Characterization of the shallow groundwater system in an area with thin soils and sinkholes

Door County, Wisconsin, is a region of karst topography underlain by Silurian dolomite bedrock. Numerous sinkholes intercept much of the surface runoff and act as sites for direct groundwater recharge. The clay-rich and impermeable Upper Ordovician Maquoketa formation separates the dolomite aquifer from the deeper aquifers and appears to be a factor in groundwater circulation and karst formation Thin glacial drift and Quaternary materials overlie the dolomite and are hydrologically connected with it The interactions of surface and groundwater, and the role of solution features in water interchange were studied in a small drainage basin. This basin contains several large sinkholes and a nearby spring complex Mapping identified many additional sinks and swallets in surface drainage routes Water flowing into two sinks was traced and found to have a residence time of several hours. Water flowing into sinkholes and from the spring was sampled to identify the quality and seasonal trends in composition of the shallow groundwater Water quality parameters monitored include magnesium, sodium, potassium, chloride, phosphorous, nitrate and ammonia, nitrogen, alkalinity, pH, turbidity, and specific conductance. Nitrate levels were found to increase 5 to 6 times during periods when there was zero input through sinkhole recharge sites. Nitrate levels approached the 10 mg/l NO₃ ⁻-N limit set by the U.S. Public Health Service for drinking water In this basin sandy soils are most susceptible to sink development, whereas clay-rich soils have a lesser number of sinks. It appears, however, that a network of bedrock solution features exists under all soils The loss of soil into sinkholes has impacted groundwater quality and reduced agricultural productivity through a reduction in tillable acreage and water retention capacity.     

X-ray K-edge absorption spectra of Fe minerals and model compounds: II. EXAFS

K-edge extended X-ray absorption fine structure (EXAFS) spectra of Fe in varying environments in a suite of well-characterized silicate and oxide minerals were collected using synchrotron radiation and analyzed using single scattering approximation theory to yield nearest neighbor Fe-O distances and coordination numbers. The partial inverse character of synthetic hercynite spinal was verified in this way. Comparison of the results from all samples with structural data from X-ray diffraction crystal structure refinements indicates that EXAFS-derived first neighbor distances are generally accurate to ±0.02 Å using only theoretically generated phase information, and may be improved over this if similar model compounds are used to determine EXAFS phase functions. Coordination numbers are accurate to ±20 percent and can be similarly improved using model compound EXAFS amplitude information. However, in particular cases the EXAFS-derived distances may be shortened, and the coordination number reduced, by the effects of static and thermal disorder or by partial overlap of the longer Fe-O first neighbor distances with second neighbor distances in the EXAFS structure function. In the former case the total information available in the EXAFS is limited by the disorder, while in the latter case more accurate results can in principle be obtained by multiple neighbor EXAFS analysis. The EXAFS and XANES spectra of Fe in Nain, Labrador osumulite and Lakeview, Oregon plagioclase are also analyzed as an example of the application of X-ray absorption spectroscopy to metal ion site occupation determination in minerals.     

“Fluffy” Type A Ca-, Al-rich inclusions in the Allende meteorite

Allende “fluffy” Type A's (FTA's) are a distinct sub-group of Ca-, Al-rich inclusions whose primary mineral assemblage consists of Al-rich melilite (Åk 0–33), spinel that is commonly very V-rich, perovskite and, frequently, hibonite. Some contain relatively coarse-grained melilite (up to 1.5 mm) that is intensely kink-banded and commonly reversely-zoned, hibonite and V-rich spinel. Others contain much finer-grained and strain-free melilite (?50 μm) and have not been found to contain hibonite or V-rich spinel. Some FTA's contain both coarser- and finer-grained melilite and textural relationships indicate that the latter is replacing the former. FTA's are characterized by extremely irregular shapes and 60–75 volume per cent of fine-grained, secondary alteration products. Many are aggregates of innumerable nodules, each of which is surrounded by a Wark-Lovering-type rim sequence. These nodules are frequently separated from one another by matrix-like clastic rim material. Other FTA's do not have nodular structure. Structural and mineralogical characteristics of their Wark-Lovering rims suggest that FTA's did not achieve their shapes by deformation of a liquid or a hot, plastic solid. In contrast to those in Type B inclusions, formation of reverse zoning in the coarser-grained melilite crystals in FTA's cannot be understood in terms of crystallization from a liquid but are readily explainable by condensation from a solar nebular gas during a period of falling pressure. Further evidence against a liquid origin is the wide range of spinel compositions within individual coarser-grained FTA's. The fact that the reversely-zoned melilite crystals cannot have been produced in any kind of sublimation or distillation process precludes formation of these inclusions as volatilization residues. FTA's are aggregates in some of which are preserved vapor-solid condensate grains that formed at high temperature in the solar nebula.     

Stereochemistry of amino acids in surface samples of a marine sediment

In two surface samples of marine sediment, the percentages of d-alanine and d-aspartic acid are significantly higher than the other d-amino acids and are similar to the range found in soils. The percentage of d-glutamic acid is also higher than the other amino acids but less than d-alanine and d-aspartic acid. These d-amino acids may come mainly from bacteria.     

Observations and theoretical reconstruction of the green flash

Summary The phenomenon of the green flash at sunset (or sunrise) is reviewed. Several possible mechanisms that have been put forth to explain the green flash are discussed. A quantitative model for the phenomenon is then described, which includes parameters that are representative for a polar atmosphere (low humidity and small aerosol optical depth). It is supposed that the primary mechanism responsible for causing the green flash are natural molecular disperion, and, the filtering action imposed by the atmosphere for low elevation angles. Results from the model indicate that a green rim of vertical extent 0.15 milliradians would appear at the upper limb of the sun during sunset or sunrise. The theoretical results are compared with observations of a green flash made at wintertime in interior Alaska.     

Comparisons between the diets of distant taxa (teleost and cormorant) in an Australian estuary

While most studies of the utilisation of food resources in aquatic ecosystems have focused on comparing the diets of closely related taxa, the present study was aimed at elucidating whether the diets of five species, representing two distant taxa, were correlated and overlapped. We have thus compared the diets of a fish species (the flathead, Platycephalus speculator) with those of two small species of cormorant (little pied, Phalocrocorax melanoleucos, and little black, P. sulcirostris) and two larger species of cormorant (pied, P. varius, and black, P. carbo) in a temperate southwestern Australian estuary. The flathead and the two smaller cormorants consumed predominantly shrimp and small, short-lived teleosts, whereas the two larger cormorants fed almost exclusively on larger species of teleost. Although the diet of flathead were correlated with and overlapped those of the two smaller cormorant species, there was no correlation or overlap between the diets of these three species and those of either of the larger species of cormorant. Our observations of P. speculator are consistent with the results of previous studies which have shown that platycephalids are ambush predators, whereas cormorants are pursuit surface plungers, with the little pied cormorant feeding solitarily and the little black cormorant feeding communally. Flathead preyed on both demersal and mid-water teleosts. The little pied cormorant fed almost exclusively on demersal teleosts and the little black cormorant exploited predominantly mid-water schooling fish. Thus, differences in the fish components of the diets of these three predators can be related to differences in the mode of foraging and the level in the water column in which feeding takes place. The respective daily consumption of shrimp and teleosts in the estuary was estimated as 1,000 kg and 450 kg by flathead and as 180 kg and 150kg by the four species of cormorants combined. The results of this study show that, in estuaries, the degree to which diets were correlated and overlapped amongst predatory vertebrates can be greater between representatives of distant taxa than between species within the same genus.     

Recovery of the mean Jovian temperature structure from inversion of spectrally resolved thermal radiance data

The mean thermal structure of the Jovian atmosphere near the temperature minimum (0.1 bar) is recovered by inversion of thermal radiance data. Improvements over previous studies of this type are made in two respects. (1) Care is taken to select data sources which are on a consistent calibration scale and from a frequency region which minimizes the variance in the recovered temperature. (2) The accuracy in the temperature recovery vs the vertical resolution capability is studied quantitatively. The contributions of various sources of systematic error, which generate significant uncertainty in the recovered thermal structure, are assessed. Sources of systematic error include assumptions about the stratospheric NLTE source function, the extent of cloud cover, the methane mixing ratio, and the calibration scale. Future investigations are outlined which would reduce such uncertainties and provide consistency with a wider range of data on the Jovian upper atmosphere.     

Photometry of the asteroid 1976 AA at 0.56 and 2.2 μm

We report observations at 0.56 and 2.2 μm of the Apollo asteroid 1976 AA made during its discovery apparition. We derive a 2.2-μm relative spectral reflectance (scaled to unity at 0.56 μm) of R(2.2 μm) = 1.5 ± 0.3. This 2.2-μm reflectance is not compatible with a carbonaceous surface composition. However, it is compatible with a wide variety of meteoritic types including ordinary chondrites, stony irons, and mesosiderites. Thus, 1976 AA may have a silicate surface similar to other Apollo-Amor objects.     

Visual and radiometric photometry of 1580 Betulia

We obtained broadband visual and 10.6-μm photometry of 1580 Betulia during its close approach to Earth in May 1976. We analyzed our photometry by using the “radiometric method” to derive the radius (2.10 ± 0.40 km) and albedo (0.108 ± 0.012) of Betulia. Radar and polarimetric results indicate a radius greater than 3.0 km and a geometric albedo of about 0.05. To be compatible with these results we also modeled Betulia as having a surface with the thermal characteristics of bare rock rather than those of the “lunar” regolith model used for previous analysis of radiometry of other asteroids. A 3.7-km radius and a geometric albedo of ～0.04 are compatible with all available observations. Betulia is the first Mars-crossing asteroid found to have such a low albedo, which may be indicative of carbonaceous surface material.