Oxygen and Carbon Isotope Studies of Contact Metamorphism of Carbonate Rocks

O¹⁸/O¹⁶ and C¹²/C¹³ ratios have been determined for carbonaterocks and coexisting minerals from two contact metamorphic aureolesat Birch Creek, California and Marble Canyon, Texas. The peliticmetasediments and granitic intrusions of the Birth Creek localitywere also analyzed for their O¹⁸/¹⁶ and D/H ratios. Oxygen andcarbon isotope fractionations in coexisting dolomite and calciteare interrelated but show no obvious correlation with sampledistance from the intrusive contact. Small-scale oxygen isotopicexchange effects between rock units are observed within a fewfeet of the intrusive-country rock contacts and the marble-schistcontacts at Birch Creek. Oxygen isotopic temperatures obtainedfrom quartz—biotite fractionations in the biotite schistsof Birch Creek show a systematic decrease with increasing distanceaway from the intrusive contact; the isotopic contact temperatureis calculated to be 535–45°C. Low O¹⁸/¹⁶ and C¹³/¹²ratiosof the contact metamorphic marbles generally correlate wellwith presence of calc-silicate minerals, indicating that theCO₂ liberated during metamorphic decarbonation reactions isenriched in both O¹⁸and C¹² relative to the carbonates. Materialbalance calculations indicate that the liberated CO₂ is about5 per mille richer in O¹⁸ and about 6 per mille richer in C¹³than coexisting calcite.     

O18/O16 Ratios in Rocks and Coexisting Minerals of the Skaergaard Intrusion, East Greenland

The Skaergaard intrusion of East Greenland is a gravitationallystratified gabbroic mass that has undergone extreme fractionalcrystallization. Oxygen-isotopic analyses have been obtainedfor the various rock types of this intrusion and for severalcoexisting minerals of these rocks. The general relationshipsamong the O¹⁸/O¹⁶ ratios of the minerals are the same as havebeen found for other igneous rocks, but the isotopic fracticnationsare smaller, probably as a result of the higher temperatureof formation of the Skaergaard rocks. The later differentiatesare progressively depleted in O¹⁸ to a marked degree relativeto the earlier-formed portions of the layered series; the late-stagegranophyres are 4–5 per mil lower in O¹⁸/O¹⁶ than thelayered Lower Zone gabbros, and are 7–9 per mil lowerthan normal granitic rocks from other localities. This progressivedepletion in O¹⁸ is a result of crystallization and settlingout of minerals that are, on the whole, about 1 per mil higherin O¹⁸/O¹⁶ than the magma liquid. Calculations based on a simplecrystallization model are in agreement with the experimentalresults.     

Inhibition of dissolution within shallow water carbonate sediments: impacts of terrigenous sediment input on syn-depositional carbonate diagenesis

The early diagenetic chemical dissolution of skeletal carbonates has previously been documented as taking place within bioturbated, shallow water, tropical carbonate sediments. The diagenetic reactions operating within carbonate sediments that fall under the influence of iron‐rich (terrigenous) sediment input are less clearly understood. Such inputs should modify carbonate diagenetic reactions both by minimizing bacterial sulphate reduction in favour of bacterial iron reduction, and by the reaction of any pore‐water sulphide with iron oxides, thereby minimizing sulphide oxidation and associated acidity. To test this hypothesis sediment cores were taken from sites within Discovery Bay (north Jamaica), which exhibit varying levels of Fe‐rich bauxite sediment contamination. At non‐impacted sites sediments are dominated by CaCO₃ (up to 99% by weight). Pore waters from the upper few centimetres of cores show evidence for active sulphate reduction (reduced SO₄/Cl^? ratios) and minor CaCO₃ dissolution (increased Ca²⁺/Cl^? ratios). Petrographic observations of carbonate grains (specifically Halimeda and Amphiroa) show clear morphological evidence for dissolution throughout the sediment column. In contrast, at bauxite‐impacted sites, the sediment is composed of up to 15% non‐carbonate and contains up to 6000 μg g^?1 Fe. Pore waters show no evidence for sulphate reduction, but marked levels of Fe(II), suggesting that bacterial Fe(III) reduction is active. Carbonate grains show little evidence for dissolution, often exhibiting pristine surface morphologies. Samples from the deeper sections of these cores, which pre‐date bauxite influence, commonly exhibit morphological evidence for dissolution implying that this was a significant process prior to bauxite input. Previous studies have suggested that dissolution, driven by sulphate reduction and sulphide oxidation, can account for the loss of as much as 50% of primary carbonate production in localized platform environments. The finding that chemical dissolution is minor in a terrigenous‐impacted carbonate environment, therefore, has significant implications for carbonate budgets and cycling, and the preservation of carbonate grains in such sediment systems.     

IDENTIFICATION OF SEA-BOTTOM SEDIMENTS BY A SHIP UNDERWAY*

The authors propose a method of determining the sedimentary composition of the sea-bottom by studying the variation of the frequency contents of the consecutive multiple reflections between bottom and surface of the sea.     

High Field Strength Element Anomalies in Arc Lavas: Source or Process?

An understanding of the origin of depletion in the high fieldstrength elements (HFSE), Nb, Zr and Ti, relative to rare earthelements (REE) in arc lavas is critical to models both for magmagenesisin ares and for the relationship between are magmatism and growthof the continental crust. The presence of HFSE depletion inboth are lavas and in the bulk continental crust constitutessome of the strongest evidence that continental crust is/wasgenerated in subduction zones, especially if the HFSE are retainedrelative to REE in the subducting slab (Saunders et al., 1980;McDonough, 1991). Recently, however, it has been proposed thatHFSE depletion develops during the main are magma melting eventin the mantle wedge (McKenzie & O'Nions, 1991), during meltascent to the surface (Kelemen et al., 1990), or even that aworld-wide shallow mantle reservoir with HFSE depletion exists(Salters & Shimizu, 1988). If so, it is possible that HFSEdepletion may have developed in magmas unrelated to subductionzones during crust-generation processes in the Precambrian.The common presence of high-MgO lavas in the Southern LesserAntilles provides a rare opportunity to test these models, becausetheir chemistry is essentially unmodified since derivation fromthe mantle. We show that depletion (relative to REE) in theHFSE Ti, Zr, and Nb exists in the mantle wedge before melting,and is probably produced by an REE-rich slab flux. In contrastto many other arcs (Woodhead et al., 1993), there is no evidencethat the Lesser Antilles mantle source is more depleted in HFSEthan the source of mid-ocean ridge basalts. Relative to REE,Ti depletion in melts is enhanced during melting, requiringa Ti-rich phase in the residue at low melt fractions. Ti depletionis also enhanced during fractionation of magnetite and amphibole,whereas relative Zr depletion is reduced during fractionation.In most arc magmas (usually <6% MgO), fractionation is probablya major control on the extent of Ti and Zr depletion. In theLesser Antilles, the extent of Nb depletion relative to La islargely unaffected by melting or crystal fractionation processes.     

The granulitic impactite suite: Impact melts and metamorphic breccias of the early lunar crust

Abstract— An important and poorly understood group of rocks found in the ancient lunar highlands is called “feldspathic granulitic impactites.” Rocks of the granulite suite occur at most of the Apollo highlands sites as hand samples, rake samples, clasts in breccias, and soil fragments. Most lunar granulites contain 70–80% modal plagioclase, but they can range from anorthosite to troctolite and norite. Previous studies have led to different interpretations for the thermal history of these rocks, including formation as igneous plutons, long-duration metamorphism at high temperatures, and short-duration metamorphism at low temperatures. This paper reports on a study of 24 polished thin sections of lunar granulites from the Apollo 15, 16, and 17 missions. We identify three different textural types of granulitic breccias: poikilitic, granoblastic, and poikilitic-granoblastic breccias. These breccias have similar equilibration temperatures (1100 ± 50 °C), as well as common compositions. Crystal size distributions in two granoblastic breccias reveal that Ostwald ripening took place during metamorphism. Solid-state grain growth and diffusion calculations indicate relatively rapid cooling during metamorphism (0.5 to 50 °C/year), and thermal modeling shows that they cooled at relatively shallow depths (<200 m). In contrast, we conclude that the poikilitic rocks formed by impact melting, whereas the poikilitic-granoblastic rocks were metamorphosed and may have partially melted. These results indicate formation of lunar granulites in relatively small craters (30–90 km in diameter), physically associated with the impact-melt breccia pile, and possibly from fine-grained fragmental precursor lithologies.     

Spinels and oxygen fugacity in olivine‐phyric and lherzolitic shergottites

Abstract— We examine the occurrences, textures, and compositional patterns of spinels in the olivine‐phyric shergottites Sayh al Uhaymir (SaU) 005, lithology A of Elephant Moraine A79001 (EET‐A), Dhofar 019, and Northwest Africa (NWA) 1110, as well as the Iherzolitic shergottite Allan Hills (ALH) A77005, in order to identify spinel‐olivine‐pyroxene assemblages for the determination of oxygen fugacity (using the oxybarometer of Wood [1991]) at several stages of crystallization. In all of these basaltic martian rocks, chromite was the earliest phase and crystallized along a trend of strict Cr‐Al variation. Spinel (chromite) crystallization was terminated by the appearance of pyroxene but resumed later with the appearance of ulvöspinel. Ulvöspinel formed overgrowths on early chromites (except those shielded as inclusions in olivine or pyroxene), retaining the evidence of the spinel stability gap in the form of a sharp core/rim boundary (except in ALH A77005, where subsolidus reequilibration diffused this boundary). Secondary effects seen in chromites include reaction with melt before ulvöspinel overgrowth, reaction with melt inclusions, reaction with olivine hosts (in ALH A77005), and exsolution of ulvöspinel or ilmenite. All chromites experienced subsolidus Fe/Mg reequilibration. Spinel‐olivine‐pyroxene assemblages representing the earliest stages of crystallization in each rock essentially consist of the highest‐Cr#, lowest‐fe# chromites not showing secondary effects plus the most magnesian olivine and equilibrium low‐Ca pyroxene. Assemblages representing the onset of ulvöspinel crystallization consist of the lowest‐Ti ulvöspinel, the most magnesian olivine in which ulvöspinel occurs as inclusions, and equilibrium low‐Ca pyroxene. The results show that, for early crystallization conditions, oxygen fugacity (fO₂) increases from SaU 005 and Dhofar 019 (?QFM ‐3.8), to EET‐A (QFM ‐2.8) and ALH A77005 (QFM ‐2.6), to NWA 1110 (QFM ‐1.7). Estimates for later conditions indicate that in SaU 005 and Dhofar 019 oxidation state did not change during crystallization. In EET‐A, there was an increase in fO₂ that may have been due to mixing of reduced material with a more oxidized magma. In NWA 1110, there was a dramatic increase, indicating a non‐buffered system, possibly related to its high oxidation state. Differences in fO₂ among shergottites are not primarily due to igneous fractionation but, rather, to derivation from (and possibly mixing of) different reservoirs.     

Concentration and variability of the AIB amino acid in polar micrometeorites: Implications for the exogenous delivery of amino acids to the primitive Earth

Abstract— Micrometeorites (MMs) are extraterrestrial particles ranging in size from 25 μm to 2 mm that survive atmospheric entry and are collected on the Earth's surface. They represent the largest mass flux (MF) of extraterrestrial material (30,000 ± 20,000 t/yr) to the present‐day Earth. Studies of large collections of MMs suggest that about 20% have not been heated to high temperatures and that they contain organic carbon. Since non‐protein amino acids have been found in some carbonaceous meteorites, they might also be found in unmelted MMs. However, previous searches for amino acids in MMs were inconclusive. We combined a new extraction method for amino acids with a highly sensitive analytical method to detect and quantitate amino acids in MMs collected at the South Pole. We found the non‐protein amino acid α‐amino isobutyric acid (AIB) in one of our samples. The non‐detection of this amino acid in the other samples analyzed suggests that there are amino acid‐containing and amino acid‐free MMs, with ?14% of the MMs containing AIB. Since the MF of MMs is much higher than that of carbonaceous chondrites (CMs), amino acids in these small particles would represent an important source of exogenous delivery of organic molecules. Therefore, the results are discussed on the basis of their implications for astrobiology.     

Fossils in folklore

Fossils have been known to people since at least Palaeolithic times, when they were employed decoratively. However, it was not until the 17th century that the true origin of fossils became widely acknowledged. In the interim period, a rich folklore developed around fossils, including some bizarre beliefs about their origins and medicinal and magical properties. Names such as thunderbolts, tonguestones, toadstones, snakestones and Devil's Toenails became widely used for different types of fossils in Britain. Fossil folklore not only played an important part in the early history of palaeontology but also serves to underline the role of comparative morphology and the need for living analogues if we are to interpret fossils correctly.