Noble gas composition in Ogi and Siena meteorites

The elemental and isotopic composition of noble gases in two chondritic meteorites which belong to documented “falls” is reported. Ogi, which belongs to the group of H-chondrites, fell in Saga, Kyushu (Japan) at 11am on 8 June 1741 and Siena which belongs to the group of LL-chondrites, fell in Tuscany (Italy) at 7pm on 16 June 1794. The recovered mass of Ogi and Siena were 14·2 and 4 kg respectively. Their exposure ages are 13±2 m.y. and 13±3 m.y. respectively.     

Isotopic composition of strontium in Indian kimberlites

Strontium isotopic studies on twenty three whole rock kimberlites from two petrographic provinces in India show variation of initial ${}^{87}\text{Sr}{}^{86}\text{Sr}$ ratios from 0.7027 to 0.7102. The variation is unrelated to the degree of alteration. Between the micaceous and basaltic varieties there is some overlap in the Sr isotopic ratios. Leaching experiments on whole rock samples showed more highly radiogenic Sr in leaches compared to the bulk samples.In two diatremes, the initial ${}^{87}\text{Sr}{}^{86}\text{Sr}$ ratios show a positive correlation with $\text{Rb}\text{Sr}$ which is believed to reflect a source event earlier than the formation of the kimberlites. The observed Sr isotopic data can be caused by (i) melting of a heterogeneous source or (ii) disequilibrium partial melting in the source region. In the former case, variable isotopic composition would be a necessary consequence of melting in small subsystems.     

Isotopic composition of thermal waters in Chukotka

Twenty three groups of thermomineral springs in eastern Chukotka with the discharge temperature of 2 to 97°C and mineralization of 1.47 to 37.14 g/l are studied and compared with surface freshwater from their localities. The δD and δ¹⁸O values in surface waters vary from ?121.4 to ?89.5‰ and from ?16.4 to ?11.1‰, respectively, while respective values in thermomineral waters range from ?134.2 to ?92.5‰ and from ?17.6 to ?10.5‰. The δD value in surface waters decreases from the east to west, i.e., toward interior areas of the peninsula. Hydrothermal springs most depleted in deuterium (δD < ?120‰) are localized in the geodynamically active Kolyuchinskaya-Mechigmen Depression. According to the proposed formation model of Chukotka thermomineral waters, their observed chemical and isotopic characteristics could result from the mixing (in different proportions) of surface waters with the deep-sourced isotopically light mineralized component (δD ≈ ?138‰, δ¹⁸O ≈ ?19‰, M = 9.5?14.7 g/l). The latter originates most likely from subpermafrost waters subjected to slight cryogenic metamorphism.     

Isotopic composition of hydration water in gypsum

The isotopic composition of the hydration water of gypsum is a sensitive diagnostic tool for specifying the mechanisms of its formation, either from an evaporating brine, by hydration of anhydriate or in situ formation in surface or groundwaters through oxidation of sulfides. Primarily, gypsum is formed in isotopic equilibrium with the mother brine; later, exchange of water occurs rapidly under humid conditions by means of a mechanism of recrystallization of gypsum or through diffusion of water into the intact crystal. Under arid conditions, however, the primary isotopic record has been preserved, in some instances, since the Pleistocene.     

Isotopic anomalies of noble gases in meteorites and their origins—III. LL-chondrites

Nine LL-chondrites were studied by a selective etching technique, to characterize the noblegas components in three mineral fractions: HF-HCl-solubles (silicates, metal, troilite, etc.; comprising ～ 99% of the meteorite), chromite and carbon (～ 0.3–0.7%) and Q (a poorly characterized mineral defined by its solubility in HNO₃, comprising ～ 0.05% of the meteorite but containing most of the Ar, Kr, Xe and a neon component of ${}^{20}\text{Ne}{}^{22}\text{Ne}\text{= 10.9 ± 0.8}$). The ${}^{20}\text{Ne}{}^{36}\text{Ar}$ ratio in Q falls wi petrologic type and rising ³⁶Ar content, as expected for condensation from a cooling solar nebula, but contrary to the trend expected for metamorphic losses. Chondrites of different petrologic types therefore cannot all be derived from the same volatile-rich ancestor, but must have formed over a range of temperatures, with correspondingly different intrinsic volatile contents.The CCFXe (carbonaceous chondrite fission) component varies systematically with petrologic type. The most primitive LL3s (Krymka, Bishunpur, Chainpur) contain substantial amounts of CCFXe in chromite-carbon, enriched relative to primordial Xe as shown by high ${}^{136}\text{Xe}{}^{132}\text{Xe}$ (0.359–0.459, vs 0.310 for primordial Xe). These are accompanied by He and by Ne with ${}^{20}\text{Ne}{}^{22}\text{Ne}\text{≈ 8.0}$ and by variable amounts of a xenon component enriched in the light isotopes. The chromite in these meteorites is compositionally peculiar, containing substantial amounts of Fe(III). These meteorites, as well as Parnallee (LL3) and Hamlet (LL4) also contain CCFXe in phase Q, heavily diluted by primordial $\text{Xe}\text{(}{}^{136}\text{Xe}{}^{132}\text{Xe}\text{= 0.317–0.329)}$. On the other hand, LL5s and 6s (Olivenza, St. Séverin, Manbhoom and Dhurmsala) contain no CCFXe in either mineral. This deficiency must be intrinsic rather than caused by metamorphic loss, because Q in these meteorites still contains substantial amounts of primordial Ne.If CCFXe comes from a supernova, then its distribution in LL-chondrites requires three presolar carrier minerals of the right solubility properties, containing three different xenon components in certain combinations. These minerals must be appropriately distributed over the petrologic types, together with locally produced Q containing primordial gases, and they must be isotopically normal, in contrast to the gases they contain. On the other hand, if CCFXe comes from fission of a volatile superheavy element, then its decrease from LL3 to LL6 can be attributed to progressively less complete condensation from the solar nebula. Ad hoc assumptions must of the host phase Q, its association with ferrichromite and the origin of the associated xenon component enriched in the light isotopes.Soluble minerals in LL3s and LL4s contain a previously unobserved, solar xenon component, which, however, is not derived from the solar wind. Three types of ‘primordial’ xenon thus occur side-by-side in different minerals of the same meteorite: strongly fractionated Xe in ferrichromite and carbon, lightly fractionated Xe in phase Q, and ‘solar’ Xe in solubles. Because the first two can apparently be derived from the third by mass fractionation, it seems likely that all were trapped from the same solar nebula reservoir, but with different degrees of mass fractionation.     

Chemical composition of lunar meteorites and the lunar crust

The paper presents the first analyses of major and trace elements in 19 lunar meteorites newly found in Oman. These and literature data were used to assay the composition of highland, mare, and transitional (highland-mare interface) regions of the lunar surface. The databank used in the research comprises data on 44 meteorites weighing 11 kg in total, which likely represent 26 individual falls. Our data demonstrate that the lunar highland crust should be richer in Ca and Al but poorer in mafic and incompatible elements than it was thought based on studying lunar samples and the first orbital data. The Ir concentration in the highland crust and the analysis of lunar crater population suggest that most lunar impactites were formed by a single major impact event, which predetermined the geochemical characteristics of these rocks. Lunar mare regions should be dominated by low-Ti basalts, which are, however, enriched in LREEs compared to those sampled by lunar missions. The typical material of mare-highland interface zones can contain KREEP and magnesian VLT basalts. The composition of the lunar highland crust deduced from the chemistry of lunar meteorites does not contradict the model of the lunar magma ocean, but the average composition of lunar mare meteorites is inconsistent with this concept and suggests assimilation of KREEP material by basaltic magmas. The newly obtained evaluations of the composition of the highland crust confirm that the Moon can be enriched in refractory elements and depleted in volatile and siderophile elements.     

Isotopic composition of cellulose from aquatic organisms

The stable isotopic ratios of oxygen, carbon and the non-exchangeable carbon-bound hydrogen of cellulose from marine plants (algae and higher vascular forms) and animals (tunicates) collected in their natural habitats and from freshwater vascular plants grown in the laboratory under controlled conditions were determined.The δ¹⁸Ovalues of cellulose from all the plants and animals were 27 ±3% more positive than the δ¹⁸O values of the waters in which the organisms grew. Temperature had little or no influence on this relationship for three species of freshwater vascular plants that were analyzed. The relationship between the δ¹⁸O values of cellulose and the water used in its synthesis is probably established by the isotopic fractionation that occurs during the hydration of carbonyl groups of the intermediates involved in cellulose synthesis.The δD values of the non-exchangeable hydrogen of cellulose (determined by analyzing cellulose nitrate) from different organisms that grew in the same environment differed by large amounts. This difference ranged up to 200‰ for different species of algae collected at a single site: the corresponding difference for different species of tunicates and vascular plants was 60 and 20‰ respectively. The δD values of cellulose nitrate from different species of freshwater vascular plants grown in water of constant temperature and isotopic composition differed by as much as 60‰ The relationship between the δD values of the carbon-bound hydrogen of cellulose and the water used in its synthesis displayed a significant temperature dependence for four species of freshwater vascular plants that were analyzed. The δD values of cellulose nitrate prepared from different parts of one of the plants grown under constant conditions differed by 40‰ Hydrogen isotopic fractionation during cellulose synthesis appears to be more variable among different species and displays a larger temperature dependence than was suggested by previous studies.     

The isotopic composition of titanium in the Allende and Leoville meteorites

We describe the analytical techniques developed for the precise measurement of the titanium isotope abundances using a TiO⁺ ion beam. Terrestrial, lunar, and bulk meteorite samples yield identical results. Using a normalization to ${}^{46}\text{Ti}{}^{48}\text{Ti}$ for mass dependent isotope fractionation, we obtain the normal Ti composition: ${}^{46}\text{Ti}{}^{48}\text{Ti}\text{= 0.108548}$; ${}^{47}\text{Ti}{}^{48}\text{Ti}\text{= 0.099315 ± 0.000005}$; ${}^{49}\text{Ti}{}^{48}\text{Ti}\text{= 0.074463 ± 0.000004}$; ${}^{50}\text{Ti}{}^{48}\text{Ti}\text{= 0.072418 ± 0.000004}$ (2σ grand mean), taking ${}^{18}\text{O}{}^{16}\text{O}\text{= 0.002045}$ and ${}^{17}\text{O}{}^{16}\text{O}\text{= 0.00037}$. Measurements on thirteen coarse-grained and fine-grained Ca-Al-Ti-rich inclusions from the Allende and Leoville meteorites show the presence of widespread, significant, nonlinear isotope anomalies in the Ti isotopes which were not used for normalization. The data require the addition of at least three exotic components. The distinct correlation of non-linear effects for the most neutron-rich isotopes of Ca and Ti and the absence of substantial effects at ⁴⁶Ca in the FUN samples EK-1-4-1 and C-1 indicate that the effects reflect neutron-rich equilibrium or quasi-equilibrium nucleosynthetic processes in the outer layers of a supernova core. The results on Ca and Ti in conjunction with the isotopic effects on other elements (Mg, Sr, Ba, Nd, Sm) show that the samples represent mixtures of different nucleosynthetic components from distinctive processes (‘e’, ‘r’, ‘p’) which do not appear to be related to processes in the same stellar sites.     

Isotopic composition of sulfur in modern metalliferous hydrotherms in Cheleken

Iron and zinc sulfides, deposited by petroleum brines, are believed to have been derived from terrigenic sedimentary rocks, judging by the isotopic composition of their sulfur, and not from any deposits of these metals in the depths. This view is supported by isotopic analysis of sulfur in brines inside and outside the oil field and in waters of mud volcanoes. Isotopic composition of native (and apparently young) lead, deposited in two of the wells, may likewise represent an epigenetic concentration of the originally dispersed metals in the brines.     

Isotopic composition of precipitation and groundwater in Sicily,Italy

The isotopic composition of meteoric water in Sicily, Italy was investigated from May 2004 until June 2006. Samples were sampled monthly from a network of 50 rain gauges. During the same period 580 groundwater samples were collected from springs and wells to obtain insight into the isotopic composition of the water circulating in the main aquifers of the area. The mean weighted precipitation values were used to define the weighted local meteoric water line for five different sectors of Sicily. The use of Geographical Information System tools, coupled with isotopic vertical gradients, allowed designing an isotopic contour map of precipitation in Sicily. The defined meteoric compositions were highly consistent with most of the groundwater samples in each sector. However, in some areas fractionation processes occurring during and after rainfall slightly modify the isotopic composition of the groundwater. The obtained data set defines the present day isotopic composition of meteoric water in the central Mediterranean area and provides baseline values for future climatic and/or isotope-based hydrology studies.     

Isotopic composition and origin of the precipitation in Northern Chile

A 3 a data set of isotopes in precipitation from northern Chile show a very distinct pattern, with δ¹⁸O values ranging between −18 and −15‰ at high altitude stations, compared to δ¹⁸O values between −10 and −6‰ at the lower altitude areas. The ¹⁸O-depleted values observed in the high altitude area, the Altiplano, are related to processes that affect the air masses that originated over the Atlantic, cross the Amazon Basin (continental effect), ascend the Andes (altitude effect) and precipitated (convective effect) in the Altiplano. It is postulated that a second source of moisture, associated with air masses from the Pacific, may contribute to the ¹⁸O-enriched values observed in the lower altitude areas. Similar isotopic patterns are documented in springs and groundwater indicating that the data presented in this paper are an accurate representation of the long term behavior isotopic composition of rain in northern Chile.     

Isotopic composition of surface-correlated chromium in Apollo 16 lunar soils

We have analyzed by thermal ionization mass spectrometry (TIMS) the isotopic composition of Cr in five progressive etches of size-sorted plagioclase grains separated from lunar soils 60601 and 62281. Aliquots of the etch solutions were spiked for isotopic dilution (ID) analysis of Cr and Ca. The Ca ID data indicate that the initial etch steps represent dissolution of an average 0.1 to 0.2 μm depth from the grain surfaces, the approximate depth expected for implanted solar wind. The Cr/Ca ratio in the initial etches is several fold higher than that expected for bulk plagioclase composition, but in subsequent etches decreases to approach the bulk value. This indicates a source of Cr extrinsic to the plagioclase grains, surface-correlated and resident in the outermost fraction of a μm, which we provisionally identify as solar wind Cr. The surface-correlated Cr is isotopically anomalous and by conventional TIMS data reduction has approximately 1 permil excess ⁵⁴Cr and half as great excess ⁵³Cr. In successive etches, as the Cr/Ca ratio decreases and approaches the bulk plagioclase value, the magnitude of the apparent anomalies decreases approaching normal composition. If these results do indeed characterize the solar wind, then either the solar wind is enriched in Cr due to spallation in the solar atmosphere, or the Earth and the various parent bodies of the meteorites are isotopically distinct from the Sun and must have formed from slightly different mixes of presolar materials. Alternative interpretations include the possibility that the anomalous Cr is meteoritic rather than solar or that the observed (solar) Cr is normal except for a small admixture of spallation Cr generated on the Moon. We consider these latter possibilities less likely than the solar wind interpretation. However, they cannot be eliminated and remain working hypotheses.     

Can enstatite meteorites form from a nebula of solar composition?

Doubts have been expressed as to whether solar matter is sufficiently reducing to explain the minerals occurring in the enstatite chondrites and in the enstatite achondrites. Thermodynamic calculations on the stabilities of TiN, Si₂N₂O, CaS and silicon-bearing iron metal show that these substances can form under equilibrium conditions from a nebula of solar composition provided that the total pressure exceeds ~ 1 atm and that thermodynamic equilibria are frozen in at near-formation temperatures.     

河北平原第四系咸水同位素组成

本文讨论了河北平原地下咸水的同位素组成。并且依据水文地质、水化学和同位素特征将咸水成因分为两种类型,即大陆盐化成因和海水成因咸水。前者δ１８Ｏ＜－７．００‰,δＤ＜－５５．０‰,３６Ｃｌ／Ｃｌ＞５７±９（×１０－１５）,１４Ｃ年龄为１０００～４０００ａ（校正）;后者δ１８Ｏ＞－７．００‰,δＤ＞－５５．０‰,δ３７Ｃｌ值接近海水值,１４Ｃ年龄大于１００００ａ（校正）,咸水中的海水百分比大于３８．０％。     

Isotopic anomalies of noble gases in meteorites and their origins—VII. C3V carbonaceous chondrites

Noble gases were measured in bulk samples of the C3V chondrites Grosnaja, Vigarano, and Leoville, and in HF,HCl-insoluble residues before and after etching with HNO₃. The residues were characterized by INAA and SEM. Gas components were determined, directly or by subtraction, for the following fractions: HF,HCl-solubles (?98% of the meteorite), ‘sphase Q’, a poorly characterized trace mineral that is insoluble in HCl-HF but soluble in HNO₃, and an insoluble residue, consisting of ferrichromite, carbonaceous matter, and spinel.Bulk meteorites show some correlation of the noble-gas pattern with McSween's subclasses: two ‘oxidized’ C3V's—Allende (LEWIS et al, 1975) and Grosnaja— have lower Ar/Xe but higher Ne/Xe ratios than the ‘reduced’ C3V's—Vigarano and Leoville—which are transitional to LL3's and C3O chondrites in both respects. An HCl-soluble mineral of high Ar/Xr ratio seems to be responsible. In other respects, the 3 C3V's of this study resemble Allende, with only moderate differences. Phase Q contains most of the Ar, Kr, Xe, but only small amounts of Ne; the etched residues contain planetary Ne ($\text{Ne}{}^{20}\text{Ne}{}^{22}\text{? 8.5}$) and the controversial CCFXe component, enriched in the heavy Xe isotopes ($\text{Xe136}\text{Xe132 ? 0.4–0.5}$). The CCFXe is accompanied by an ‘L-Xe’ component that is enriched in the light Xe isotopes. The proportion of the two is virtually constant in C3V's. as in all other C-chondrites. in contrast to the ~ 2-fold variation in ordinary chondrites.C3V's have systematically higher $\text{Xe}{}^{136}\text{Xe}{}^{132}$ ratios, and hence higher ratios of CCFXe to planetary Xe, than do other chondrite classes. This may reflect some peculiarity in their formation conditions, favoring uptake of CCFXe.     

Isotopic anomalies in meteorites and their origins—V. Search for fission fragment recoils in Allende sulfides

Three troilite- and pentlandite-rich samples from the Allende C3 chondrite were analyzed for Xe (and in one case Ne and Ar) by mass spectrometry, in 13–22 temperature steps. All samples released a small ‘CCFXe’ component (enriched in the heavy isotopes Xe^{134, 136}) at the relatively low temperature of 700–800°C, ahead of adsorbed atmospheric Xe (~900°C), radiogenic Xe¹²⁹ (1000°C), and primordial Xe (1250°C). Though such a labile component suggests implanted fission recoils, the simultaneous release of Ne, Ar, and Xe^{124, 126} shows that it instead comes from carbon and perhaps chromite, two major host phases of CCFXe. Apparently small amounts of these phases are occluded in sulfides, and decompose by chemical reaction upon heating. Thus the experiment fails to resolve the nature of CCFXe.A marked enrichment of Xe¹²⁴, without corresponding enrichments in Xe¹²⁶ or Xe^131–136, was observed in the 550–650° and 1400–1500° fractions. Though requiring confirmation, it supports earlier evidence for the complexity and variability of the light xenon component, contrary to claims that it is an integral part of CCFXe.     

Pallasites—metal composition,classification and relationships with iron meteorites

Concentrations of Au, As, Co, Ga, Ge, Ir, Ni and W were determined in the metal of 28 different pallasites plus 6 which are probably paired, to help elucidate their origin. Most divide into two clusters:

     

20.

Isotopic composition of formation waters from deep drillings in southern Israel     

E Fleischer  M Goldberg  J.R Gat  M Magaritz 《Geochimica et cosmochimica acta》1977,41(4):511-525

Formation water samples from deep drillings in southern Israel fall into three regional groups, each of which shows distinct chemical and isotopic characteristics. Waters from the Mediterranean coastal plain appear to be of marine lagoonal origin; some of these brines are associated with occurrences of oil. In the mountain region the top part of the sedimentary sequence has been flushed by fresher waters, apparently during Pleistocene time. In Jurassic and deeper-lying formations one encounters concentrated brines of seawater origin, with low Na/Ca ratios, which have undergone a process of ultrafiltration. In the Rift Valley proper, magnesium-rich brines have invaded the deeper formations, and are evidently of continental lake origin.The absence of oil occurrences in association with the CaCl₂ brines of the inland locations is interpreted as being due mainly to loss of oil as a result of the tectonic events associated with the formation of the Jordan Rift Valley.     

	No.	Ni (%)	Ga (μg/g)	Ge (μg/g)	Au (μg/g)	Fa (mole %)
Main group	19	7.8–11.7	16–26	29–65	1.7–3.0	11–13
Eagle Station trio	3	14–16	4.5–6	75–120	0.8–1.0	19–20

Isotopic composition of formation waters from deep drillings in southern Israel

Formation water samples from deep drillings in southern Israel fall into three regional groups, each of which shows distinct chemical and isotopic characteristics. Waters from the Mediterranean coastal plain appear to be of marine lagoonal origin; some of these brines are associated with occurrences of oil. In the mountain region the top part of the sedimentary sequence has been flushed by fresher waters, apparently during Pleistocene time. In Jurassic and deeper-lying formations one encounters concentrated brines of seawater origin, with low Na/Ca ratios, which have undergone a process of ultrafiltration. In the Rift Valley proper, magnesium-rich brines have invaded the deeper formations, and are evidently of continental lake origin.The absence of oil occurrences in association with the CaCl₂ brines of the inland locations is interpreted as being due mainly to loss of oil as a result of the tectonic events associated with the formation of the Jordan Rift Valley.