A salt-water reservoir as the source of a compositionally stratified plume on Enceladus

The discovery of a plume of water vapour and ice particles emerging from warm fractures ('tiger stripes') in Saturn's small, icy moon Enceladus raised the question of whether the plume emerges from a subsurface liquid source or from the decomposition of ice. Previous compositional analyses of particles injected by the plume into Saturn's diffuse E ring have already indicated the presence of liquid water, but the mechanisms driving the plume emission are still debated. Here we report an analysis of the composition of freshly ejected particles close to the sources. Salt-rich ice particles are found to dominate the total mass flux of ejected solids (more than 99 per cent) but they are depleted in the population escaping into Saturn's E ring. Ice grains containing organic compounds are found to be more abundant in dense parts of the plume. Whereas previous Cassini observations were compatible with a variety of plume formation mechanisms, these data eliminate or severely constrain non-liquid models and strongly imply that a salt-water reservoir with a large evaporating surface provides nearly all of the matter in the plume.     

Water vapour and hydrogen in the terrestrial-planet-forming region of a protoplanetary disk

Planetary systems (ours included) formed in disks of dust and gas around young stars. Disks are an integral part of the star and planet formation process, and knowledge of the distribution and temperature of inner-disk material is crucial for understanding terrestrial planet formation, giant planet migration, and accretion onto the central star. Although the inner regions of protoplanetary disks in nearby star-forming regions subtend only a few nano-radians, near-infrared interferometry has recently enabled the spatial resolution of these terrestrial zones. Most observations have probed only dust, which typically dominates the near-infrared emission. Here I report spectrally dispersed near-infrared interferometric observations that probe the gas (which dominates the mass and dynamics of the inner disk), in addition to the dust, within one astronomical unit (1 au, the Sun-Earth distance) of the young star MWC 480. I resolve gas, including water vapour and atomic hydrogen, interior to the edge of the dust disk; this contrasts with results of previous spectrally dispersed interferometry observations. Interactions of this accreting gas with migrating planets may lead to short-period exoplanets like those detected around main-sequence stars. The observed water vapour is probably produced by the sublimation of migrating icy bodies, and provides a potential reservoir of water for terrestrial planets.     

矿热炉塌料过程中烟尘扩散的数值模拟

以铁合金生产车间为研究对象,利用Fluent软件对车间内矿热炉生产过程中塌料事故的烟尘扩散规律进行非稳态的数值模拟.对连续相和离散相,分别采用标准k～ε模型和DPM模型,分析不同风速和风向的烟尘扩散规律.研究结果表明:当风速在2 m/s以下时,南风能更有效地排除烟尘,并且风速越大,清洁作用越明显;当塌料事故结束时,不论何种风速或风向,车间内烟尘污染面积达到最大;在300 s且无风时最大烟尘质量浓度是风速为4 m/s时的36.6倍;车间内的死角是烟尘最难排出的地方,北风风速为0.2 m/s的最大停留时间长达4 800 s.     

山东小清河流域黄土的发现及勘探意义

通过钻孔取样、野外考察、粒度分析等方法对山东小清河流域浅层的沉积物特征进行研究。结果表明:小清河流域南部浅层沉积物以泥质粉砂和粉砂质泥为主,富含钙质结核和蜗牛化石等黄土标志物,发育明显的黄土-古土壤沉积旋回;南部粒度特征与青州黄土、北京降尘、西峰黄土等典型的风成沉积物相似,具有中国黄土的典型双峰特征,粒度分布明显粗于北京降尘和西峰黄土,而与邻近的青州黄土相似或较其稍粗,体现近物源的特性;末次冰期时裸露的渤海陆架是研究区黄土的主要物源区,中国东部季风和流域以南的山脉为黄土的形成提供搬运动力和地形条件;流域最北端发育古河道沉积,黄土与古河道间存在一个过渡带,沉积特征的差异和流域内南高北低的地势致使南部潜水面深度远大于北部,最终导致油气地震勘探中北部的地震激发效果明显优于南部。     

焊后多次正火对超细晶粒钢热影响区组织与硬度的影响

为研究400 MPa级超细晶粒钢焊接接头热影响区粗晶区的晶粒细化行为,对其空冷与水冷接头均进行了3次焊后正火热处理.组织观察表明:第1次正火后粗晶区晶粒明显细化,但细晶区和母材区的晶粒均比正火前的稍微粗大,第2次与第3次正火并不能进一步细化晶粒;冷却条件对热影响区组织的影响并不十分显著.显微硬度测试表明:第1次正火使接头硬度大幅度降低,甚至低于母材的原始硬度,后续正火对硬度的影响较小;在所有试样中,仅水冷接头第1次正火后的热影响区硬度与原始母材及母材区的硬度接近.由于焊后多次正火并不能使热影响区晶粒进一步细化,反而使其有粗化与软化的趋势,故应避免焊后多次正火处理.     

Detection of carbonates in dust shells around evolved stars.

Carbonates on large Solar System bodies like Earth and Mars (the latter represented by the meteorite ALH84001) form through the weathering of silicates in a watery (CO3)2- solution. The presence of carbonates in interplanetary dust particles and asteroids (again, represented by meteorites) is not completely understood, but has been attributed to aqueous alteration on a large parent body, which was subsequently shattered into smaller pieces. Despite efforts, the presence of carbonates outside the Solar System has hitherto not been established. Here we report the discovery of the carbonates calcite and dolomite in the dust shells of evolved stars, where the conditions are too primitive for the formation of large parent bodies with liquid water. These carbonates, therefore, are not formed by aqueous alteration, but perhaps through processes on the surfaces of dust or ice grains or gas phase condensation. The presence of carbonates which did not form by aqueous alteration suggests that some of the carbonates found in Solar System bodies no longer provide direct evidence that liquid water was present on large parent bodies early in the history of the Solar System.     

奥氏体变形及冷却速率对低碳贝氏体组织中大角晶界分布的影响

使用电子背散射衍射技术研究了低C高Mn高Nb成分设计下,非再结晶奥氏体变形及加速冷却速率对低碳贝氏体组织取向差特征和大角晶界分布的影响.结果表明,与原奥氏体晶粒内部的相变组织相比,原奥氏体晶界附近具有更高的大角晶界密度,非再结晶区奥氏体变形及快速冷却都有利于提高共格相变的驱动力、弱化变体选择以及有效增加大角晶界密度.此外,非再结晶区的大变形除了可充分压扁奥氏体晶粒和增加单位面积的奥氏体晶界密度外,还导致奥氏体晶界上细小的非共格转变铁素体晶粒生成,且这些铁素体晶粒与相邻组织表现出大取向差.     

Shear heating as the origin of the plumes and heat flux on Enceladus

Enceladus, a small icy satellite of Saturn, has active plumes jetting from localized fractures ('tiger stripes') within an area of high heat flux near the south pole. The plume characteristics and local high heat flux have been ascribed either to the presence of liquid water within a few tens of metres of the surface, or the decomposition of clathrates. Neither model addresses how delivery of internal heat to the near-surface is sustained. Here we show that the most likely explanation for the heat and vapour production is shear heating by tidally driven lateral (strike-slip) fault motion with displacement of approximately 0.5 m over a tidal period. Vapour produced by this heating may escape as plumes through cracks reopened by the tidal stresses. The ice shell thickness needed to produce the observed heat flux is at least 5 km. The tidal displacements required imply a Love number of h2 > 0.01, suggesting that the ice shell is decoupled from the silicate interior by a subsurface ocean. We predict that the tiger-stripe regions with highest relative temperatures will be the lower-latitude branch of Damascus, Cairo around 60 degrees W longitude and Alexandria around 150 degrees W longitude.     

A 'dry' condensation origin for circumstellar carbonates

The signature of carbonate minerals has long been suspected in the mid-infrared spectra of various astrophysical environments such as protostars. Abiogenic carbonates are considered as indicators of aqueous mineral alteration in the presence of CO2-rich liquid water. The recent claimed detection of calcite associated with amorphous silicates in two planetary nebulae and protostars devoid of planetary bodies questions the relevance of this indicator; but in the absence of an alternative mode of formation under circumstellar conditions, this detection remains controversial. The main dust component observed in circumstellar envelopes is amorphous silicates, which are thought to have formed by non-equilibrium condensation. Here we report experiments demonstrating that carbonates can be formed with amorphous silicates during the non-equilibrium condensation of a silicate gas in a H2O-CO2-rich vapour. We propose that the observed astrophysical carbonates have condensed in H2O(g)-CO2(g)-rich, high-temperature and high-density regions such as evolved stellar winds, or those induced by grain sputtering upon shocks in protostellar outflows.     

Identification of iron sulphide grains in protoplanetary disks

Sulphur is depleted in cold dense molecular clouds with embedded young stellar objects, indicating that most of it probably resides in solid grains. Iron sulphide grains are the main sulphur species in cometary dust particles, but there has been no direct evidence for FeS in astronomical sources, which poses a considerable problem, because sulphur is a cosmically abundant element. Here we report laboratory infrared spectra of FeS grains from primitive meteorites, as well as from pyrrhotite ([Fe, Ni](1-x)S) grains in interplanetary dust, which show a broad FeS feature centred at approximately 23.5 micrometres. A similar broad feature is seen in the infrared spectra of young stellar objects, implying that FeS grains are an important but previously unrecognized component of circumstellar dust. The feature had previously been attributed to FeO. The observed astronomical line strengths are generally consistent with the depletion of sulphur from the gas phase, and with the average Galactic sulphur/silicon abundance ratio. We conclude that the missing sulphur has been found.     

源库处理对两种不同穗型水稻品种籽粒灌浆的影响

选用直立穗型水稻品种辽粳454和弯曲穗品种辽开79在相同栽培条件下，通过剪叶、疏花处理改变源库关系，比较源库处理对两种不同穗型水稻品种籽粒灌浆的影响．结果表明：正常情况下，直立穗品种源的供应能力强，能够充分满足籽粒灌浆的需要，与直立穗品种比较，弯曲穗品种源的供应能力较弱．减源时，二者的强、弱颖花的灌浆都会受到不同程度的影响，其中直立穗品种弱势颖花所受影响大，而弯曲穗品种甚至强势颖花也受到了影响．疏花处理对辽粳454的强势籽粒影响不大，却使其弱势籽粒的灌浆得到很大改善；对辽开79的强、弱势粒都有很大影响．源库处理对两品种的强势粒籽粒重影响不大，但对弱势粒籽粒重影响较大．     

Low-temperature crystallization of silicate dust in circumstellar disks.

Silicate dust in the interstellar medium is observed to be amorphous, yet silicate dust in comets and interplanetary dust particles is sometimes partially crystalline. The dust in disks that are thought to be forming planets around some young stars also appears to be partially crystalline. These observations suggest that as the dust goes from the precursor clouds to a planetary system, it must undergo some processing, but the nature and extent of this processing remain unknown. Here we report observations of highly crystalline silicate dust in the disks surrounding binary red-giant stars. The dust was created in amorphous form in the outer atmospheres of the red giants, and therefore must be processed in the disks to become crystalline. The temperatures in these disks are too low for the grains to anneal; therefore, some low-temperature process must be responsible. As the physical properties of the disks around young stars and red giants are similar, our results suggest that low-temperature crystallization of silicate grains also can occur in protoplanetary systems.     

Grains and grain boundaries in single-layer graphene atomic patchwork quilts

The properties of polycrystalline materials are often dominated by the size of their grains and by the atomic structure of their grain boundaries. These effects should be especially pronounced in two-dimensional materials, where even a line defect can divide and disrupt a crystal. These issues take on practical significance in graphene, which is a hexagonal, two-dimensional crystal of carbon atoms. Single-atom-thick graphene sheets can now be produced by chemical vapour deposition on scales of up to metres, making their polycrystallinity almost unavoidable. Theoretically, graphene grain boundaries are predicted to have distinct electronic, magnetic, chemical and mechanical properties that strongly depend on their atomic arrangement. Yet because of the five-order-of-magnitude size difference between grains and the atoms at grain boundaries, few experiments have fully explored the graphene grain structure. Here we use a combination of old and new transmission electron microscopy techniques to bridge these length scales. Using atomic-resolution imaging, we determine the location and identity of every atom at a grain boundary and find that different grains stitch together predominantly through pentagon-heptagon pairs. Rather than individually imaging the several billion atoms in each grain, we use diffraction-filtered imaging to rapidly map the location, orientation and shape of several hundred grains and boundaries, where only a handful have been previously reported. The resulting images reveal an unexpectedly small and intricate patchwork of grains connected by tilt boundaries. By correlating grain imaging with scanning probe and transport measurements, we show that these grain boundaries severely weaken the mechanical strength of graphene membranes but do not as drastically alter their electrical properties. These techniques open a new window for studies on the structure, properties and control of grains and grain boundaries in graphene and other two-dimensional materials.     

轴流导叶式旋风管内气固两相流的实验研究

为研究颗粒分离机理,提高分离性能,采用五孔球探针测试仪及等动采样法对轴流导叶式旋风管内气固两相流速度与压力分布进行了测量,并分别对不同导流锥和排尘结构参数下的纯气流流场及颗粒浓度场分布进行了对比分析。实验结果表明,旋风管内气流切向速度分布呈典型的准Rankin涡结构,固相颗粒分布在离心力作用下沿径向分为近壁的密相区与中心的稀相区。减小导流锥下口内径,采用带有排尘侧缝的单锥排尘结构有利于旋风管内颗粒的分离。     

粮食伴生粉尘最低着火温度的实验研究

按照IEC标准建立了工业粉尘云和粉尘层最低着火温度(MIT)测试装置,对8种取自工业现场的粮食伴生粉尘进行了粉尘云和粉尘层MIT实验测试,并对灰分、粒径、水分对MIT的影响进行了实验研究和分析·发现粮食储运系统后期工艺比早期危险,按照粮食精粉或淀粉实验数据进行工业实际防爆设计的安全裕度过大,并提出了可行的防爆温度组别·所得结论为粮食行业的防爆设备选型提供了实验依据,对于粉尘着火和爆炸危险性评价具有借鉴意义·     

A close halo of large transparent grains around extreme red giant stars

An intermediate-mass star ends its life by ejecting the bulk of its envelope in a slow, dense wind. Stellar pulsations are thought to elevate gas to an altitude cool enough for the condensation of dust, which is then accelerated by radiation pressure, entraining the gas and driving the wind. Explaining the amount of mass loss, however, has been a problem because of the difficulty of observing tenuous gas and dust only tens of milliarcseconds from the star. For this reason, there is no consensus on the way sufficient momentum is transferred from the light from the star to the outflow. Here we report spatially resolved, multiwavelength observations of circumstellar dust shells of three stars on the asymptotic giant branch of the Hertzsprung-Russell diagram. When imaged in scattered light, dust shells were found at remarkably small radii (less than about two stellar radii) and with unexpectedly large grains (about 300 nanometres in radius). This proximity to the photosphere argues for dust species that are transparent to the light from the star and, therefore, resistant to sublimation by the intense radiation field. Although transparency usually implies insufficient radiative pressure to drive a wind, the radiation field can accelerate these large grains through photon scattering rather than absorption--a plausible mass loss mechanism for lower-amplitude pulsating stars.     

三相淤浆床中合成气直接合成二甲醚双功能混合催化剂的失活研究

用双功能混合催化剂在三相淤浆床反应器中进行合成气直接合成二甲醚,考察双功能混合催化剂在三相床中的稳定性和失活现象。探讨了合成气含水蒸气对合成二甲醚以及合成甲醇的影响。分析了三相淤浆床反应器中直接合成二甲醚催化剂的失活原因,认为反应中生成的水是催化剂活性降低的原因之一。氨的程序升温脱附、X射线衍射、X光电子能谱表征结果证实甲醇合成催化剂中活性组分Cu晶粒的长大及甲醇合成催化剂中Cu元素流失导致双功能催化剂活性降低。     

An early extrasolar planetary system revealed by planetesimal belts in beta Pictoris

beta Pictoris (beta Pic) is a main-sequence star with an edge-on dust disk that might represent a state of the early Solar System. The dust does not seem to be a remnant from the original protoplanetary disk, but rather is thought to have been generated from large bodies like planetesimals and/or comets. The history and composition of the parent bodies can therefore be revealed by determining the spatial distribution, grain size, composition and crystallinity of the dust through high-resolution mid-infrared observations. Here we report that the sub-micrometre amorphous silicate grains around beta Pic have peaks in their distribution around 6, 16 and 30 au (1 au is the Sun-Earth distance), whereas the crystalline and micrometre-sized amorphous silicate grains are concentrated in the disk centre. As sub-micrometre grains are blown quickly out from the system by radiation pressure from the central star, the peaks indicate the locations of ongoing dust replenishment, which originates from ring-like distributions of planetesimals or 'planetesimal belts'.     

No evidence for thick deposits of ice at the lunar south pole

Shackleton crater at the Moon's south pole has been suggested as a possible site of concentrated deposits of water ice, on the basis of modelling of bi-static radar polarization properties and interpretations of earlier Earth-based radar images. This suggestion, and parallel assumptions about other topographic cold traps, is a significant element in planning for future lunar landings. Hydrogen enhancements have been identified in the polar regions, but these data do not identify the host species or its local distribution. The earlier Earth-based radar data lack the resolution and coverage for detailed studies of the relationship between radar scattering properties, cold traps in permanently shadowed areas, and local terrain features such as the walls and ejecta of small craters. Here we present new 20-m resolution, 13-cm-wavelength radar images that show no evidence for concentrated deposits of water ice in Shackleton crater or elsewhere at the south pole. The polarization properties normally associated with reflections from icy surfaces in the Solar System were found at all the observed latitudes and are strongly correlated with the rock-strewn walls and ejecta of young craters, including the inner wall of Shackleton. There is no correlation between the polarization properties and the degree of solar illumination. If the hydrogen enhancement observed by the Lunar Prospector orbiter indicates the presence of water ice, then our data are consistent with the ice being present only as disseminated grains in the lunar regolith.     

百叶窗对静电除尘器二次扬尘的抑制效应

提出了一种旨在削弱或消除静电除尘器(Electrostatic precipitator,简称ESP)振打形成的二次扬尘现象,借以提高ESP的粉尘捕集效率。建立了静电除尘器电晕电场,流场,颗粒荷电及运动场的二维数值模型,借助有限元软件Comsolmultiphysics进行模拟计算,模拟结果与已公开的电晕电场和除尘效率的实验结果吻合较好。通过添加百叶窗结构在阳极板前形成有效的静止空间,保证在振打清灰时颗粒不与主气流混合,降低二次扬尘。分析了3种不同结构的百叶窗结构,并对百叶窗布置形成进行优化。结果表明：添加百叶窗结构能够降低收尘极板附近气流流速在0.1m/s以下;耦合电场、流场、颗粒荷电运动场可以得出,添加百叶窗后,颗粒被捕集时的速度小于0.2m/s,能够有效的控制二次扬尘,提高除尘器的除尘效率。