Sediment-water oxygen and nutrient fluxes in a river-dominated estuary     

Kenneth G. Teague  Christopher J. Madden  John W. Day 《Estuaries and Coasts》1988,11(1):1-9

Sediment oxygen uptake and net sediment-water fluxes of dissolved inorganic and organic nitrogen and phosphorus were measured at two sites in Fourleague Bay, Louisiana, from August 1981, through May 1982. This estuary is an extension of Atchafalaya Bay which receives high discharge and nutrient loading from the Atchafalaya River. Sediment O₂ uptake averaged 49 mg m^?2 h^?1. On the average, ammonium (NH₄ ⁺) was released from the sediments (mean flux =+129 μmol m^?2 h^?1), and NO₃ ^? was taken up (mean flux =?19 μmol m^?2h^?1). However, very different NO₃ ^? fluxes were observed at the two sites, with sediment uptake at the upper, river-influenced, high NO₃ ^? site (mean flux =?112 μmol m^?2 h^?1) and release at the lower, marine-influenced low NO₃ ^? site (mean flux =+79 μmol m^?2 h^?1). PO₄ ^3? fluxes were low and often negative (mean flux =?8 μmol m^?2 h^?1), while dissolved organic phosphorus fluxes were high and positive (mean flux =+124 μmol m^?2 h^?1). Dissolved organic nitrogen fluxes varied greatly, ranging from a mean of +305 μmol m^?2 h^?1 at the lower bay, to ?710 μmol m^?2 h^?1 at the upper bay. Total dissolved nitrogen and phosphorus fluxes indicated the sediments were a nitrogen (mean flux =+543 μmol m^?2 h^?1) and phosphorus source (mean flux =+30 μmol m^?2 h^?1) at the lower bay, and a nitrogen sink (mean flux =?553 μmol m^?2 h^?1) and phosphorus source (mean flux =+17 μmol m^?2 h^?1) in the upper bay. Mean annual O∶N ration of the positive inorganic sediment fluxes were 27∶1 at the upper bay and 18∶1 at the lower bay. Based on these data we hypothesize that nitrification and denitrification are important sediment processes in the upper bay. We further hypothesize that Atchafalaya River discharge affects sediment-water fluxes through seasonally high nutrient loading which leads to net nutrient uptake by sediments in the upper bay and release in the lower bay, where there is less river influnces.  相似文献   

High resolution polarimetry of the Sun at 3.7 and 11.1 cm wavelengths     

Kenneth R. Lang 《Solar physics》1977,55(1):63-68

Two methods of observing the neutral line of the large-scale photospheric magnetic field are compared: (1) neutral line positions inferred from H photographs (McIntosh, 1972a, 1975; McIntosh and Nolte, 1975) and (2) observations of the photospheric magnetic field made with low spatial resolution (3) and high sensitivity using the Stanford magnetograph. The comparison is found to be very favorable.  相似文献   

Quantitative Analysis of H₂OComa Images Using a Multiscale MHD Model with Detailed Ion Chemistry     

Roman M. Häberli  Michael R. Combi  Tamas I. Gombosi  Darren L. De Zeeuw  Kenneth G. Powell 《Icarus》1997,130(2):373-386

The observation of ions created by ionization of cometary gas, either by ground-based observations or byin situmeasurements can give us useful information about the gas production and composition of comets. However, due to the interaction of ions with the magnetized solar wind and their high chemical reactivity, it is not possible to relate measured ion densities (or column densities) directly to the parent gas densities. In order to quantitatively analyze measured ion abundances in cometary comae it is necessary to understand their dynamics and chemistry. We have developed a detailed ion–chemical network of cometary atmospheres. We include production of ions by photo- and electron impact-ionization of a background neutral atmosphere, charge exchange of solar wind ions with cometary atoms/molecules, reactions between ions and molecules, and dissociative recombination of molecular ions with thermal electrons. By combining the ion–chemical network with the three-dimensional plasma flow as computed by a new fully three-dimensional MHD model of cometary plasma environments (Gombosiet al.1996) we are able to compute the density of the major cometary ions everywhere in the coma. The input parameters for our model are the solar wind conditions (density, speed, temperature, magnetic field) and the composition and production rate of the gas. We applied our model to Comet P/Halley in early March 1986, for which the input parameters are reasonably well known. We compare the resulting column density of H₂O⁺with ground-based observations of H₂O⁺from DiSantiet al.(1990). The results of our model are in good agreement with both the spatial distribution and the absolute abundance of H₂O⁺and with their variations with the changing overall water production rate between two days. The results are encouraging that it will be possible to obtain production rates of neutral cometary constituents from observations of their ion products.  相似文献   

The astronomical theory of climatic change on Mars     

Owen B. Toon  James B. Pollack  William Ward  Joseph A. Burns  Kenneth Bilski 《Icarus》1980,44(3):552-607

We examine the response of Martian climate to changes in solar energy deposition caused by variations of the Martian orbit and obliquity. We systematically investigate the seasonal cycles of carbon dioxide, water, and dust to provide a complete picture of the climate for various orbital configurations. We find that at low obliquity (15°) the atmospheric pressure will fall below 1 mbar; dust storms will cease; thick permanent CO₂ caps will form; the regolith will release CO₂; and H₂O polar ice sheets will develop as the permafrost boundaries move poleward. At high obliquity (35°) the annual average polar temperature will increase by about 10°K, slightly desorbing the polar regolith and causing the atmospheric pressure to increase by not more than 10 to 20 mbar. Summer polar ground temperatures as high as 273°K will occur. Water ice caps will be unstable and may disappear as the equilibrium permafrost boundary moves equatorward. However, at high eccentricity, polar ice sheets will be favored at one pole over the other. At high obliquity dust storms may occur during summers in both hemispheres, independent of the eccentricity cycle. Eccentricity and longitude of perihelion are most significant at modest obliquity (25°). At high eccentricity and when the longitude of perihelion is close to the location of solstice hemispherical asymmetry in dust-storm generation and in polar ice extent and albedo will occur.The systematic examination of the relation of climate and planetary orbit provides a new theory for the formation of the polar laminae. The terraced structure of the polar laminae originates when eccentricity and/or obliquity variations begin to drive water ice off the dusty permanent H₂O polar caps. Then a thin (meters) layer of consolidated dust forms on top of a dirty, slightly thicker (tens of meters) ice sheet and the composite is preserved as a layer of laminae composed predominately of water ice. Because of insolation variation on slopes, a series of poleward- and equatorward-facing scarps are formed where the edges of the laminae are exposed. Independently of orbital variations, these scarps propagate poleward both by erosion of the equatorward slopes and by deposition on the poleward slopes. Scarp propagation resurfaces and recycles the laminae forming the distinctive spiral bands of terraces observed and provides a supply of water to form new permanent ice caps. The polar laminae boundary marks the furthest eqautorward extension of the permanent H₂O caps as the orbit varies. The polar debris boundary marks the furthest equatorward extension of the annual CO₂ caps as the orbit varies.The Martian regolith is now a significant geochemical sink for carbon dioxide. CO₂ has been irreversibly removed from the atmosphere by carbonate formation. CO₂ has also benn removed by regolith adsorption. Polar temperature increases caused by orbital variations are not great enough  相似文献   

Representations of mineral chemical analyses in 11-dimensional space part 2, amphiboles     

Kenneth Perry  Jr. 《Lithos》1968,1(4):307-321

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Location of Viking 1 Lander on the surface of Mars     

Elliot C. Morris  Kenneth L. Jones  Jan P. Berger 《Icarus》1978,34(3):548-555

A location of the Viking 1 Lander on the surface of Mars has been determined by correlating topographic features in the lander pictures with similar features in the Viking orbiter pictures. Radio tracking data narrowed the area of search for correlating orbiter and lander features and an area was found on the orbiter pictures in which there is good agreement with topographic features on the lander pictures. This location, when plotted on the 1:250,000 scale photomosaic of the Yorktown Region of Mars (U.S. Geological Survey, 1977) is at 22.487°N latitude and 48.041°W longitude.  相似文献   

Distinguished Service Award: Anne Olsen          下载免费PDF全文

Nick Page 《New Zealand geographer》2016,72(1):73-74

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Glacial Lake Musselshell: Late Wisconsin slackwater on the Laurentide ice margin in central Montana, USA     

Nicole K. Davis  William W. Locke III  Kenneth L. Pierce  Robert C. Finkel 《Geomorphology》2006,75(3-4):330

Cosmogenic surface exposure ages of glacial boulders deposited in ice-marginal Lake Musselshell suggest that the lake existed between 20 and 11.5 ka during the Late Wisconsin glacial stage (MIS 2), rather than during the Late Illinoian stage (MIS 6) as traditionally thought. The altitude of the highest ice-rafted boulders and the lowest passes on the modern divide indicate that glacial lake water in the Musselshell River basin reached at least 920–930 m above sea level and generally remained below 940 m. Exposures of rhythmically bedded silt and fine sand indicate that Lake Musselshell is best described as a slackwater system, in which the ice-dammed Missouri and Musselshell Rivers rose and fell progressively throughout the existence of the lake rather than establishing a lake surface with a stable elevation. The absence of varves, deltas and shorelines also implies an unstable lake. The changing volume of the lake implies that the Laurentide ice sheet was not stable at its southernmost position in central Montana. A continuous sequence of alternating slackwater lake sediment and lacustrine sheetflood deposits indicates that at least three advances of the Laurentide ice sheet occurred in central Montana between 20 and 11.5 ka. Between each advance, it appears that Lake Musselshell drained to the north and formed two outlet channels that are now occupied by extremely underfit streams. A third outlet formed when the water in Lake Musselshell fully breached the Larb Hills, resulting in the final drainage of the lake. The channel through the Larb Hills is now occupied by the Missouri River, implying that the present Missouri River channel east of the Musselshell River confluence was not created until the Late Wisconsin, possibly as late as 11.5 ka.  相似文献   

Evaluating the photoalteration of estuarine dissolved organic matter using direct temperature-resolved mass spectrometry and UV-visible spectroscopy     

Elizabeth C. Minor  Brent J. Dalzell  Aron Stubbins  Kenneth Mopper 《Aquatic Sciences - Research Across Boundaries》2007,69(4):440-455

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南极Lambert, Mellor和Fisher冰川的物质平衡及Amery冰架底部物质通量的估算     

温家洪  Kenneth C.Jezek  Beata M.Csathó  Ute C.Herzfeld  Katy L.Farness 《中国科学D辑》2007,37(9):1192-1204

利用现场观测与遥感数据对Lambert, Mellor和Fisher冰川的物质平衡及其在Amery冰架的底部融化与冻结状况进行了估算. 结果表明, 澳大利亚组织的Lambert冰川盆地(LGB)考察路线的上游地区, Lambert与Mellor冰川分别为(3.9±2.1)和(2.1±2.4) Gt·a^-1的正平衡, 而Fisher冰川基本处于平衡状态. 上游地区总的正平衡为(5.9±4.9) Gt·a^-1. 考察路线以下, 3条冰川均处于负平衡, 总的负平衡为(-8.5±5.8) Gt·a^-1. 整个Lambert, Mellor和Fisher冰川均接近于平衡状态. 3条冰川总净平衡为(-2.6±6.5) Gt·a^-1. 前人认为GL线(1970年代初澳大利亚在LGB建立的冰川运动观测点的连线)以上的内陆盆地处于显著正平衡, 可能是因为过高地估算了总积累量, 并低估了穿过GL线的冰通量. 靠近Amery冰架南端着地线, 冰架底部的平均融化速率为(-23.0±3.5) m冰·a^-1, 向下游方向快速减小, 并在距冰架最南端约300 km处过渡为底部冻结. 沿3条冰川在Amery冰架的冰流带(flowband), 冻结速率约介于(0.5±0.1)~(1.5±0.2) m 冰·a^-1. 由于冰流带底部的融化, 流入冰架的内陆冰损失了大约80%±5%. 3条冰流带底部总融化和总冻结分别为(50.3±7.5)和(7.0±1.1) Gt 冰·a^-1, 这要比前人通过模拟和海洋观测估算的整个Amery冰架底部总融化和总冻结还要大很多.  相似文献