排序方式： 共有40条查询结果，搜索用时 15 毫秒
11.
Athena Coustenis 《Astronomy& Geophysics》2007,48(2):2.14-2.20
In the Harold Jeffreys Lecture of the Royal Astronomical Society, given on 10 November 2006, Athena Coustenis examines the new world of Saturn's moon Titan, as revealed by the Cassini-Huygens mission. 相似文献
12.
A. Coustenis 《Earth, Moon, and Planets》1994,67(1-3):95-100
In spite of a marked resemblance with our planet, Titan should not be hastily considered as another Earth but rather as a useful tool in the study of chemical and physical processes in the primitive Earth. 相似文献
13.
14.
15.
Athena Masson 《Natural Hazards》2014,72(2):617-632
There is a tendency to equate the word “hurricane” with the tropical regions of the world. Many residents do not recognize the danger and risks that occur when a tropical cyclone reaches colder subtropical waters and undergoes extratropical transition. Atlantic Canada, particularly the island of Newfoundland, is most at risk from extratropical transitions. The circumstances, location and dynamics of extratropical transitions in the North Atlantic have not been extensively studied. Consequently, forecasters continue to call approaching storms “hurricanes,” when most are extratropical cyclones by the time they reach Atlantic Canada. Newfoundland, in particular, has suffered devastating impacts from extratropical transition, notably Igor in 2010. Igor impacted Newfoundland as a Category 1 hybrid system, which was still undergoing extratropical transition. Igor was an example of a classic Cape Verde cyclone. Flooding was a severe problem, destroying property and roads and isolating communities. Total damages were estimated to be at least $110 million CAD with some values reaching as high as $200 million CAD. Fire and emergency services-Newfoundland and Labrador, the government of Canada, climatologists and meteorologists will benefit from a deeper understanding of extratropical transitions. Better forecasts could warn a given population of when and where a transition could take place and how best to prepare for the consequences. 相似文献
16.
17.
The power of total coliforms (TC), faecal coliforms (FC) and Enterococci to predict the presence of Salmonella in seawater was investigated. Indicator cut-off values with the most satisfactory combination of sensitivity and specificity in predicting Salmonella presence were 1000 CFU 100 ml−1 TC, 200 CFU 100 ml−1 FC, 500 CFU 100 ml−1 Enterococci. When TC or FC were used for Salmonella prediction in logistic regression, then the addition of another indicator did not have a statistically significant effect. When Enterococci were used for prediction, then the addition of either of the two other indicators led to a statistically significant improvement (P = 0.001 for TC, P = 0.003 for FC). These results suggest that using either TC or FC alone provided an adequate indicator of Salmonella presence, but a statistically significant improvement is possible over using Enterococci alone. Concerning Enterococci, European Union limits for excellent coastal water quality (100 CFU 100 ml−1) and United States Environmental Protection Agency criteria for marine bathing waters (35 CFU 100 ml−1) have the same value in predicting Salmonella absence (92.5%). 相似文献
18.
Spatial discretization of large watersheds and its influence on the estimation of hillslope sediment yield 
下载免费PDF全文
下载免费PDF全文 Virginia I. González Athena B. Carkovic Gabriel P. Lobo Dennis C. Flanagan Carlos A. Bonilla 《水文研究》2016,30(1):30-39
The combined use of water erosion models and geographic information systems has facilitated soil loss estimation at the watershed scale. Tools such as the Geo‐spatial interface for the Water Erosion Prediction Project (GeoWEPP) model provide a convenient spatially distributed soil loss estimate but require discretization to identify hillslopes and channels. In GeoWEPP, the TOpographic PArameteriZation (TOPAZ) model is used as an automated procedure to extract a watershed boundary, hillslopes and channels from a digital elevation model (DEM). Previous studies in small watersheds have shown that the size of the hillslopes and the channel distribution affect the model estimates, but in large watersheds, the effects on the soil loss estimates have yet to be tested. Therefore, the objective of this study was to evaluate the effect of discretization on the hillslope sediment yield estimates using GeoWEPP in two large watersheds (>10 km2). The watersheds were selected and discretized varying the TOPAZ parameters [critical source area (CSA) and minimum source channel length (MSCL)] in a 30‐m resolution digital elevation model. The drainage networks built with TOPAZ were compared with each other using the drainage density index. The results showed that the discretization affected hillslope sediment yield estimates and their spatial distribution more than the total runoff. The drainage density index and the hillslope sediment yield were proportional but inversely related; thus, soil loss estimates were highly affected by the spatial discretization. As a result of this analysis, a method to choose the CSA and MSCL values that generates the greatest fraction of hillslopes having profile lengths less than 200 m was developed. This slope length condition is particularly crucial when using the WEPP and GeoWEPP models, in order for them to produce realistic estimates of sheet and rill erosion. Finally, and as a result of this analysis, a more reliable method was developed for selecting the TOPAZ channel network parameters (CSA and MSCL). Copyright © 2015 John Wiley & Sons, Ltd. 相似文献
19.
20.
Athena Coustenis Alberto Negrão Alberto Salama Emmanuel Lellouch Pierre Drossart Bernard Schmitt Andrei Nikitin 《Icarus》2006,180(1):176-185
The near-infrared spectrum of Titan, Saturn's largest moon and one of the Cassini/Huygens' space mission primary targets, covers the 0.8 to 5 micron region in which it shows several weak CH4 absorption regions, and in particular one centered near 2.75 micron. Due to the interference of telluric absorption, only part of this window region (2.9-3.1 μm) has previously been observed from the ground [Noll, K.S., Geballe, T.R., Knacke, R., Pendleton, F., Yvonne, J., 1996. Icarus 124, 625-631; Griffith, C.A., Owen, T., Miller, G.A., Geballe, T., 1998. Nature 395, 575-578; Griffith, C.A., Owen, T., Geballe, T.R., Rayner, J., Rannou, P., 2003. Science 300, 628-630; Geballe, T.R., Kim, S.J., Noll, K.S., Griffith, C.A., 2003. Astrophys. J. 583, L39-L42]. We report here on the first spectroscopic observations of Titan covering the whole 2.4-4.9 μm region by two instruments on board the Infrared Space Observatory (ISO) in 1997. These observations show the 2.75-μm window in its complete extent for the first time. In this study we have also used a high-resolution Titan spectrum in the 2.9-3.6 μm region taken with the Keck [Geballe, T.R., Kim, S.J., Noll, K.S., Griffith, C.A., 2003. Astrophys. J. 583, L39-L42; Kim, S.J., Geballe, T.R., Noll, K.S., Courtin, R., 2005. Icarus 173, 522-532] to infer information on the atmospheric parameters (haze extinction, single scattering albedo, methane abundance, etc.) by fitting the methane bands with a detailed microphysical model of Titan's atmosphere (updated from Rannou, P., McKay, C.P., Lorenz, R.D., 2003. Planet. Space Sci. 51, 963-976). We have included in this study an updated version of a database for the CH4 absorption coefficients [STDS, Wenger, Ch., Champion, J.-P., 1998. J. Quant. Spectrosc. Radiat. Transfer 59, 471-480. See also http://www.u-bourgogne.fr/LPUB/TSM/sTDS.html for latest updates; Boudon, V., Champion, J.-P., Gabard, T., Loëte, M., Michelot, F., Pierre, G., Rotger, M., Wenger, Ch., Rey, M., 2004. J. Mol. Spectrosc. 228, 620-634]. For the atmosphere we find that (a) the haze extinction profile that best matches the data is one with higher (by 40%) extinction in the atmosphere with respect to Rannou et al. (2003) down to about 30 km where a complete cut-off occurs; (b) the methane mixing ratio at Titan's surface cannot exceed 3% on a disk-average basis, yielding a maximum CH4 column abundance of 2.27 km-am in Titan's atmosphere. From the derived surface albedo spectrum in the 2.7-3.08 micron region, we bring some constraints on Titan's surface composition. The albedo in the center of the methane window varies from 0.01 to 0.08. These values, compared to others reported in the other methane windows, show a strong compatibility with the water ice spectrum in the near-infrared. Without confirming its existence from this work alone, our data then appear to be compatible with water ice. A variety of other ices, such as CO2, NH3, tholin material or hydrocarbon liquid cannot be excluded from our data, but an additional unidentified component with a signature around 2.74 micron is required to satisfy the data. 相似文献