Indication of drier periods on Mars from the chemistry and mineralogy of atmospheric dust

The ubiquitous atmospheric dust on Mars is well mixed by periodic global dust storms, and such dust carries information about the environment in which it once formed and hence about the history of water on Mars. The Mars Exploration Rovers have permanent magnets to collect atmospheric dust for investigation by instruments on the rovers. Here we report results from M?ssbauer spectroscopy and X-ray fluorescence of dust particles captured from the martian atmosphere by the magnets. The dust on the magnets contains magnetite and olivine; this indicates a basaltic origin of the dust and shows that magnetite, not maghemite, is the mineral mainly responsible for the magnetic properties of the dust. Furthermore, the dust on the magnets contains some ferric oxides, probably including nanocrystalline phases, so some alteration or oxidation of the basaltic dust seems to have occurred. The presence of olivine indicates that liquid water did not play a dominant role in the processes that formed the atmospheric dust.     

兰州市大气降尘的化学特性

对定期收集的兰州市降尘样品,用X射线荧光法分析了其中24种元素的相对浓度,并用富集因子法对数据进行了处理,分析,结果表明兰州市现代降尘中主要有SiO2,Al2O3,CaO,铁的氧化物,MgO,Na2O,K2O,TiO2等,同时含有微量P,Mn,Zn,Ba,Pb等元素,从元素浓度的年内变化情况看,Fe,Co,Cu,Cr,As等元素在采暖期（11月－次年3月）浓度均高于非采暖期,Al,Si,Ca,Pb等元素浓度年内差异不大,而Na,Mg,K等元素浓度在采暖期明显降低,在降尘中富集程度最高的元素Zn,Pb,As主要来自人为污染,Si,Al,Mg,K,Na,V,Co,Ni则基本源于本地和邻近地区的土壤表土,Fe,Ca,Ti,P,Cu,Ba,Cr,Mn人为污染亦占有一定比例。     

大气降尘研究方法综述

通过阅览文献,对大气降尘领域的研究技术与方法进行了分类综述,包括尘样物质的收集、理化特性的分析、各种源解析技术以及降尘与TSP浓度的关系.最后对降尘研究领域存在的问题进行了概括并提出了展望.     

Outgassing from Amazonian rivers and wetlands as a large tropical source of atmospheric CO2

Terrestrial ecosystems in the humid tropics play a potentially important but presently ambiguous role in the global carbon cycle. Whereas global estimates of atmospheric CO2 exchange indicate that the tropics are near equilibrium or are a source with respect to carbon, ground-based estimates indicate that the amount of carbon that is being absorbed by mature rainforests is similar to or greater than that being released by tropical deforestation (about 1.6 Gt C yr-1). Estimates of the magnitude of carbon sequestration are uncertain, however, depending on whether they are derived from measurements of gas fluxes above forests or of biomass accumulation in vegetation and soils. It is also possible that methodological errors may overestimate rates of carbon uptake or that other loss processes have yet to be identified. Here we demonstrate that outgassing (evasion) of CO2 from rivers and wetlands of the central Amazon basin constitutes an important carbon loss process, equal to 1.2 +/- 0.3 Mg C ha-1 yr-1. This carbon probably originates from organic matter transported from upland and flooded forests, which is then respired and outgassed downstream. Extrapolated across the entire basin, this flux-at 0.5 Gt C yr-1-is an order of magnitude greater than fluvial export of organic carbon to the ocean. From these findings, we suggest that the overall carbon budget of rainforests, summed across terrestrial and aquatic environments, appears closer to being in balance than would be inferred from studies of uplands alone.     

兰州市冬季大气沉降尘粒度特征及来源解析

通过对兰州市冬季大气沉降尘颗粒的粒度分布特征及参数的分析,认识其可能来源及对环境的影响．从实验结果发现兰州市大气沉降尘粒径主要为10-50μm,各个采样点的PM2．5和PM10贡献突出,说明兰州市颗粒物污染严重．研究表明兰州市大气中可吸入颗粒物的来源主要为生活燃煤和汽车、工厂产生的废气;粒径〈50μm的颗粒物主要来源于空气搬运作用迁移而来的黄土粉尘等;粒径〉50μm的颗粒物主要是由人为引入或由特大尘暴使大颗粒物近源搬运的结果．不同的功能区中,工业区内污染最大,其次为生活区和其他区．从整体看兰州市的4个行政区内大气沉降尘粒度特征有较大的相似性,除了受生活、汽车、工业以及黄土高原的影响外,兰州城市整体布局存在较大缺陷,工业区和生活区混杂、密集。布局不合理．     

高斯-谢尔光束通过湍流大气任意粗糙目标的散射统计特性

基于广义惠更斯-菲涅耳原理和任意粗糙目标模型,考虑大气湍流对激光从发射机到目标和从目标到接收机的影响,研究部分相干高斯-谢尔光束经任意粗糙目标散射后的统计特性.我们假设相位结构函数占优,推导了接收场处互相关函数的表达式,平均强度以及波前相干长度大小,并对此进行数值模拟.结果表明,接收面的平均强度与粗糙面的横向相关长度与表面高度均方根有关;接收场的波前相干长度与湍流强度、表面粗糙度、传播距离和光源相干度有关.     

大型锅炉烟道电除尘监控系统的设计与实现

锅炉烟道电除尘监控系统使用现场总线技术和计算机网络技术,采用网桥模块将多个现场智能监控设备、上层以太网和可编程逻辑控制器互联,完成了基于现场总线和以太网远程监控与管理的功能。     

Charon's radius and atmospheric constraints from observations of a stellar occultation

The physical characteristics of Pluto and its moon, Charon, provide insight into the evolution of the outer Solar System. Although previous measurements have constrained the masses of these bodies, their radii and densities have remained uncertain. The observation of a stellar occultation by Charon in 1980 established a lower limit on its radius of 600 km (ref. 3) (later refined to 601.5 km; ref. 4) and suggested a possible atmosphere. Subsequent, mutual event modelling yielded a range of 600-650 km (ref. 5), corresponding to a density of 1.56 +/- 0.22 g cm(-3) (refs 2, 5). Here we report multiple-station observations of a stellar occultation by Charon. From these data, we find a mean radius of 606 +/- 8 km, a bulk density of 1.72 +/- 0.15 g cm(-3), and rock-mass fraction 0.63 +/- 0.05. We do not detect a significant atmosphere and place 3sigma upper limits on atmospheric number densities for candidate gases. These results seem to be consistent with collisional formation for the Pluto-Charon system in which the precursor objects may have been differentiated, and they leave open the possibility of atmospheric retention by the largest objects in the outer Solar System.     

Determining the ages of comets from the fraction of crystalline dust

The timescale for the accretion of bodies in the disk surrounding a young star depends upon a number of assumptions, but there are few observational constraints. In our own Solar System, measurements of meteoritic components can provide information about the inner regions of the nebula, but not the outer parts. Observations of the evolution of more massive protostellar systems (Herbig Ae/Be stars) imply that significant changes occur in the physical properties of their dust with time. The simplest explanation is that thermal annealing of the original, amorphous grains in the hot inner nebula slowly increases the fractional abundance of crystalline material over time. Crystalline dust is then transported outward, where it is incorporated into comets that serve as a long-term reservoir for dust disks, such as that surrounding Beta Pictoris. Here we show that when applied to our own Solar System, this process can explain observed variations in both the volatile and dusty components of comets, while also providing a natural indicator of a comet's mean formation age. Studies of comets with different dust contents can therefore be used to investigate the timescales of the early Solar System.     

High-velocity streams of dust originating from Saturn

High-velocity submicrometre-sized dust particles expelled from the jovian system have been identified by dust detectors on board several spacecraft. On the basis of periodicities in the dust impact rate, Jupiter's moon Io was found to be the dominant source of the streams. The grains become positively charged within the plasma environment of Jupiter's magnetosphere, and gain energy from its co-rotational electric field. Outside the magnetosphere, the dynamics of the grains are governed by the interaction with the interplanetary magnetic field that eventually forms the streams. A similar process was suggested for Saturn. Here we report the discovery by the Cassini spacecraft of bursts of high-velocity dust particles (> or = 100 km s(-1)) within approximately 70 million kilometres of Saturn. Most of the particles detected at large distances appear to originate from the outskirts of Saturn's outermost main ring. All bursts of dust impacts detected within 150 Saturn radii are characterized by impact directions markedly different from those measured between the bursts, and they clearly coincide with the spacecraft's traversals through streams of compressed solar wind.     

A large dust/ice ratio in the nucleus of comet 9P/Tempel 1

Comets spend most of their life in a low-temperature environment far from the Sun. They are therefore relatively unprocessed and maintain information about the formation conditions of the planetary system, but the structure and composition of their nuclei are poorly understood. Although in situ and remote measurements have derived the global properties of some cometary nuclei, little is known about their interiors. The Deep Impact mission shot a projectile into comet 9P/Tempel 1 in order to investigate its interior. Here we report the water vapour content (1.5 10(32) water molecules or 4.5 10(6) kg) and the cross-section of the dust (330 km2 assuming an albedo of 0.1) created by the impact. The corresponding dust/ice mass ratio is probably larger than one, suggesting that comets are 'icy dirtballs' rather than 'dirty snowballs' as commonly believed. High dust velocities (between 110 m s(-1) and 300 m s(-1)) imply acceleration in the comet's coma, probably by water molecules sublimated by solar radiation. We did not find evidence of enhanced activity of 9P/Tempel 1 in the days after the impact, suggesting that in general impacts of meteoroids are not the cause of cometary outbursts.     

高喷煤比时高炉炉尘灰中含碳物质研究

测定了高喷煤比的高炉炉尘(重力灰和瓦斯灰)中矿物组成,给出了在不同煤比条件下未消耗焦炭和煤粉面积比.分析了高喷煤比对高炉炉尘中碳质量分数和未消耗煤粉比例的影响.确定了宝钢高炉在高喷煤比时高炉炉尘中未消耗煤粉量、焦炭颗粒量和煤粉在高炉内的利用率.通过试验发现,随着喷煤比增加,炉尘量增加,但在高喷煤比后,炉尘量波动较大.高炉炉尘中未消耗碳量和煤粉量随着喷煤比的增加逐渐增加,而未消耗焦炭量不受喷煤比变化的影响,基本上保持在3 kg.t-1的水平,表明宝钢高炉焦炭品质很高.     

矿尘痕量元素在飘积土和地面土中的分布和识别

研究了黄铁矿采矿场12种矿样与采矿场附近降尘累积土(飘积土)和地面土中As、Cd、Co、Cr、Cu、Mo、Ni、Pb、Tl、Ba和Se的分布.将土壤学中元素比的概念引入痕量元素溯源,提出元素相似比和相似度2个概念,结合元素相关性识别飘积土和地面土中的来自矿尘的痕量元素.结果表明,在2.0～16.0 cm的飘积表土和地面表土中,大部分痕、微量元素的最低值均低于其背景值(<1 km地面土中Pb和>1 km地面土中Cd和Co除外),而平均值和最高值均高于背景值(飘积土中的Cu、Se的平均值、<1 km地面土中Cr、>1 km地面土中Cu和上述全部样品中的Ba除外).在18.0～36.0 cm的飘积心土和地面心土中,大部分痕、微量元素的最低值和平均值均高于背景值(飘积心土的Co、Cu、Se和>1 km地面心土Pb、Cu、Ba除外).痕、微量元素呈亚层积聚特征.同时,相关系数r>0.2的矿样元素,与飘积土和地面土至少有1个相似度>0.5的元素相似比,相关系数r≥0.54的矿样元素,与飘积土和地面土有2个以上相似度>0.5的元素相似比.据此可识别飘积土和地面土中的来自矿尘的痕量元素.     

Io as a source of the jovian dust streams

Streams of dust emerging from the direction of Jupiter were discovered in 1992 during the flyby of the Ulysses spacecraft, but their precise origin within the jovian system remained unclear. Further data collected by the Galileo spacecraft, which has been orbiting Jupiter since December 1995, identified the possible sources of dust as Jupiter's main ring, its gossamer ring, comet Shoemaker-Levy 9 (ref. 8) and Io. All but Jupiter's gossamer ring and Io have since been ruled out. Here we find that the dominant source of the jovian dust streams is Io, on the basis of periodicities in the dust impact signal. Io's volcanoes, rather than impact ejecta, are the dust sources.     

沙尘暴过程观测数据与实测数据的综合分析

不断加深沙尘暴起沙、传输、沉降机制及其辐射强迫机理认识,提高沙尘暴的预测预警以及防治水平,已成为科研界和政府部门共同关注的问题.我们充分利用已观测的数据进行了深入的综合研究和方法探索,在数据处理本身和多元数据分析方面均取得一些新进展.本文充分利用遥感观测和地面实测手段,对亚洲沙尘暴进行监测.通过对多元数据进行分析和综合,建立了遥感监测结果与地面观测结果之间的关联关系,这些监测结果能够为综合风侵蚀模型系统和GCM(全球尺度沙尘模拟模型)模型系统提供参数和验证数据,同时为沙尘暴的预警预报提供基础数据和客观依据.     

烧结电除尘灰浸出液分离制备球形碳酸钙的研究

对包钢烧结电除尘灰进行了浸出试验,研究结果表明浸出液中有较高含量的钾盐和钙盐。为了提升钾盐产品质量和降低硫酸钙结垢对设备安全操作的影响,在回收钾盐之前,需要对浸出液中的硫酸钙盐进行去除。以碳酸钠溶液为沉淀剂,考察了沉淀剂浓度、反应温度、搅拌强度和平衡时间对浸出液中硫酸钙的去除效果及碳酸钙产品晶型晶貌的影响。结果表明,钙离子去除率几乎达到100%,同时获得了粒径10μm左右、颗粒分散均匀、高附加值的球形碳酸钙副产品。     

Slip zone and energetics of a large earthquake from the Taiwan Chelungpu-fault Drilling Project

Determining the seismic fracture energy during an earthquake and understanding the associated creation and development of a fault zone requires a combination of both seismological and geological field data. The actual thickness of the zone that slips during the rupture of a large earthquake is not known and is a key seismological parameter in understanding energy dissipation, rupture processes and seismic efficiency. The 1999 magnitude-7.7 earthquake in Chi-Chi, Taiwan, produced large slip (8 to 10 metres) at or near the surface, which is accessible to borehole drilling and provides a rare opportunity to sample a fault that had large slip in a recent earthquake. Here we present the retrieved cores from the Taiwan Chelungpu-fault Drilling Project and identify the main slip zone associated with the Chi-Chi earthquake. The surface fracture energy estimated from grain sizes in the gouge zone of the fault sample was directly compared to the seismic fracture energy determined from near-field seismic data. From the comparison, the contribution of gouge surface energy to the earthquake breakdown work is quantified to be 6 per cent.