A contribution to the stable carbon isotope geochemistry of iron meteorites

For most iron meteorites studied, the carbon isotopic composition of nodular graphite falls in the range ?4.8 to ?8.2%. vs PDB and shows a mode between ?5 and ?6%.. Fourteen cohenite analyses from the Magura meteorite fall between ?18.1 and ?19.2%. with a pronounced clustering around ?18.5%.. Carbon of a taenite separate from the same meteorite has an isotopic composition of ?18.8%.; compositions between ?19.7 and ?22.1%. were found for taenite carbon in five other octahedrites. It is suggested that the ¹²C enrichment in cohenite and taenite relative to the nodular graphite is a general phenomenon in iron meteorites, and that the study of ¹³C abundances in iron meteorites may aid in the elucidation of their history. To this end an experimental study of carbon isotope fractionations in the system Fe-Ni-C is essential. The ¹³C content of carbon from several silicate inclusions in the Four Corners and ‘El Taco’ (Campo del Cielo) meteorites is generally similar to the nodular graphite, the ¹²C enrichment (?13%.) in one specimen may be interpreted in terms of a mixing model involving an original inclusion carbon and carbon exsolved from the taenite upon cooling.     

Ecological succession, palaeoenvironmental change, and depositional sequences of Barremian–Aptian shallow-water carbonates in northern Oman

Abstract Barremian and Aptian shallow‐water carbonate facies (uppermost Lekhwair, Kharaib and Shuaiba Formations) are described from outcrops in northern Oman. Based on facies analysis and bedding pattern, three orders of depositional sequences are defined (third to fifth order) and correlated between sections. Over the course of three third‐order sequences, covering the Barremian to Lower Aptian, a third‐order depositional pattern is documented that consists of a succession of three distinct faunal assemblages: discoidal orbitolinids and calcareous algae were deposited during early transgression; microbialites and microencrusters dominate the late transgressive to early highstand facies; and a rudist‐ and miliolid‐dominated facies is typical of the highstand. This ecological succession was controlled largely by palaeoenvironmental changes, such as trophic level and clay influx, rather than sedimentological factors controlled by variations in accommodation space. Orbitolinid beds and carbonates formed by microbialites and microencrusters seem to be the shallow‐water carbonate response to global changes affecting Late Barremian to Aptian palaeoclimate and palaeoceanography.     

Applicability and methodology of determining sustainable yield in groundwater systems

There is currently a need for a review of the definition and methodology of determining sustainable yield. The reasons are: (1) current definitions and concepts are ambiguous and non-physically based so cannot be used for quantitative application, (2) there is a need to eliminate varying interpretations and misinterpretations and provide a sound basis for application, (3) the notion that all groundwater systems either are or can be made to be sustainable is invalid, (4) often there are an excessive number of factors bound up in the definition that are not easily quantifiable, (5) there is often confusion between production facility optimal yield and basin sustainable yield, (6) in many semi-arid and arid environments groundwater systems cannot be sensibly developed using a sustained yield policy particularly where ecological constraints are applied. Derivation of sustainable yield using conservation of mass principles leads to expressions for basin sustainable, partial (non-sustainable) mining and total (non-sustainable) mining yields that can be readily determined using numerical modelling methods and selected on the basis of applied constraints. For some cases there has to be recognition that the groundwater resource is not renewable and its use cannot therefore be sustainable. In these cases, its destiny should be the best equitable use.

Effects Of Changing Surface Heat Flux On Atmospheric Boundary-Layer Flow Over Flat Terrain

We examine the unsteady response of a neutral atmospheric boundary layer (ABL) of depth h and friction velocity u _* when a uniform surface heat flux is applied abruptly or decreased rapidly over a time scale t<inf>θ</inf> less than about h /(10u _*). Standard Monin–Obukhov (MO) relationships are used for the perturbed eddy viscosity profile in terms of the changes to the heat flux and mean shear. Analytical solutions for changes in temperature, mean wind and shear stress profile are obtained for the surface layer, when there are small changes in h /|L_MO| over the time scale t_MO~|L _MO|/(10u_*) (where L _MO and t _MO are the length and time scales, respectively). They show that a maximum in the wind speed profile occurs at the top of the thermal boundary layer for weak surface cooling, i.e. a wind jet, whereas there is a flattening of the profile and no marked maximum for weak surface heating. The modelled profiles are approximately the same as those obtained from the U.K. Met Office Unified Model when operating as a mesoscale model at 12-km horizontal resolution. The theoretical model is modified when strong surface heating is suddenly applied, resulting in a large change in h /|L _MO| (>>1), over the time scale t _MO. The eddy structure is predicted to change significantly and the addition of convective turbulence increases the shear turbulence at the ground. A low-level wind jet can form, with convective turbulence adding to the mean momentum of the flow. This was verified by our laboratory experiment and direct numerical simulations. Additionally, it is shown that the effects of Coriolis acceleration diminish (rather than as suggested in the literature, amplify) the formation of the wind jets in the situations considered here. Hence, only when the surface heat flux changes over time scales greater than 1/f (where f is the Coriolis parameter) does the ABL adjust monotonically between its equilibrium states. These results are also applicable to the ABL passing over spatially varying surface heat fluxes.     

Amorphous Magnesiosilicate Smokes Annealed in Vacuum: The Evolution of Magnesium Silicates in Circumstellar and Cometary Dust

The mid-infrared spectral evolution of amorphous metastable eutectic magnesiosilica smokes, obtained by kinetically controlled gas-to-solid condensation of a Mg-SiO-O₂-H₂ vapor, proceeded in three distinct phases as a function of increasing time and temperature. This paper reports the mineralogical and chemical properties of these same samples. We found a previously unanticipated size dependence of the petrologic development of the initially amorphous magnesiosilica smokes that may also be at least partially responsible for the previously reported spectroscopic changes. Condensed grains less than approximately 20 nm in diameter remained amorphous throughout the thermal annealing experiment. Mineralogical changes occurred only after fusion of condensed magnesiosilica grains and chemical homogenization of large amorphous agglomerates and ring structures. Kinetically favored nucleation and growth produced the thermodynamically unstable nanocrystalline assemblage forsterite + tridymite. Further mineralogical development was stalled until continued fusing of agglomerates, rings, and some fraction of condensed grains had produced smooth amorphous magnesiosilica sheets of 42 and 20 wt% MgO. In rare sheets with more than ∼55 wt% MgO large forsterite crystals had grown, while enstatite had nucleated in low-MgO sheets still in the presence of forsterite and tridymite. The mineralogical evolution of the samples is critically dependent on the mass of the structural entities in the condensed sample and seems to be restricted to fused agglomerates and ring structures larger than about 20 nm in diameter and the sheet materials. We discuss the implications of our study for the interpretation of similar astrophysical dust analog studies and for astrophysical applications.     

High resolution problems in astrometry and spectroscopy of binaries and their significance for the progress of stellar physics

Two centuries were necessary for binaries to become, after having been unknown and ignored, one of the outstanding subjects of stellar research. This remarkable evolution has resulted now in the reversed situation with the painful question, at least for some of us: do single stars really exist? It is recognized by everybody, that many essential properties of stars can only be obtained from observations of close and wide binaries. It is the aim of this contribution to see how binaries can help us to better understand binaries and single stars, even if the existence of the latter is not yet definitely confirmed.     

Uranium-lead systematics. The case of crystals with discrete cores

The method of Levchenkov & Shukolyukov for calculating age and time of disturbance of minerals without correction for original lead is generalized to include the cases when (1) original lead and radiogenic lead leach differently, and (2) the crystals studied consist of a core and a mantle. Is it also shown that a straight line obtained from the solution of the equations is the locus of the isotopic composition of original lead.     

Laboratory hydration of condensed magnesiosilica smokes with implications for hydrated silicates in IDPs and comets

Abstract— Samples of silica‐rich and MgO‐rich condensed, amorphous magnesiosilica smokes were hydrated to monitor systematic mineralogical and chemical changes as a function of time and temperature controlled by their unique metastable eutectic compositions, their porous texture, and the ultrafine, nanometer grain size of all entities. At water supersaturated conditions, proto‐phyllosilicates formed by spinodal‐type homogeneous nucleation. Their formation and subsequent growth was entirely determined by the availability of water via pore spaces inherited from the original smokes and the textural continuity of magnesiosilica material with a mostly smectite‐dehydroxylate composition. The results may have implications for the hydration of proto‐CI material, the presence of rare periclase and brucite in primitive solar system bodies, and the pervasiveness of hydrated amorphous magnesiosilica dust and saponite proto‐phyllosilicates in icy‐protoplanets, such as comet nuclei.     

The formation of Mg,Fe‐silicates by reactions between amorphous magnesiosilica smoke particles and metallic iron nanograins with implications for comet silicate origins

This thermal annealing experiment at 1000 K for up to 167 h used a physical mixture of vapor phase‐condensed magnesiosilica grains and metallic iron nanograins to test the hypothesis that a mixture of magnesiosilica grains and an Fe‐source would lead to the formation of ferromagnesiosilica grains. This exploratory study found that coagulation and thermal annealing of amorphous magnesiosilica and metallic grains yielded ferromagnesiosilica grains with the Fe/(Fe + Mg) ratios in interplanetary dust particles. Furthermore, decomposition of brucite present in the condensed magnesiosilica grains was the source for water and the cause of different iron oxidation states, and the formation of amorphous Fe³⁺‐ferrosilica, amorphous Fe³⁺‐Mg, Fe‐silicates, and magnesioferrite during thermal annealing. Fayalite and ferrosilite that formed from silica/FeO melts reacted with forsterite and enstatite to form Mg, Fe‐silicates. The presence of iron in different oxidation states in extraterrestrial materials almost certainly requires active asteroid‐like parent bodies. If so, the possible presence of trivalent Fe compounds in comet P/Halley suggests that Halley‐type comets are a mixture of preserved presolar and processed solar nebula dust. The results from this thermal annealing experiment further suggest that the Fe‐silicates detected in the impact‐induced ejecta from comet 9P/Temple 1 might be of secondary origin and related to the impact experiment or to processing in a regolith.