Fracture Aperture Measurements and Migration of Solutes, Viruses, and Immiscible Creosote in a Column of Clay-Rich Till   总被引：1，自引：0，他引：1  

K. Hinsby  L.D. McKay  P. JØrgensen  M. Lenczewski  C.P. Gerba 《Ground water》1996,34(6):1065-1075

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A calculation of the Rosseland mean opacity of dust grains in primordial solar system nebulae     

James B. Pollack  Christopher P. McKay  Bruce M. Christofferson 《Icarus》1985,64(3):471-492

The Rosseland mean opacity was determined for an ensemble of dust grain species though to have been present in the early solar nebula, as well as in the primordial nebulae that helped to form the outer planets. In performing these calculations, we have derived and used more general equation for the Rosseland opacity that allows for anisotropic scattering. The identity of the major particle species and their relative abundances were found from thermodynamic equilibrium and solar elemental abundances. The optical constants of these materials were defined at wavelengths ranging from near-UV to the radio domain. Calculations were performed for a very wide range of particle size distributions, including a nominal one based on that of interstellar dust grains. In addition, asymptotic expressions for the Rosseland opacity are derived in the limits of very small and very large sized particles. Results are presented for nebular temperatures varying from 10 to 2500°K and for nebular gas densities varying from 10^?14 to 1 g/cm³. The values of the Rosseland mean opacity do not depend sensitively on the choice of the particle size distribution function, provided that there are few particles having sizes in excess of several tens of microns. At low temperatures that lie within the stability field of condensed water (?200°K), this opacity varies approximately as the square of the temperature for the nominal size distribution and for all distributions having few particles larger than several tens of microns. However, the Rosseland opacity has a much weaker temperature dependence at higher temperatures for this class of size distributions and at all temperatures for size distributions containing numerous particles larger than several tens of microns. As a result, thermal convection in primordial nebulae occurs over broader ranges of altitudes at low temperatures and for size distributions for which extensive aggregation has not yet occurred.  相似文献   

Preliminary report on radiocarbon dating of cryptoendolithic microorganisms   总被引：1，自引：0，他引：1  

Bonani G  Friedmann EI  Ocampo-Friedmann R  McKay CP  Woelfli W 《Polarforschung》1988,58(2-3):199-200

The existence of microbial communities living inside desert rocks has been reported by FRIEDMANN et al. (1967, 1976), first in rocks collected from the hot and dry Negev desert and later in rocks in the frigid Ross Desert of Southern Victoria Land, Antarctica. The extremely inhospitable climatic conditions in both places has led to the suggestion that these organisms have very low rates of metabolism and may, in addition, be very old (FRIEDMANN 1982). Our preliminary measurements showed a 14C deficiency indicating a carbon age in the order of magnitude of 10(3) years.  相似文献   

Pure-phase transport and dissolution of TCE in sedimentary rock saprolite     

Lenczewski M  McKay L  Pitner A  Driese S  Vulava V 《Ground water》2006,44(3):406-414

The objective of this study was to experimentally determine the influence of pore structure on the transport and dissolution of trichloroethylene (TCE) in clay-rich saprolite. In order to simulate a "spill," pure-phase TCE containing a water-insoluble fluorescent dye was injected into two heterogeneous 24-cm-diameter by 37-cm-long undisturbed columns of water-saturated saprolite. TCE entry occurred at capillary pressures of 2.7 and 4.0 kPa. Ten or 28 d after injection, the column was sliced horizontally into three sections and visually examined. The distribution of fluorescent dye indicated that pure-phase TCE migrated mainly through fractures in the shale saprolite and through fine root holes or other macropores in the limestone saprolite residuum. Analysis of saprolite subsamples indicated that TCE was present throughout much of the saprolite column but usually at concentrations less than the solubility of TCE. This spreading was caused by diffusion, which also contributed to the rapid dissolution of TCE in the fractures and macropores. Modeling was carried out using previously published dissolution and diffusion equations. The calculations confirm that rapid disappearance of immiscible TCE can occur in this type of material because of the small size of fracture or macropore openings and the high porosity of the fine-grained material. This study indicates that industrial solvents can readily enter fractures and macropores in otherwise very fine-grained subsoils and then rapidly dissolve and diffuse into the fine-pore structure, from which they may be very difficult to remove.  相似文献   

Limits on the trapping of atmospheric CH₄ in martian polar ice analogs     

Melissa G. Trainer  Margaret A. Tolbert  Christopher P. McKay 《Icarus》2010,208(1):192-197

Recent detection of methane (CH₄) on Mars has generated interest in possible biological or geological sources, but the factors responsible for the reported variability are not understood. Here we explore one potential sink that might affect the seasonal cycling of CH₄ on Mars - trapping in ices deposited on the surface. Our apparatus consisted of a high-vacuum chamber in which three different Mars ice analogs (water, carbon dioxide, and carbon dioxide clathrate hydrates) were deposited in the presence of CH₄ gas. The ices were monitored for spectroscopic evidence of CH₄ trapping using transmission Fourier-Transform Infrared (FT-IR) spectroscopy, and during subsequent sublimation of the ice films the vapor composition was measured using mass spectrometry (MS). Trapping of CH₄ in water ice was confirmed at deposition temperatures <100 K which is consistent with previous work, thus validating the experimental methods. However, no trapping of CH₄ was observed in the ice analogs studied at warmer temperatures (140 K for H₂O and CO₂ clathrate, 90 K for CO₂ snow) with approximately 10 mTorr CH₄ in the chamber. From experimental detection limits these results provide an upper limit of 0.02 for the atmosphere/ice trapping ratio of CH₄. If it is assumed that the trapping mechanism is linear with CH₄ partial pressure and can be extrapolated to Mars, this upper limit would indicate that less than 1% is expected to be trapped from the largest reported CH₄ plume, and therefore does not represent a significant sink for CH₄.  相似文献   

Lunar deposits of possible pyroclastic origin     

Geant H Heiken  David S McKay  R.W Brown 《Geochimica et cosmochimica acta》1974,38(11):1703-1718

Glass droplets of possible pyroclastic origin are present in the lunar regolith at the Apollo 11, 15, and 17 sites. The droplets may be derived from deposits, interbedded with mare lava flows, which have been partly mixed into the regolith by impact processes. Orange glass droplets from the Apollo 17 site (spheres, ovoids, broken droplets) are both chemically and texturally homogeneous and have rare olivine phenocrysts. None of the droplets contain shock damaged crystals which are common in glass produced during meteorite impacts. The droplets are similar to those formed in terrestrial lava fountains and are here interpreted as tephra.The homogeneous glass droplets sampled at the Apollo 11, 15 and 17 sites are located on or close to mare basin rims. Vents for the youngest mare lava flows, located near basin rims, have been identified photogeologically. Dark mantle deposits, interpreted as pyroclastic blankets in some locations, and numerous rules are also present on the mare surface, near basin rims. The glass droplets, having ages nearly contemporaneous with the associated mare lavas, may be concentrated locally near such vent areas. This association is in accordance with the limited extent of ash deposits from terrestrial lava fountains (? km from the vent).  相似文献   

Aquifer vulnerability to pesticide migration through till aquitards   总被引：1，自引：0，他引：1  

Jørgensen PR  McKay LD  Kistrup JP 《Ground water》2004,42(6-7):841-855

This study investigates the influence of key factors-mainly recharge rate and degradation half-life--on downward migration of the widely used pesticide mecoprop (MCPP) through a typical clayey till aquitard. The study uses the numerical model FRAC3Dvs, which is a three-dimensional discrete fracture/matrix diffusion (DFMD) numerical transport model. The model was calibrated with laboratory and field data from a site near Havdrup, Denmark, but the overall findings are expected to be relevant to many other sites in similar settings. Fracture flow and MCPP transport parameters for the model were obtained through calibration using well-characterized laboratory experiments with large (0.5 m diameter by 0.5 m high) undisturbed columns of the fractured till and a field experiment. A second level of upscaling and sensitivity analysis was then carried out using data on hydraulic head, fracture spacing, and water budget from the field site. The simulations of downward migration of MCPP show that MCPP concentration and mass flux into the underlying aquifer, and hence the aquifer vulnerability to this pesticide compound, is mainly dependent on the degradation rate of the pesticide, the overall aquitard water budget, and the ground water recharge rate into the aquifer. The influence of flow rate, matrix diffusion, and degradation rate are intertwined. This results in one to four orders of magnitude higher MCPP flux into the aquifer from aquifer recharge rates of 20 and 120 mm/yr, respectively, for no degradation and MCPP half-life of 0.5 yr. From a sensitivity analysis it was found that the range of MCPP flux into the aquifer varied less than one order of magnitude due to (1) changing fracture spacing from 1 to 10 m, or (2) preferential flow along inclined thin sand layers, which represent common conditions for the current and other settings of clayey till in Denmark and other glaciated areas in Europe and North America. The results indicate that for aquifers overlain by fractured clayey tills, the vulnerability to contamination with pesticides (pesticide flux into the aquifer) and other widespread agricultural contaminants is going to vary strongly in the watershed as a function of the distribution of aquitard water budget (flow rate) and aquitard redox environment (controlling contaminant degradation rates), even if the thickness of the till is relatively constant. DFMD modeling of cause-effect relationships within such systems has great potential to support decisions in planning, regulation, and contaminant remediation.  相似文献   

Paleolakes on Mars     

Robert A. Wharton Jr.  Jamison M. Crosby  Christopher P. McKay  James W. Rice Jr. 《Journal of Paleolimnology》1995,13(3):267-283

Observational evidence such as outflow channels and valley networks suggest that in the past there was flowing water on Mars. The images of fluvial features on Mars logically suggest that there must exist downstream locations in which the water pooled and the sediment load deposited (i.e. lakes). Sediments and morphological features associated with the martian paleolakes are believed to occur in Valles Marineris, and several large basins including Amazonis, Chryse and Elysium planitia. As Mars became progressively colder over geological time, any lakes on its surface would have become seasonally, and eventually perennially ice-covered. We know from polar lakes on Earth that ice-covered lakes can persist even when the mean annual temperature falls below freezing. Thus, the most recent lacustrine sediments on Mars were probably deposited in ice-covered lakes. While life outside of the Earth's atmosphere has yet to be observed, there is a general consensus among exobiologists that the search for extraterrestrial life should be based upon liquid water. The inference that there was liquid water on Mars during an earlier epoch is the primary motivation for considering the possibility of life during this time. It would be of enormous interest from both an exobiological and paleolimnological perspective to discover lakes or the evidence of former lakes on another planet such as Mars. Limnology would then become an interplanetary science.  相似文献   

A coupled soil-atmosphere model of H2O2 on Mars     

Bullock MA  Stoker CR  McKay CP  Zent AP 《Icarus》1994,107(1):142-154

The Viking Gas Chromatograph Mass Spectrometer failed to detect organic compounds on Mars, and both the Viking Labeled Release and the Viking Gas Exchange experiments indicated a reactive soil surface. These results have led to the widespread belief that there are oxidants in the martian soil. Since H2O2 is produced by photochemical processes in the atmosphere of Mars, and has been shown in the laboratory to reproduce closely the Viking LR results, it is a likely candidate for a martian soil oxidant. Here, we report on the results of a coupled soil/atmosphere transport model for H2O2 on Mars. Upon diffusing into the soil, its concentration is determined by the extent to which it is adsorbed and by the rate at which it is catalytically destroyed. An analytical model for calculating the distribution of H2O2 in the martian atmosphere and soil is developed. The concentration of H2O2 in the soil is shown to go to zero at a finite depth, a consequence of the nonlinear soil diffusion equation. The model is parameterized in terms of an unknown quantity, the lifetime of H2O2 against heterogeneous catalytic destruction in the soil. Calculated concentrations are compared with a H2O2 concentration of 30 nmoles/cm3, inferred from the Viking Labeled Release experiment. A significant result of this model is that for a wide range of H2O2 lifetimes (up to 10(5) years), the extinction depth was found to be less than 3 m. The maximum possible concentration in the top 4 cm is calculated to be approximately 240 nmoles/cm3, achieved with lifetimes of greater than 1000 years. Concentrations higher than 30 nmoles/cm3 require lifetimes of greater than 4.3 terrestrial years. For a wide range of H2O2 lifetimes, it was found that the atmospheric concentration is only weakly coupled with soil loss processes. Losses to the soil become significant only when lifetimes are less than a few hours. If there are depths below which H2O2 is not transported, it is plausible that organic compounds, protected from an oxidizing environment, may still exist. They would have been deposited by meteors, or be the organic remains of past life.  相似文献   

Microscopic physical biomarkers in carbonate hot springs: implications in the search for life on Mars.   总被引：2，自引：0，他引：2  

C C Allen  F G Albert  H S Chafetz  J Combie  C R Graham  T L Kieft  S J Kivett  D S McKay  A Steele  A E Taunton  M R Taylor  K L Thomas-Keprta  F Westall 《Icarus》2000,147(1):49-67

Physical evidence of life (physical biomarkers) from the deposits of carbonate hot springs were documented at the scale of microorganisms--submillimeter to submicrometer. The four moderate-temperature (57 to 72 degrees C), neutral pH springs reported on in this study, support diverse communities of bacteria adapted to specific physical and chemical conditions. Some of the microbes coexist with travertine deposits in endolithic communities. In other cases, the microbes are rapidly coated and destroyed by precipitates but leave distinctive mineral fabrics. Some microbes adapted to carbonate hot springs produce an extracellular polymeric substance which forms a three-dimensional matrix with living cells and cell remains, known as a biofilm. Silicon and iron oxides often coat the biofilm, leading to long-term preservation. Submicrometer mineralized spheres composed of calcium fluoride or silica are common in carbonate hot spring deposits. Sphere formation is biologically mediated, but the spheres themselves are apparently not fossils or microbes. Additionally, some microbes selectively weather mineral surfaces in distinctive patterns. Hot spring deposits have been cited as prime locations for exobiological exploration of Mars. The presence of preserved microscopic physical biomarkers at all four sites supports a strategy of searching for evidence of life in hot spring deposits on Mars.  相似文献