The activity coefficients of Fe(III) hydroxide complexes in NaCl and NaClO₄ solutions     

Frank J. Millero  Denis Pierrot 《Geochimica et cosmochimica acta》2007,71(20):4825-4833

The osmotic coefficients of FeCl₃ at 25 °C from 0.15 to 1.7 m [Rumyantsev et al., Z. Phys. Chem., 218, 1089-1127, 2004] have been used to determine the Pitzer parameters (β⁽⁰⁾, β⁽¹⁾ and C^?) for FeCl₃. Since the differences in the Pitzer coefficients of rare earths in NaCl and NaClO₄ are small, the values of Fe(ClO₄)₃ have been estimated using the differences between La(ClO₄)₃ and LaCl₃. The Pitzer coefficients for FeCl₃ combined with enthalpy and heat capacity data for the rare earths can be used to estimate the activity coefficients of Fe³⁺ in NaCl over a wide range of temperatures (0 to 50 °C) and ionic strength (0 to 6 m).The activity coefficients of Fe³⁺ in NaCl and NaClO₄ solutions have been used to determine the activity coefficients of Fe(OH)²⁺ in these solutions from the measured first hydrolysis constants of Fe³⁺ [Byrne et al., Mar. Chem., 97, 34-48, 2005]. The activity coefficients of , Fe(OH)₃ and from 0 to 50 °C have also been determined from the solubility measurements of Fe(III) in NaCl solutions [Liu and Millero, Geochim. Cosmochim Acta, 63, 3487-3497, 1999]. These activity coefficients have been fitted to the Pitzer equations. These results can be used to estimate the speciation of Fe(III) with OH⁻ in natural waters with high concentrations of NaCl from 0 to 50 °C.  相似文献   

Bias in hydraulic head measurements from multilevel vibrating-wire piezometers with excessively permeable backfill     

Young  Nathan L.  Lemieux  Jean-Michel  Locat  Pascal  Demers  Denis  Delottier  Hugo  Mony  Laura 《Hydrogeology Journal》2022,30(4):1337-1344

Hydrogeology Journal - An extensive network of multilevel vibrating-wire piezometers (VWP) was recently created to monitor the spatial and temporal variation of pore pressure (and hydraulic head)...  相似文献   

Characterization of karst systems using SIc-Pco2 method coupled with PCA and frequency distribution analysis. Application to karst systems in the Vaucluse county (Southeastern France)     

S. Minvielle  R. Lastennet  A. Denis  N. Peyraube 《Environmental Earth Sciences》2015,74(12):7593-7604

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Quantified,multi-scale X-ray fluorescence element mapping using the Maia detector array: application to mineral deposit studies     

Louise A. Fisher  Denis Fougerouse  James S. Cleverley  Christopher G. Ryan  Steven Micklethwaite  Angela Halfpenny  Robert M. Hough  Mary Gee  David Paterson  Daryl L. Howard  Kathryn Spiers 《Mineralium Deposita》2015,50(6):665-674

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Influence d'un changement climatique dû à une hausse de gaz à effet de serre sur l'agriculture au quebec     

Bhawan Singh  Mustapha El Maayar  Pierre André  Jean‐Pierre Thouez  Christopher Bryant  Denis Provençal 《大气与海洋》2013,51(2):379-399

Abstract

This study, using a climate change scenario generated by the Canadian Climate Centre (CCC) general circulation model (GCM) examines the impacts of such a climate change on agriculture in southern Quebec. Using a crop model from the Food and Agriculture Organization (FAO), yield responses of a variety of cereals, legumes, oleaginous and special crops to climate change are analysed and discussed.

Results show that under the 2 × CO₂ climate scenario the growing season would be longer and accumulation of corn heat units and growing degree days would be more important than under actual climate (1961–1990). One of the more important results of this study is that, on the one hand yield of C₃ cereals would be lower and that of C₄ cereals higher in most agricultural regions. On the other hand, the direct fertilisation effect of increased CO₂ is not considered. It must be cautioned however that we can not generalise results obtained for one legume crop to all legumes.  相似文献   

A search for evidence of critical internal wave reflection on the continental rise and slope off Nova Scotia     

Denis Gilbert 《大气与海洋》2013,51(1):99-122

Abstract

According to linear inviscid theory, the reflection of internal waves off a uniformly sloping bottom should lead to greatly enhanced energy density, and a cross‐isobath alignment of motions, near the critical frequency ω_c for which the wave ray slope equals the bottom slope. Current‐meter data from the continental rise and slope off Nova Scotia are used to test this hypothesis. Near‐bottom energy enhancement at ω_c was found to be significant at the 95% level for 8 out of 30 tests performed, whereas cross‐isobath alignment of motions near ω_c was significant at the 95% level for 10 out of 15 tests performed. Some aspects of the observations that appear to be consistent with non‐linear reflection theory are briefly discussed.  相似文献   

Acidification of Lower St. Lawrence Estuary Bottom Waters     

Alfonso Mucci  Michel Starr  Denis Gilbert  Bjorn Sundby 《大气与海洋》2013,51(3):206-218

Accumulation of metabolic CO₂ can acidify marine waters above and beyond the ongoing acidification of the ocean by anthropogenic CO₂. The impact of respiration on carbonate chemistry and pH is most acute in hypoxic and anoxic basins, where metabolic CO₂ accumulates to high concentrations. The bottom waters of the Lower St. Lawrence Estuary (LSLE), where persistently severe hypoxia has developed over the last 80 years, is one such case. We have reconstructed the evolution of pH in the bottom waters from historical and recent data, and from first principles relating the stoichiometry of CO₂ produced to oxygen consumed during microbial degradation of organic matter. Based on the value of the atmospheric partial pressure of CO₂ that best reproduces the preformed dissolved inorganic carbon concentration in the bottom waters, we estimate the average ventilation age of the bottom waters to be 16?±?3 years. The pH of the bottom waters has decreased by 0.2 to 0.3 over the last 75 years, which is four to six times greater than can be attributed to the uptake of anthropogenic CO₂. The pH decrease is accompanied by a decline in the saturation state with respect to both calcite and aragonite. As of 2007, bottom waters in the LSLE are slightly supersaturated with respect to calcite (Ω_c?≈?1.06?±?0.04) but are strongly undersaturated with respect to aragonite (Ω_a?≈?0.67?±?0.03).

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小型激光天文动力学空间计划概念   总被引：1，自引：0，他引：1  

倪维斗  朱进  武向平  褚桂柏  杨彬  高健  关敏  汤健仁  周翊  张中豪  黄天衣  曲钦岳  易照华  李广宇  陶金河  吴岸明  罗俊  叶贤基  周泽兵  熊耀恒  毕少兰  须重明  吴雪君  唐孟希  包芸  李芳昱  黄珹  杨福民  叶叔华  张书练  张元仲  聂玉昕  陈光  Joergen Christensen-Dalsgaard  Hansjoerg Dittus  Yasunori Fujii  Claus Laemmerzahl  Jean Francois Mangin  Achim Peters  Albrecht Ruediger  Etienne Samain  Stephan Schiller 《天文研究与技术》2002,(3):123-136

小型激光天文动力学空间计划是 :使用在太阳轨道上无拖曳航天器和地面站以激光干涉和脉冲测距的方法 ,精确地探讨天文动力学 ,检测相对论与时空基本定律 ,改进探测引力波的灵敏度以及更准确地测定太阳、行星和小行星的参数。 1 969年开始的月球激光 (反射 )测距 ,对地球物理、参考坐标的选定、相对论的检验均有重要的贡献。 3 0年来 ,激光技术的长足进步 ,使现在正是适合于开始进行研究空间有源 (主动 )测距和光波空间通讯的时候。激光天文动力学的兴起是必然的趋势 ,其精确度将比现在提高 3到 6个数量级 ,将是天文动力学革命性的发展。小型激光天文动力学空间计划可以起到带头作用。它的关键技术有三 ,即 :弱光锁相、极精确无拖曳航天和高衰减日冕仪。弱光锁相已有长足的进步。对高衰减日冕仪的研究 ,也有了初步的方案。LISA空间计划将于 2 0 0 6年 8月发射SMART -2 ,研究测试极精确无拖曳航天。小型激光天文动力学空间计划的关键技术已日趋成熟。在第一届国际激光天文动力学研讨会 ( 2 0 0 1 ,9.1 3 -2 3 )中介绍了各相关学科背景及前沿研究 ,讨论了激光天文动力学空间计划科学目标及相关技术 ,并召开了两次小型激光天文动力学空间计划预研究筹备会 ,建立了和欧洲的合作关系。会后着手进行此项对基础  相似文献   

Multiwavelength focusing with the Sun as gravitational lens     

Laurent Koechlin  Denis Serre  Gerald K. Skinner  Peter Von Ballmoos  Thomas Crouzil 《Experimental Astronomy》2005,20(1-3):307-315

The light deviation caused by the gravitational potential in the vicinity of the sun could be used as a means of focussing radiation that cannot be focussed easily otherwise. The gravitational lens formed by the sun is not stigmatic, but does have the advantage of being achromatic and acts identically on all types of mass-less radiations. For a source at infinity, its geometrical characteristics present a “caustic” line starting at 550 astronomical units (UA) downstream from the sun. In a plane perpendicular to that caustic line, images of distant objects are formed.The perturbations by the solar corona plasma will significantly blur electromagnetic radiation for wavelengths longer than those of the IR domain. At shorter wavelengths, for example the γ domain, the focussing process could lead to 10⁸ amplification factors. In order to reach the regions where images are formed, long distance space missions are necessary. Once launched, missions of this type would be dedicated to a single field. Some possible targets are considered, such as Sagitarius A observed in X and γ rays.In this paper we study the point spread function (PSF) of the sun as a gravitational lens. Taking into account perturbations by the planets, the non sphericity of the sun and coronal plasma index, we derive limits within which such observations could be possible.  相似文献   

Multiwavelength study of X-ray selected star-forming galaxies within the Chandra Deep Field-South     

Daniel Rosa-González  Denis Burgarella  Kirpal Nandra  Daniel Kunth  Elena Terlevich †  Roberto Terlevich † 《Monthly notices of the Royal Astronomical Society》2007,379(1):357-369

We have combined multiwavelength observations of a selected sample of star-forming galaxies with galaxy evolution models in order to compare the results obtained for different star formation rate (SFR) tracers and to study the effect that the evolution of the star-forming regions has on them. We also aimed at obtaining a better understanding of the corrections due to extinction and nuclear activity on the derivation of the SFR. We selected the sample from Chandra data for the well studied region Chandra Deep Field -South (CDFS) and chose the objects that also have ultraviolet (UV) and infrared (IR) data from Galaxy Evolution Explorer ( GALEX ) and Great Observatories Origins Deep Survey (GOODS) Spitzer , respectively.
Our main finding is that there is good agreement between the extinction corrected SFR(UV) and the SFR(X), and we confirm the use of X-ray luminosities as a trustful tracer of recent star formation activity. Nevertheless, at SFR(UV) larger than about  5 M_⊙ yr⁻¹  there are several galaxies with an excess of SFR(X) suggesting the presence of an obscured active galactic nucleus (AGN) not detected in the optical spectra. We conclude that the IR luminosity is driven by recent star formation even in those galaxies where the SFR(X) is an order of magnitude higher than the SFR(UV) and therefore may harbour an AGN. One object shows SFR(X) much lower than expected based on the SFR(UV); this SFR(X) 'deficit' may be due to an early transient phase before most of the massive X-ray binaries were formed. An X-ray deficit could be used to select extremely young bursts in an early phase just after the explosion of the first supernovae associated with massive stars and before the onset of massive X-ray binaries.  相似文献