cai. "Using Apatite to Track Volatile Evolution in the Shallow Magma Chamber below the Yonaguni Knoll IV Hydrothermal Field in the Southwestern Okinawa Trough." Journal of Marine Science and Engineering 11, no. 3 (March 9, 2023): 583. http://dx.doi.org/10.3390/jmse11030583.

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The Yonaguni Knoll IV is an active seafloor hydrothermal system associated with submarine silicic volcanism located in the “cross back-arc volcanic trail” (CBVT) in the southwestern Okinawa Trough. However, the behavior of volatiles during magmatic differentiation in the shallow silicic magma chamber is unclear. Here, the volatile contents of apatite inclusions trapped in different phenocrysts (orthopyroxene and amphibole) and microphenocrysts in the rhyolite from the Yonaguni Knoll IV hydrothermal field were analyzed by using electron microprobe analysis, which aims to track the behavior of volatiles in the shallow magma chamber. Notably, the ‘texturally constrained’ apatites showed a decreasing trend of XCl/XOH and XF/XCl ratios. Based on the geochemical analyses in combination with thermodynamic modeling, we found that the studied apatites were consistent with the mode of volatile-undersaturated crystallization. Therefore, volatiles were not saturated in the early stage of magmatic differentiation in the shallow rhyolitic magma chamber, and consequently, the metal elements were retained in the rhyolitic melt and partitioned into crystalline magmatic sulfides. Additionally, previous studies suggested that the shallow rhyolitic magma chamber was long-lived and periodically replenished by mafic magma. The injection of volatile-rich and oxidized subduction-related mafic magmas can supply abundant volatiles and dissolve magmatic sulfide in the shallow magma chamber. These processes are important for the later-stage of volatile exsolution, while the forming metal-rich magmatic fluids contribute to the overlying Yonaguni Knoll IV hydrothermal system.

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13

Degruyter, Wim, Andrea Parmigiani, Christian Huber, and Olivier Bachmann. "How do volatiles escape their shallow magmatic hearth?" Philosophical Transactions of the Royal Society A: Mathematical, Physical and Engineering Sciences 377, no. 2139 (January 7, 2019): 20180017. http://dx.doi.org/10.1098/rsta.2018.0017.

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Only a small fraction (approx. 1–20%) of magmas generated in the mantle erupt at the surface. While volcanic eruptions are typically considered as the main exhaust pipes for volatile elements to escape into the atmosphere, the contribution of magma reservoirs crystallizing in the crust is likely to dominate the volatile transfer from depth to the surface. Here, we use multiscale physical modelling to identify and quantify the main mechanisms of gas escape from crystallizing magma bodies. We show that most of the outgassing occurs at intermediate to high crystal fraction, when the system has reached a mature mush state. It is particularly true for shallow volatile-rich systems that tend to exsolve volatiles through second boiling, leading to efficient construction of gas channels as soon as the crystallinity reaches approximately 40–50 vol.%. We, therefore, argue that estimates of volatile budgets based on volcanic activity may be misleading because they tend to significantly underestimate the magmatic volatile flux and can provide biased volatile compositions. Recognition of the compositional signature and volumetric dominance of intrusive outgassing is, therefore, necessary to build robust models of volatile recycling between the mantle and the surface. This article is part of the Theo Murphy meeting issue ‘Magma reservoir architecture and dynamics’.

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14

Remusat, L. "Organic and volatile elements in the solar system." EPJ Web of Conferences 18 (2011): 05002. http://dx.doi.org/10.1051/epjconf/20111805002.

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15

Takeda, Yoichi, Hikaru Taguchi, Kazuo Yoshioka, Osamu Hashimoto, Toshiki Aikawa, and Satoshi Kawanomoto. "Abundances of Volatile Elements in Post-AGB Candidates." Publications of the Astronomical Society of Japan 59, no. 6 (December 25, 2007): 1127–40. http://dx.doi.org/10.1093/pasj/59.6.1127.

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16

WANG, MING-SHENG, JENNIFER A. MOKOS, and MICHAEL E. LIPSCHUTZ. "Martian meteorites: Volatile trace elements and cluster analysis." Meteoritics & Planetary Science 33, no. 4 (July 1998): 671–75. http://dx.doi.org/10.1111/j.1945-5100.1998.tb01672.x.

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17

Štěpánek, B., V. Šestáková, and J. Krištofik. "Doping of GaSb single crystals with volatile elements." Crystal Research and Technology 29, no. 1 (1994): 19–23. http://dx.doi.org/10.1002/crat.2170290106.

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18

Liu, Xuena, Jinghua Guo, Zijing Chen, Kun Xu, and Kang Xu. "Detection of Volatile Compounds and Their Contribution to the Nutritional Quality of Chinese and Japanese Welsh Onions (Allium fistulosum L.)." Horticulturae 10, no. 5 (April 26, 2024): 446. http://dx.doi.org/10.3390/horticulturae10050446.

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Allium vegetables attract attention for their flavor and aroma in Asia, especially in China and Japan. The aim of this experiment was to uncover the differences in the unique flavor compounds of two Welsh onions that are typical cultivars in China and Japan (‘Zhangqiu’ and ‘Tenko’). Chemical methods and solid-phase microextraction–gas chromatography-mass spectrometry were performed to determine the nutritional quality and quantity of volatile compounds of various organs of Welsh onions. The results show that a total of 30, 37, and 28 compounds were detected in the roots, pseudostem, and leaves of ‘Zhangqiu’, respectively, while 21, 27, and 20 compounds were detected in the corresponding organs of ‘Tenko’. The distribution of sulfur compounds in the roots, pseudostem, and leaves of ‘Zhangqiu’ accounted for 72%, 83%, and 26% of the total content, while those of ‘Tenko’ accounted for 55%, 84%, and 57%, respectively. Aldehydes are the second largest class of volatiles in Welsh onions. The distribution of aldehydes in the leaves was notably different: 52% and 27% in ‘Zhangqiu’ and ‘Tenko’, respectively. The contribution of S to the volatile substances was outstanding, and through forward selection, it was found that P, Ca, and Mg contribute to the volatile substances of Welsh onions. The above results indicate that the different genotypes of Welsh onions have various flavors, and mineral elements contribute variously to these flavors. Calcium could be a new topic of interest for our subsequent research on elements and volatiles.

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19

Nunes, Ana R., Ana C. Gonçalves, Edgar Pinto, Filipa Amaro, José D. Flores-Félix, Agostinho Almeida, Paula Guedes de Pinho, Amílcar Falcão, Gilberto Alves, and Luís R. Silva. "Mineral Content and Volatile Profiling of Prunus avium L. (Sweet Cherry) By-Products from Fundão Region (Portugal)." Foods 11, no. 5 (March 4, 2022): 751. http://dx.doi.org/10.3390/foods11050751.

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Large amounts of Prunus avium L. by-products result from sweet cherry production and processing. This work aimed to evaluate the mineral content and volatile profiling of the cherry stems, leaves, and flowers of the Saco cultivar collected from the Fundão region (Portugal). A total of 18 minerals were determined by ICP-MS, namely 8 essential and 10 non-essential elements. Phosphorus (P) was the most abundant mineral, while lithium (Li) was detected in trace amounts. Three different preparations were used in this work to determine volatiles: hydroethanolic extracts, crude extracts, and aqueous infusions. A total of 117 volatile compounds were identified using HS-SPME/GC-MS, distributed among different chemical classes: 31 aldehydes, 14 alcohols, 16 ketones, 30 esters, 4 acids, 4 monoterpenes, 3 norisoprenoids, 4 hydrocarbons, 7 heterocyclics, 1 lactone, 1 phenol, and 2 phenylpropenes. Benzaldehyde, 4-methyl-benzaldehyde, hexanal, lilac aldehyde, and 6-methyl-5-hepten-2-one were the major volatile compounds. Differences in the types of volatiles and their respective amounts in the different extracts were found. This is the first study that describes the mineral and volatile composition of Portuguese sweet cherry by-products, demonstrating that they could have great potential as nutraceutical ingredients and natural flavoring agents to be used in the pharmaceutical, cosmetic, and food industries.

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20

Sarafian, Adam R., Erik H. Hauri, Francis M. McCubbin, Thomas J. Lapen, Eve L. Berger, Sune G. Nielsen, Horst R. Marschall, Glenn A. Gaetani, Kevin Righter, and Emily Sarafian. "Early accretion of water and volatile elements to the inner Solar System: evidence from angrites." Philosophical Transactions of the Royal Society A: Mathematical, Physical and Engineering Sciences 375, no. 2094 (April 17, 2017): 20160209. http://dx.doi.org/10.1098/rsta.2016.0209.

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Inner Solar System bodies are depleted in volatile elements relative to chondrite meteorites, yet the source(s) and mechanism(s) of volatile-element depletion and/or enrichment are poorly constrained. The timing, mechanisms and quantities of volatile elements present in the early inner Solar System have vast implications for diverse processes, from planetary differentiation to the emergence of life. We report major, trace and volatile-element contents of a glass bead derived from the D'Orbigny angrite, the hydrogen isotopic composition of this glass bead and that of coexisting olivine and silicophosphates, and the 207 Pb– 206 Pb age of the silicophosphates, 4568 ± 20 Ma. We use volatile saturation models to demonstrate that the angrite parent body must have been a major body in the early inner Solar System. We further show via mixing calculations that all inner Solar System bodies accreted volatile elements with carbonaceous chondrite H and N isotope signatures extremely early in Solar System history. Only a small portion (if any) of comets and gaseous nebular H species contributed to the volatile content of the inner Solar System bodies. This article is part of the themed issue ‘The origin, history and role of water in the evolution of the inner Solar System’.

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21

Harfoush, A., and S. Sh Soulayman. "Presparking Effect in Spark Source Mass Spectrometry." Zeitschrift für Naturforschung A 47, no. 6 (June 1, 1992): 748–52. http://dx.doi.org/10.1515/zna-1992-0605.

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AbstractThe Relative Sensitivity Factor (RSF) in Spark Source Mass Spectrometry analysis was found to be dependent on the number and duration of previous sparking periods. This dependency becomes very strong when dealing with volatile elements. By statistical analysis of experimental RSF values it was found that there is a linear correlation between In (RSF) of some trace elements and their boiling temperature. This correlation fails when dealing with volatile elements and carbon. It was found that elements with a large diffusion coefficient have a large RSF.

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22

Sturgeon, R. E., S. N. Willie, G. I. Sproule, P. T. Robinson, and S. S. Berman. "Sequestration of volatile element hydrides by platinum group elements for graphite furnace atomic absorption." Spectrochimica Acta Part B: Atomic Spectroscopy 44, no. 7 (January 1989): 667–82. http://dx.doi.org/10.1016/0584-8547(89)80065-5.

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23

Narendranath, S., Netra S. Pillai, Srikar P. Tadepalli, Menelaos Sarantos, K. Vadodariya, A. Sarwade, Radhakrishna V, and A. Tyagi. "Sodium Distribution on the Moon." Astrophysical Journal Letters 937, no. 2 (September 26, 2022): L23. http://dx.doi.org/10.3847/2041-8213/ac905a.

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Abstract The Moon is significantly depleted in volatile elements when compared to Earth, an observation that has resulted in various formation scenarios leading to the loss of volatiles. Sodium is a moderately volatile element that is a lithophile, which can be utilized as a tracer of the volatile history in planetary bodies. It is also well observed in the exosphere of several bodies in our solar system and exoplanetary systems. But lunar surface sodium abundances have so far been measured only in samples brought back to Earth. We report on results from the first effort to provide a global-scale measurement of sodium on the lunar surface using X-ray fluorescent spectra from Chandrayaan-2. A global average of 1.33 ± 0.03 wt% derived here is higher than previously known. Trends in the sodium abundance indicate a long-lived adsorbate component that could explain the higher abundances reported here, which would act as a reservoir that sustains the lunar sodium exosphere.

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24

Palme, H., G. Kurat, B. Spettel, and A. Burghele. "Chemical Composition of an Unusual Xenolith of the Allende Meteorite." Zeitschrift für Naturforschung A 44, no. 10 (October 1, 1989): 1005–14. http://dx.doi.org/10.1515/zna-1989-1012.

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Abstract The chemical composition of an unusual xenolith (All-AF) from the Allende meteorite was determined by neutron activation and x-ray fluorescence analyses. The xenolith is similar in bulk composition to Allende, but has large excesses in some moderately volatile trace elements, such as Na, K, Au, Sb etc. Some of these elements show considerable variations in other components of Allende, suggesting inhomogeneous distribution in Allende. However, elements of higher volatility, such as Zn and Se have concentrations typical of bulk Allende and other type 3 carbonaceous chondrites. Therefore, All-AF must have formed from the same reservoir as bulk Allende.All-AF has uniform grain size and does not, and did never, contain chondrules. The low content of volatile elements, therefore cannot be ascribed to loss of volatiles during the chondrule forming process. It is a characteristic of the Allende reservoir. The chemical composition of related dark inclusions (DIs) in Allende is different from All-AF. Dark inclusions may have formed by separation of fine grained material in the early solar nebula while All-AF resembles bulk Allende material that was never subject to chondrule formation. Both, dark inclusions and All-AF have oxygen isotopic compositions which plot at the upper end of the δ18O vs. δ17O correlation, suggesting extensive oxygen exchange with ambient gas.

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Herrmann, Wolfgang A., Norbert W. Huber, and Thomas Priermeier. "Solvent-Free Volatile Alkoxides of the Alkaline-Earth Elements." Angewandte Chemie International Edition in English 33, no. 1 (January 17, 1994): 105–7. http://dx.doi.org/10.1002/anie.199401051.

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26

Ballof, Jochen, Mia Au, Ermanno Barbero, Katerina Chrysalidis, Christoph E. Düllmann, Valentin Fedosseev, Eduardo Granados, et al. "A cold electron-impact ion source driven by a photo-cathode – New opportunities for the delivery of radioactive molecular beams?" Journal of Physics: Conference Series 2244, no. 1 (April 1, 2022): 012072. http://dx.doi.org/10.1088/1742-6596/2244/1/012072.

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Abstract The thick-target ISOL (Isotope mass Separation OnLine) method provides beams of more than 1000 radionuclides of 74 elements. The method is well established for elements with sufficiently high volatility at ca. 2000 °C. To extract non-volatile elements the formation of a volatile molecule is required. While successful in some cases (e.g. carbon or boron), most of these elements are not yet available as ISOL beam. A variety of volatile carrier molecules has been proposed for all elements produced in the target material, but their probability of survival during the extraction and ionization process is often limited by the high temperatures required for isotope diffusion in the thick targets and for ion source operation. While cold target concepts have already been proposed, the normal mode of operation of the typically used Versatile Arc Discharge Ion Source (VADIS) with a hot cathode is not well suited. Here, we report about first measurements with an electron-impact ion source operated at ambient temperature using electrons that were liberated via the photo-electric effect from a copper cathode.

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Taylor, G. Jeffrey, and Mark A. Wieczorek. "Lunar bulk chemical composition: a post-Gravity Recovery and Interior Laboratory reassessment." Philosophical Transactions of the Royal Society A: Mathematical, Physical and Engineering Sciences 372, no. 2024 (September 13, 2014): 20130242. http://dx.doi.org/10.1098/rsta.2013.0242.

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New estimates of the thickness of the lunar highlands crust based on data from the Gravity Recovery and Interior Laboratory mission, allow us to reassess the abundances of refractory elements in the Moon. Previous estimates of the Moon fall into two distinct groups: earthlike and a 50% enrichment in the Moon compared with the Earth. Revised crustal thicknesses and compositional information from remote sensing and lunar samples indicate that the crust contributes 1.13–1.85 wt% Al 2 O 3 to the bulk Moon abundance. Mare basalt Al 2 O 3 concentrations (8–10 wt%) and Al 2 O 3 partitioning behaviour between melt and pyroxene during partial melting indicate mantle Al 2 O 3 concentration in the range 1.3–3.1 wt%, depending on the relative amounts of pyroxene and olivine. Using crustal and mantle mass fractions, we show that that the Moon and the Earth most likely have the same (within 20%) concentrations of refractory elements. This allows us to use correlations between pairs of refractory and volatile elements to confirm that lunar abundances of moderately volatile elements such as K, Rb and Cs are depleted by 75% in the Moon compared with the Earth and that highly volatile elements, such as Tl and Cd, are depleted by 99%. The earthlike refractory abundances and depleted volatile abundances are strong constraints on lunar formation processes.

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Anazawa, Katsuro, and Minoru Yoshida. "Multivariate analysis of Japanese volcanic rocks: Volatile and major elements." GEOCHEMICAL JOURNAL 30, no. 6 (1996): 355–72. http://dx.doi.org/10.2343/geochemj.30.355.

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Couturier, G., and M. Rappaz. "Effect of volatile elements on porosity formation in solidifying alloys." Modelling and Simulation in Materials Science and Engineering 14, no. 2 (February 15, 2006): 253–71. http://dx.doi.org/10.1088/0965-0393/14/2/009.

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Yinghui, Liu, Zheng Chuguang, and Wang Quanhai. "Speciation of Most Volatile Toxic Trace Elements during Coal Combustion." Developments in Chemical Engineering and Mineral Processing 11, no. 3-4 (May 15, 2008): 381–94. http://dx.doi.org/10.1002/apj.5500110413.

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Ahmadi, L., M. Mirza, and F. Shahmir. "The volatile constituents ofArtemisia marschaliana Sprengel and its secretory elements." Flavour and Fragrance Journal 17, no. 2 (2002): 141–43. http://dx.doi.org/10.1002/ffj.1055.

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Kleine, Thorsten, Theodor Steller, Christoph Burkhardt, and Francis Nimmo. "An inner solar system origin of volatile elements in Mars." Icarus 397 (June 2023): 115519. http://dx.doi.org/10.1016/j.icarus.2023.115519.

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Righter, K. "Volatile element depletion of the Moon—The roles of precursors, post-impact disk dynamics, and core formation." Science Advances 5, no. 1 (January 2019): eaau7658. http://dx.doi.org/10.1126/sciadv.aau7658.

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The compositional and isotopic similarity of Earth’s primitive upper mantle (PUM) and the Moon supports the derivation of the Moon from proto-Earth, but the Moon’s inventory of volatile lithophile elements—Na, K, Rb, and Cs—is lower than Earth’s PUM by factors of 4 to 5. The abundances of 14 other volatile elements exhibit siderophile behavior [volatile siderophile elements (VSEs); i.e., P, As, Cu, Ag, Sb, Ga, Ge, Bi, Pb, Zn, Sn, Cd, In, and Tl] that can be used to evaluate whether the Moon was derived from proto-Earth and if core formation or volatility controlled their depletion. At lunar core formation conditions, As, Sb, Ag, Ge, Bi, and Sn are siderophile, whereas P, Cu, Ga, Pb, Zn, Cd, In, and Tl are weakly siderophile or lithophile. VSEs may help to discriminate between physical and chemical processes that formed the Moon such as low- versus high-energy impacts and gas-melt interactions.

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Burggräf, P., M. Dannapfel, T. Adlon, A. Riegauf, K. Müller, and C. Fölling. "Agile Montage*/Agile assembly – Assembly planning and assembly system as integral elements of factory planning." wt Werkstattstechnik online 109, no. 09 (2019): 622–27. http://dx.doi.org/10.37544/1436-4980-2019-09-8.

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Produzierende Unternehmen intensivieren aufgrund zunehmend volatiler Kundenbedürfnisse die Anwendung agiler Produktentwicklungsansätze. Ziel des Beitrags ist die Einführung eines Konzepts zur Befähigung dieser dynamischen Produktentwicklung in der Montage. Der integrative Lösungsansatz basiert auf der wirtschaftlichen Optimierung des Agilitätsgrades von Montagesystemen sowie dem selektiven Einsatz agiler Methoden in der traditionell plangetriebenen Montageplanung als Teil der Fabrikplanung.   To meet more volatile customer needs, manufacturing companies increasingly make use of agile product development approaches. This article aims to introduce a concept to enable for dynamic product development in assembly. This integrative solution approach is based on the economic optimization of the degree of agility of assembly systems and on the selective use of agile methods in traditional, plan-driven assembly planning as part of factory planning.

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S., Haroon Rasheed, and Rajeev Pankaj Nelapati. "Low-power and area-efficient memristor based non-volatile D latch and flip-flop: Design and analysis." PLOS ONE 19, no. 3 (March 7, 2024): e0300073. http://dx.doi.org/10.1371/journal.pone.0300073.

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In recent years, non-volatile memory elements have become highly appealing for memory applications to implement a new class of storage memory that could replace flash memories in sequential logic applications, with features such as compactness, low power, fast processing speed, high endurance, and retention. The memristor is one such non-volatile element that fits the fundamental blocks of sequential logic circuits, the latch and flip-flop; hence, in this article, a non-volatile latch architecture using memristor ratioed logic (MRL) inverter and CMOS components is focused, with an additional memristor as a memory element. A Verilog-A model was used to create the memristor element. The simulation findings validated the compact, low-voltage, and reliable design of the latch design. We evolved in technology enough to create a master-slave flip-flop and arrange it to function as a counter and a shift register. Power, number of elements, cell size, energy, programming time, and robustness are compared to comparable non-volatile topologies. The proposed non-volatile latch proves non-volatility and can store data with a 24% reduction in power consumption and a near 10% reduction in area.

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Flynn, G. J., S. Bajt, S. R. Sutton, M. E. Zolensky, K. L. Thomas, and L. P. Keller. "The Abundance Pattern of Elements Having Low Nebular Condensation Temperatures in Interplanetary Dust Particles: Evidence for a New Chemical Type of Chondritic Material." International Astronomical Union Colloquium 150 (1996): 291–94. http://dx.doi.org/10.1017/s0252921100501717.

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AbstractThe abundances of Ni, Fe, Cr, Mn, P, Cu, K, Na, Ga, Ge, Se, Zn, S, Br, and C were measured in interplanetary dust particles (IDPs) collected from the Earth's stratosphere. All elements with nebular condensation temperatures lower than Mn, except S, were enriched relative to the most volatile-rich type of meteorite while the refractory elements Cr and Ni were present at chondritic abundances. This element abundance pattern is consistent with nebular condensation, suggesting the IDPs condensed at either a different location or time in the evolving solar nebula than do the meteorites. The enrichments of the major elements C, Na, P, and K exclude the possibility that the volatile enrichment in IDPs results from a minor amount of contamination.

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Martins, Rayssa, Sven Kuthning, Barry J. Coles, Katharina Kreissig, and Mark Rehkämper. "Nucleosynthetic isotope anomalies of zinc in meteorites constrain the origin of Earth’s volatiles." Science 379, no. 6630 (January 27, 2023): 369–72. http://dx.doi.org/10.1126/science.abn1021.

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Material inherited from different nucleosynthesis sources imparts distinct isotopic signatures to meteorites and terrestrial planets. These nucleosynthetic isotope anomalies have been used to constrain the origins of material that formed Earth. However, anomalies have only been identified for elements with high condensation temperatures, leaving the origin of Earth’s volatile elements unconstrained. We determined the isotope composition of the moderately volatile element zinc in 18 bulk meteorites and identified nucleosynthetic zinc isotope anomalies. Using a mass-balance model, we find that carbonaceous bodies, which likely formed beyond the orbit of Jupiter, delivered about half of Earth’s zinc inventory. Combined with previous constraints obtained from studies of other elements, these results indicate that ~10% of Earth’s mass was provided by carbonaceous material.

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Sossi, Paolo A., Frédéric Moynier, and Kirsten van Zuilen. "Volatile loss following cooling and accretion of the Moon revealed by chromium isotopes." Proceedings of the National Academy of Sciences 115, no. 43 (October 8, 2018): 10920–25. http://dx.doi.org/10.1073/pnas.1809060115.

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Terrestrial and lunar rocks share chemical and isotopic similarities in refractory elements, suggestive of a common precursor. By contrast, the marked depletion of volatile elements in lunar rocks together with their enrichment in heavy isotopes compared with Earth’s mantle suggests that the Moon underwent evaporative loss of volatiles. However, whether equilibrium prevailed during evaporation and, if so, at what conditions (temperature, pressure, and oxygen fugacity) remain unconstrained. Chromium may shed light on this question, as it has several thermodynamically stable, oxidized gas species that can distinguish between kinetic and equilibrium regimes. Here, we present high-precision Cr isotope measurements in terrestrial and lunar rocks that reveal an enrichment in the lighter isotopes of Cr in the Moon compared with Earth’s mantle by 100 ± 40 ppm per atomic mass unit. This observation is consistent with Cr partitioning into an oxygen-rich vapor phase in equilibrium with the proto-Moon, thereby stabilizing the CrO2 species that is isotopically heavy compared with CrO in a lunar melt. Temperatures of 1,600–1,800 K and oxygen fugacities near the fayalite–magnetite–quartz buffer are required to explain the elemental and isotopic difference of Cr between Earth’s mantle and the Moon. These temperatures are far lower than modeled in the aftermath of a giant impact, implying that volatile loss did not occur contemporaneously with impact but following cooling and accretion of the Moon.

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Wang, Ming-Sheng, and Michael E. Lipschutz. "Thermal Metamorphism of Primitive Meteorites—XII. The Enstatite Chondrites Revisited." Environmental Chemistry 2, no. 3 (2005): 215. http://dx.doi.org/10.1071/en04075.

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Environmental Context.The first Solar System material condensed 4.567 billion years ago, rapidly forming planetesimals—solid bodies that might combine to form planets (accretion) or survive as asteroidal meteorites. Earth’s main accretion ended within the next 30 million years, but subsequent high temperatures essentially erased evidence of this history. However, heating in these early episodes produced effects uniquely recorded by 14 volatile trace elements. The volatile element composition of chondritic meteorites, whose parent material formed closest to Earth, may thus provide important information about early planetesimal evolution. Abstract.We report data for 14 trace and ultratrace elements—Au, Co, Sb, Ga, Rb, Ag, Cs, Te, Zn, Cd, Bi, Tl, In (ordered by increasing putative nebular volatility)—in 13 enstatite (E) chondrites recovered from Antarctica and two E inclusions in the Kaidun polymict breccia that fell in 1980. These data, determined by radiochemical neutron activation analysis (RNAA), essentially double the amount of information known for E chondrites, whose parent materials formed closest to the Sun in the chondrite-forming nebular region. We discuss here the data for all 29 samples studied. The meteoritic suite studied here includes both representatives of previously rare types—like high-iron EH3 and EH5 individuals—but also unique individuals and previously unknown low-iron, EL3, chondrites. Prior hypothetical assertions by others are corrected by the new data. Volatile element contents of EL3 and EH3 chondrites are variable, but comparable, like those of type 3 ordinary chondrites (i.e. H3, L3, and LL3). Volatile element contents of EH4 chondrites are at least as high as those of the E3 types, in contrast to the lower contents of H4, L4, and LL4 types. Compositionally, E3,4 chondrites reflect only nebular condensation and/or accretion processes. Volatiles in E5 and E6 chondrites—whether of EH, EL or unique ones—are depleted relative to cosmic (i.e. CI1) or E3,4 chondrite abundances. The evidence indicates that E5,6 chondrites compositionally reflect vaporization and loss of volatiles during open-system, thermal metamorphism of their parent(s); this may have been the terrestrial environment during Earth’s formation from early planetesimals. Compositional differences between Antarctic E5,6 chondrites and contemporary falls probably do not reflect weathering during the long residence of these chondrites in Antarctica. They might reflect differences in the starting compositions and/or metamorphic conditions in the parent(s).

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40

Yang, Jing, Yaochen Li, Yuxin He, Hongying He, Xiaoqi Chen, Tingfu Liu, and Biao Zhu. "Wild vs. Cultivated Zingiber striolatum Diels: Nutritional and Biological Activity Differences." Plants 12, no. 11 (May 31, 2023): 2180. http://dx.doi.org/10.3390/plants12112180.

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Compositional, functional, and nutritional properties are important for the use-value assessments of wild and cultivated edible plants. The aim of this study was to compare the nutritional composition, bioactive compounds, volatile compounds, and potential biological activities of cultivated and wild Zingiber striolatum. Various substances, such as soluble sugars, mineral elements, vitamins, total phenolics, total flavonoids, and volatiles, were measured and analyzed using UV spectrophotometry, ICP-OES, HPLC, and GC-MS methods. The antioxidant capacity of a methanol extract of Z. striolatum, as well as the hypoglycemic abilities of its ethanol and water extracts, were tested. The results showed that the contents of soluble sugar, soluble protein, and total saponin in the cultivated samples were higher, while the wild samples contained higher amounts of K, Na, Se, vitamin C, and total amino acids. The cultivated Z. striolatum also showed a higher antioxidant potential, while the wild Z. striolatum exhibited a better hypoglycemic activity. Thirty-three volatile compounds were identified using GC-MS in two plants, with esters and hydrocarbons being the main volatile compounds. This study demonstrated that both cultivated and wild Z. striolatum have a good nutritional value and biological activity, and can be used as a source of nutritional supplementation or even in medication.

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41

Fosua, Bridget Ataa, Lijuan Ren, Wei Qiao, Jiahao Zhang, Yanning Gao, Xianli Fu, Dunyao Yu, and Renjie Dong. "Restoring the Stability of Long-Term Operated Thermophilic Anaerobic Digestion of Maize Straw by Supplying Trace Elements." Processes 11, no. 12 (December 16, 2023): 3440. http://dx.doi.org/10.3390/pr11123440.

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Maize straw has been widely used for the production of energy through anaerobic digestion, but biogas production can be hindered by a lack of trace elemental nutrients. To address this issue, a lab-scale anaerobic plug flow reactor was continuously operated at 55 °C for 300 days, with a hydraulic retention time of 42 days and an organic loading rate of 2.1 g total solids/(L·day). Results from this study showed that between days 101 and 194, the methane yield slightly decreased from 0.26 ± 0.04 to 0.24 ± 0.03 L/g volatile solids (VS), but significant volatile fatty acid accumulation was observed by reaching up to 2759 ± 261 mg/L. After trace elements were added to the reactor, the methane yield increased to 0.30 ± 0.03 L/g VS, with 53% methane content. Around 62% of the total chemical oxygen demand and volatile solids were broken down into methane. Volatile fatty acid levels dropped and stabilized at around 210 ± 50 mg/L, indicating restored process stability. The addition of trace elements increased the abundance of Firmicutes and decreased Synergistetes in bacteria while simultaneously increasing the abundance of Methanosarcina in archaea. In conclusion, trace element supplementation was experimentally found to be necessary for stable thermophilic anaerobic digestion of maize straw.

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El Babili, Fatiha, Christine Roques, Laila Haddioui, Floriant Bellvert, Cédric Bertrand, and Christian Chatelain. "Velamo do Campo: Its Volatile Constituents, Secretory Elements, and Biological Activity." Journal of Medicinal Food 15, no. 7 (July 2012): 671–76. http://dx.doi.org/10.1089/jmf.2011.0252.

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43

Chavero, C., R. de la Reza, R. C. Domingos, N. A. Drake, C. B. Pereira, and O. C. Winter. "Distribution of refractory and volatile elements in CoRoT planet host stars." Proceedings of the International Astronomical Union 5, S265 (August 2009): 424–25. http://dx.doi.org/10.1017/s1743921310001146.

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AbstractWe report on preliminary results of spectroscopic determination of the atmospheric parameters and chemical abundances of the parent stars of the recently discovered transiting planets CoRoT-2b and CoRoT-4b. We found a flat distribution of the relative abundances as a function of their condensation temperatures. Also, we introduce a new methodology to investigate a relation between the abundances of these stars and the internal migration of their planets.

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44

Ionov, Dmitri A., William L. Griffin, and Suzanne Y. O'Reilly. "Volatile-bearing minerals and lithophile trace elements in the upper mantle." Chemical Geology 141, no. 3-4 (September 1997): 153–84. http://dx.doi.org/10.1016/s0009-2541(97)00061-2.

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45

Sossi, Paolo A., Stephan Klemme, Hugh St C. O'Neill, Jasper Berndt, and Frédéric Moynier. "Evaporation of moderately volatile elements from silicate melts: experiments and theory." Geochimica et Cosmochimica Acta 260 (September 2019): 204–31. http://dx.doi.org/10.1016/j.gca.2019.06.021.

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46

Liezers, M., G. C. Eiden, and A. J. Carman. "Remote sensing volatile elements for new signatures from underground nuclear explosions." Journal of Radioanalytical and Nuclear Chemistry 318, no. 1 (September 4, 2018): 55–64. http://dx.doi.org/10.1007/s10967-018-6167-8.

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Takeda, Yoichi, Bun’ei Sato, Eiji Kambe, Wako Aoki, Satoshi Honda, Satoshi Kawanomoto, Seiji Masuda, et al. "Photospheric Abundances of Volatile and Refractory Elements in Planet-Harboring Stars." Publications of the Astronomical Society of Japan 53, no. 6 (December 25, 2001): 1211–21. http://dx.doi.org/10.1093/pasj/53.6.1211.

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48

Chavero, C., R. de la Reza, R. C. Domingos, N. A. Drake, C. B. Pereira, and O. C. Winter. "Distribution of refractory and volatile elements in CoRoT exoplanet host stars." Astronomy and Astrophysics 517 (July 2010): A40. http://dx.doi.org/10.1051/0004-6361/200912184.

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49

Kreutzberger, Melanie E., Michael J. Drake, and John H. Jones. "Origin of the Earth's moon: Constraints from alkali volatile trace elements." Geochimica et Cosmochimica Acta 50, no. 1 (January 1986): 91–98. http://dx.doi.org/10.1016/0016-7037(86)90051-7.

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Grigorovich, S. L., V. A. Fedorov, and N. S. Shumilkin. "The direct laser thermochemical synthesis of volatile hydrides from the elements." Spectrochimica Acta Part A: Molecular Spectroscopy 46, no. 4 (January 1990): 487–88. http://dx.doi.org/10.1016/0584-8539(90)80158-u.

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