Using GIS Internships to Build Capacity in a Disadvantaged Society     

Tracey Morton McKay 《Transactions in GIS》1999,3(4):370-370

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Heat budget for a shallow,sinuous salt marsh estuary     

Paul McKay  Daniela Di Iorio 《Continental Shelf Research》2008

An experimental study of temperature cycles and the heat budget in the Duplin River, a tidal creek bordered by extensive intertidal salt marshes, was carried out in late summer of 2003 and spring of 2004 near Sapelo Island on the central Georgia coast in the southeastern US. Three water masses are identified with differing temperature and salinity regimes, the characteristics of which are dictated by channel morphology, tidal communication with the neighboring sound, ground water hydrology, the extent of local intertidal salt marshes and side channels and the spring–neap tidal cycle (which controls both energetic mixing and, presumably, ground water input). For the first experiment, heat budgets are constructed for the upper (warmer) and lower (cooler) areas of the Duplin River showing the diminishing importance of tidal advection away from the mouth of the creek along with the concomitant increase in the importance of both direct atmospheric fluxes and of interactions with the marsh and side creeks. The second experiment, in the spring of 2004, reexamines the heat budget on seasonal and daily averaged scales revealing the decreased importance of advective fluxes relative to direct atmospheric fluxes on this scale but the constant importance of marsh/creek interactions regardless of time scale or season. Short period temperature fluctuations which affect larval development are examined and analogies are drawn to use heat to understand the marsh as a source of sediment, carbon and other nutrients.  相似文献   

The Sloan Digital Sky Survey monitor telescope pipeline     

D.L. Tucker  S. Kent  M.W. Richmond  J. Annis  J.A. Smith  S.S. Allam  C.T. Rodgers  J.L. Stute  J.K. Adelman‐McCarthy  J. Brinkmann  M. Doi  D. Finkbeiner  M. Fukugita  J. Goldston  B. Greenway  J.E. Gunn  J.S. Hendry  D.W. Hogg  S.‐I. Ichikawa   . Ivezi&#x;  G.R. Knapp  H. Lampeitl  B.C. Lee  H. Lin  T.A. McKay  A. Merrelli  J.A. Munn  E.H. Neilsen  H.J. Newberg  G.T. Richards  D.J. Schlegel  C. Stoughton  A. Uomoto  B. Yanny 《Astronomische Nachrichten》2006,327(9):821-843

The photometric calibration of the Sloan Digital Sky Survey (SDSS) is a multi‐step process which involves data from three different telescopes: the 1.0‐m telescope at the US Naval Observatory (USNO), Flagstaff Station, Arizona (which was used to establish the SDSS standard star network); the SDSS 0.5‐m Photometric Telescope (PT) at the Apache Point Observatory (APO), NewMexico (which calculates nightly extinctions and calibrates secondary patch transfer fields); and the SDSS 2.5‐m telescope at APO (which obtains the imaging data for the SDSS proper). In this paper, we describe the Monitor Telescope Pipeline, MTPIPE, the software pipeline used in processing the data from the single‐CCD telescopes used in the photometric calibration of the SDSS (i.e., the USNO 1.0‐m and the PT). We also describe transformation equations that convert photometry on the USNO‐1.0m u ′g ′r ′i ′z ′ system to photometry the SDSS 2.5m ugriz system and the results of various validation tests of the MTPIPE software. Further, we discuss the semi‐automated PT factory, which runs MTPIPE in the day‐to‐day standard SDSS operations at Fermilab. Finally, we discuss the use of MTPIPE in current SDSS‐related projects, including the Southern u ′g ′r ′i ′z ′ Standard Star project, the u ′g ′r ′i ′z ′ Open Star Clusters project, and the SDSS extension (SDSS‐II). (© 2006 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)  相似文献   

Microstructure,chemistry, and origin of grain rims on ilmenite from the lunar soil finest fraction     

Roy CHRISTOFFERSEN  DAVID S. McKay  Lindsay P. KELLER 《Meteoritics & planetary science》1996,31(6):835-848

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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