巷道支护的自稳平衡圈理论

基于软岩巷道围岩变形破坏的自稳平衡现象,通过数值模拟揭示了巷道顶板、两帮和底板之间的相互影响关系,得出了巷道围岩不稳定区是以巷道为中心的椭圆形。基于普氏理论,考虑“底板-两帮-顶板”相互影响,提出了巷道围岩自稳平衡圈理论,给出了自稳平衡圈的椭圆曲线方程,明确了巷道支护对象为自稳平衡圈内的岩体,支护的目的是控制自稳平衡圈岩体的稳定性。研究表明,“底板-两帮-顶板”共同构成巷道稳定性的整体系统,巷道顶板自稳平衡拱的大小随着两帮塑性区的增大而增大,两帮塑性区随底板变形而增大。加强底板和两帮的支护,将大大缩小顶板自稳平衡拱的高度。提出了“治顶先治帮,治帮先治底”的巷道支护理念,得到多年实践验证,为软岩巷道支护控制提供了新的依据。     

Search for and study of hot circumstellar dust envelopes

Long-term (1984–2008) JHKLM photometry for 254 objects is presented. The observations were carried out in the standard JHKLM photometric system using an original method and a modern IR photometer designed and built at the Sternberg Astronomical Institute. Our program of studies included searches for and studies of relatively hot circumstellar dust envelopes. The most important results obtained using these observations include the following. We have detected relatively hot dust envelopes in a number of objects for the first time, including the RCB star UV Cas, RX Cas, several classical symbiotic stars, etc. A model has been calculated for the dust envelope of FG Sge, which formed around the star as a result of several successive cycles of dust condensation beginning in Autumn 1992. Several dust-condensation episodes have been traced in the envelopes of symbiotic systems (CH Cyg, V1016 Cyg, HM Sge, etc.), as well as the role of the hot component in the formation of the dust envelopes. We have established from variations of the IR emission that the cool components in the symbiotic novae V1016 Cyg and HM Sge, and possibly CH Cyg, are Miras. The binarity of V1016 Cyg and HM Sge has also been firmly established. The variability of a whole series of object has been studied, including the stellar components of close binary systems and several dozen Mira and semi-regular variables. The ellipsoidality of the components in the RX Cas system (a prototype W Ser star) and the cool component in the symbiotic systems CI Cyg and BF Cyg has been firmly established. We have obtained the first IR light curve for the eclipsing system V444 Cyg (WN5+O6), and determined the wavelength dependence of the obtained parameters of the WN5 star. Analysis of the IR light curves of several novae indicate the condensation of dust envelopes in the transition periods of Cygnus 1992, Aquila 1993, and Aquila 1995. The IR light curve of R CrB has been obtained over a long period and analyzed. IR observations of the nova-like variable V4334 Sgr have been carried out over four years, over which the star passed through four stages during its motion along its post-AGB evolutionary track; the star’s bolometric flux and optical depth of its dust envelope have been estimated, and the structure and mass of the dust layer determined. We have analyzed the IR variability of the symbiotic star V407 Cyg over 14 years, and found its cool component to be a Mira with a period of 745 days. The observed pulsations and trend are associated with the luminosity and temperature variations of the Mira, as well as the optical depth of the dust envelope. The size of the dust grains and mass-loss rate of the Mira have been determined. We have obtained JHKL light curves for the Seyfert galaxy NGC 4151 over 23 years. The IR brightness of the galaxy grew from 1985 through 1996 (by ∼0.9 ^m at 1.25 μm, ∼1 ^m at 1.65 μm, ∼1.1 ^m at 2.2 μm, and ∼1.3 ^m at 3.5 μm), while the galaxy simultaneously reddened. The “cool” variable source in NGC 4151 was still in the active state in 1998, although its luminosity had decreased by approximately 15%–20%. If the “cool” component of the variable source in this galaxy is a dust envelope heated by the central “hot” source, it should be optically thin to the radiation of this source: its mean optical depth is in the range 0.05–0.15. Emission from dust particles heated to temperatures of 600–800 K was observed in the near IR at a distance of several parsecs from the nucleus during the period of activity in 1995–1998; the inferred mass of emitting dust was 5–20 M _⊙. In 1994–2003, we observed a tendency for NGC 4151 to become bluer at 1.25–1.65 μm while simultaneously reddening at 2.2–3.5 μm. Beginning in Autumn 2000, the galaxy began to emerge from a minimum, which lasted from March 2000 through April 2001 in the IR; a flare of the galactic nucleus was observed and followed in detail in the IR in this same period. We confirm the IR variability of the nucleus of the Seyfert galaxy NGC 1068, which can be located in various stages of activity. The variability of NGC 1068 is associated with a complex source. A periodic component has been detected in the J brightness variations of the oxygen Mira V2108 Oph; we have shown that this star is immersed in a fairly dense dust envelope, and have calculated amodel for this envelope. We have calculated an (axially symmetrical) dust-envelope model for the carbon semi-regular variable RWLMi with a density distribution characteristic for the “superwind” stage. This envelope model is able to reproduce the observed fluxes over the entire observable spectrum, and displays a good agreement with the observational data. The three hot supergiants V482 Cas, QZ Sge, and HD 338926 may be variable in the IR. Long-term photometry of eight planetary nebulae in the near IR (1.25–5 μm) has enabled us to firmly establish the IR brightness and color variability of these nebulae on time scales from several tens of days to six-to-eight years. We have analyzed long-term JK photometry of the X-ray binary Cyg X-1 (V1357 Cyg). Periodicity with a characteristic time scale of ∼11.5 years is visible in the JK brightness variations of Cyg X-1 in 1984–2007, possibly due to periodic variations of the temperature, radius and luminosity of the optical component of the binary with P ∼11.5 yr. Fourteen-year IR light curves of five RV Tau stars (R Sge, RV Tau, AC Her, V Vul, and R Sct) and the yellow supergiant and protoplanetary-nebula candidate V1027 Cyg have been analyzed. A spherically symmetrical dust-envelope model has been calculated for V1027 Cyg.     

一种改进的Delaunay三角化算法研究

Delaunay三角化在诸多应用领域具有极其广泛用途,也一直是计算机图形图像学和科学计算可视化技术的重要研究内容。针对二维约束Delaunay三角化问题,提出一种快速生成算法。该算法首先建立环形矩形,分环分治平面散乱点;然后依据Delaunay三角形的性质,从外环到内环分治逐步插入新点,一环插入完毕后,整理有效Delaunay三角形;依次循环快速生成二维约束Delaunay三角网格。本算法计算过程简单,计算效率高,程序编写十分容易无需复杂的递归过程,技巧性地解决了二维约束Delaunay三角化问题。实例证明,该算法具有较好的应用效果。     

树轮纤维素中氧同位素温度意义

树轮作为自然档案中的一种, 其同位素研究是较为新颖的领域文章比较系统地从树轮纤维素的提取、氧的来源、植物体内氧的分馏、与温度变化的关系等４ 个方面评述了树轮纤维素氧同位素组成的气候学意义已有的研究结果表明, 树轮纤维素氧同位素组成的变化是温度变化的良好载体, 但在定量恢复古温度变化时遇到了不少限制, 有待于进一步完善分馏模型     

地质全息论

以自然界中全息现象存在的普遍性为指导,以客观存在的地质现象为依据,从全息的角度来对地质现象进行分析,正式提出了地质全息理论,认为地质体形态、地质信息和地质活动的频率等其局部与整体之间具有相似性或对应性,而且这种"整体(全息系统)"和"局部(全息元)"是相对的,与实际大小无关。这三种全息分别称为地质形态全息、地质信息全息和地质时间全息。任何地质体都是地质历史中不同种类、不同级别的地质全息系统的先后和交互作用下的结果,因此在某种具体的地质对象研究中确定其主控全息系统及其级别就显得非常重要。地质全息理论可以为地质学相关研究提供一个全新的理论依据和参考手段。     

CFD simulation of blasting dust for the design of physical barriers

A computational fluid dynamics (CFD) model has been developed to simulate the dispersion of dust generated in blasting located in limestone quarries. This is a complex phenomenon that has been studied through the use of several digital video recordings of blasts and dust concentration field measurements by ‘light scattering’ dust collectors. In addition, the subsequent simulation of the dispersion of the dust cloud by means of multiphase CFD has also been studied. CFD calculations were carried out using software Ansys CFX 10.0, through transitory models with Lagrangian particle models crossing an Eulerian air continuous phase. This paper presents results obtained by model simulations where physical barriers are set close to the blasting, with the aim of decreasing the dust cloud dispersal and the associated environmental impact.     

Formation of planetary systems and brown dwarfs around single stars

The conditions for the formation of planets and brown dwarfs around single main-sequence stars are considered in two scenarios. The formation of planets and brown dwarfs requires that the initial specific angular momentum of a solar-mass protostar be (0.32)×10¹⁸ cm²/s. The accreted matter of the protostar envelope forms a compact gas ring (disk) around the young star. If the viscosity of the matter in this ring (disk) is small, increasing its mass above a certain limit results in gravitational instability and the formation of a brown dwarf. If the viscosity of the gas is sufficiently large, the bulk of the protostar envelope material will be accreted by the young star, and the gas disk will grow considerably to the size of a protoplanetary dust disk due to the conservation of angular momentum. The formation of dust in the cool part of the extended disk and its subsequent collisional coalescence ultimately results in the formation of solar-type planetary systems.     

The subaerial origin of mantle depositsZur subaerischen entstehung der decksedimenteL'origine subaérienne des formations de couverture

The authors deal with the problems of the origin of mantle formations consisting of loams and sandy loams that occur on the surface of Central and Eastern Europe. The loams are usually considered periglacial deposits; however, the authors have developed a new theory on the origin of these formations. In their opinion loams developed as a result of deposition of atmospheric dust. The new theory is supported by measurements of dust fall mainly on glaciers in the Caucasus and in Central Asia. The measurements correspond favorably with the absolute age of humus in the soils of the Russkaya ravnina (Lowland). Recently, dust fall has increased owing to activities by man. The increase disturbs the equilibrium in the subaerial lithogenesis — soil development system and therefore more attention should be given to this phenomenon.     

新疆艾比湖地区盐尘的沉积通量及其物质组成

以新疆准噶尔盆地西部的艾比湖地区为研究区,通过野外降尘监测、采样分析等方法,研究了艾比湖地区含盐粉尘的沉积通量和物质组成特征.结果表明:艾比湖干涸湖底是盐尘的输出源,盐尘的化学组成主要是无水芒硝、白钠镁矾、氯化钠等盐碱粉尘及Cr、Pb、Mn、Cu、Ni等潜在毒性元素.艾比湖地区盐尘的沉积通量约为79~381 g·m-2·a-1,盐的沉积通量约为4~61 g·m-2·a-1.盐尘的粒径分布以2~63μm的粉砂粒级为主,大于63μm的砂粒级所占比例很小.特殊的地形条件、大风天气、稀疏的植被覆盖、疏松的大面积尘源是艾比湖湖底风蚀和盐尘输送的有利条件.     

地壳运动整体观论纲

本文在全面讨论了构造体系与全球运动场、板块构造与旋转扩张、断块构造、镶嵌构造、地洼说与地球自转、构造迁移的方向性及地球水圈、气圈和生物圈的运动规律以后,提出了地球动力系统统一观,并进一步论述了包括重力、热力、离心惯性力等在内的地球动力系统中,地球自转和自转速度不均衡乃是发动地壳运动的主因,而地球整体的运动和变化,又受着天体活动的影响。
本文纲要性地指出,地壳上各种地质现象与相关的自然现象是一个有联系的整体,受控于地球整体的运动系统。      

Community mobilisation for improved livelihoods through tree crop management in Niger

Effective natural resource management requires interrelated technical practices and social arrangements that are appropriate to a region’s biophysical characteristics and that address protection and sustainable management of resources. This is illustrated from our experience in the Republic of Niger, West Africa. In 1980 barren plains, infertile soils, drought, dust storms, severe fodder shortages, and agricultural pest outbreaks were normal occurrences in Niger’s rural regions. In general, despite large investments of time and funding, conventional reforestation efforts had little impact. However by 2008 over five million hectares of once barren land had been transformed through wide adoption of an agroforestry method known as ‘Farmer Managed Natural Regeneration’ (FMNR), introduced in 1983. In the Aguie Department, the practice of FMNR was formalized through the Desert Community Initiative (DCI), addressing interrelated technical and social issues in resource management. New governance structures, which include marginalized groups, implement monitoring and enforcement systems enabling communities to manage land and regenerating trees. These, together with technical solutions that build on local knowledge and skills and use previously undervalued indigenous tree species, have generated a sustainable fuel-wood market for the first time. Increased linkage and compatibility between institutions at local and national levels and strengthened social capital have been crucial to these impacts. Food security and community resilience to drought have been markedly enhanced and local incomes have increased. The experience provides important lessons for approaches to addressing environmental degradation and poverty in other semi arid areas and facilitating the spread and adoption of new agroforestry systems.     

树轮气候学中树木年轮密度分析方法的研究进展

树木年轮密度（树轮密度）分析作为树轮气候学的一种研究方法,能够提取更准确的环境信息,应用范围更广,在过去环境变化研究中受到越来越广泛的重视。讨论了树轮密度测量技术与树轮密度分析方法在过去气候变化研究中的发展历程及最新研究成果,认为X射线分析法仍然是目前被广泛采用的树轮密度分析手段,基于树轮密度数据的过去温度变化重建仍是树轮密度研究的主要方向。相关研究表明：森林上限和高纬度地区树木年轮的最大晚材密度对夏季温度变化非常敏感,可以用来重建过去几百年、乃至千年的不同空间尺度的温度变化;树轮早材密度或最小早材密度对降水量的响应比较显著,但目前主要集中于重建区域小尺度的降水量变化方面。另外,树轮密度分析结果还可以用来研究某些气候要素分量的变化（季节变化、气候事件爆发的早晚和持续时间等）、区域气候变化的影响因子以及海气动力机制、气压异常等。     

Experimental study on water-oil migration and accumulation in a 2D micro-model of carbonate fracture media

Many achievements have been made in experimental studies of hydrocarbon migration in the clastic reservoir. On the other hand, few migration experiments have been reported in the carbonate reservoir simulation realm. This article is a tentative experimental study on hydrocarbon migration and accumulation in the carbonate reservoir, which is a complex media that includes a pore system and fracture system. This microcosmic experiment simulates oil-water displacement using a real core model. Plentiful seepage phenomena were observed in the microcosmic experiments. Three kinds of pathways were found in the plane: parallel pathway, oblique-cross pathway and network pathway. Three types of flow were found: continuous flow, sectioning flow and their combination. Three driving fronts were found in the experiment: piston front, encircle front and impulse front. All these vary with many factors such as fluid pressure, oil saturation, fissure configuration and wettability, and these factors affect each other. The results show that the relation between the fluid pressure and volume of flow is a complex segmenting correlation, instead of a simple positive correlation like the pipe flow that follows Darcy’s law. The relation between fluid pressure and the speed of flow also follows the same correlation. Speed of flow relates to the angle and width of the fissure. Speed of flow in the wide fissure that has an acute angle with the pressure gradient is faster than that in a narrow fissure with a high angle with the pressure gradient. Translated from Geological Review, 2006, 52(4): 570–576 [译自: 地质 论评]     

Using value engineering to optimize flood forecasting and flood warning systems: Golestan and Golabdare watersheds in Iran as case studies

Flood occurrence has always been one of the most important natural phenomena, which is often associated with disaster. Consequently, flood forecasting (FF) and flood warning (FW) systems, as the most efficient non-structural measures in reducing flood loss and damage, are of prime importance. These systems are low cost and the time required for their implementation is relatively short. It is emphasized that for designing the components of these systems for various rivers, climatic conditions and geographical settings different methods are required. One of the major difficulties during implementing these systems in different projects is the fact that sometimes the main functions of these systems are ignored. Based on a systematic and practical approach and considering the components of these systems, it would be possible to extract the most essential key functions of the system and save time, effort and money by this way. For instance, in a small watershed with low concentration and small lead time, the main emphasis should be on predicting and monitoring weather conditions. In this article, different components of flood forecasting and flood warning systems have been introduced. Then analysis of the FF and FW system functions has been undertaken based on the value engineering (VE) technique. Utilizing a functional view based on function analysis system technique (FAST), the total trend of FF and FW functions has been identified. The systematic trend and holistic view of this technique have been used in optimizing FF and FW systems of the Golestan province and Golabdare watersheds in Iran as the case studies.     

考虑剪力环、泥皮和防腐涂层作用的钢管复合桩工作性能模型试验研究

依托港珠澳大桥建设,通过5组不同组合的钢管复合桩模型试验,其中2组试件设有剪力环,开展了内置剪力环、泥皮和防腐涂层对钢管复合桩工作性能影响的研究,比较和分析试件的荷载-变形曲线、截面变形规律、钢管与剪力环变形等。试验结果表明,剪力环、泥皮和防腐涂层对钢管复合桩的工作性能具有一定的影响;泥皮和防腐涂层使钢管复合桩的黏结强度降低,而剪力环加强了钢管与核心混凝土的联结,钢管的受力及变形显著增加。在泥皮、防腐涂层和剪力环共同作用下,桩截面变形呈"倒v"或"m"型,不再满足经典力学的平截面变形假定。在泥皮、防腐涂层和剪力环间距S≤2D(D为桩径)的条件下,剪力环的嵌固作用可以完全克服泥皮和防腐涂层的不利影响。在试验结果研究的基础上,进一步探讨泥皮、防腐涂层和剪力环不同组合下钢管复合桩的刚度计算问题,并给出了在弹性阶段范围内钢管复合桩刚度计算公式,泥皮(厚度0.1 mm)和防腐涂层使其刚度降低,剪力环则使其增加。其研究结果可为钢管复合桩基工程设计提供重要的参考。     

Internal structure of simple S-bursts of Jovian decameter-wavelength emission

The fine internal structure of fundamental Jovian decameter-wavelength millisecond outbursts (S-bursts) is studied. Broadband data obtained with the Waveform Receiver (WFR) on the UTR-2 decameter radio telescope have been analyzed using wavelet transforms. The millisecond S-bursts have a complex internal pulse microstructure, whose parameters are presented. Our results offer new prospects for understanding Jovian decameter-wavelength emission.     

Circumstellar aluminum oxide and silicon carbide in interplanetary dust particles

A systematic NanoSIMS isotope imaging study of sub-micrometer phases in interplanetary dust particles (IDPs) has led to the discovery of two presolar grain types that previously were observed only in primitive meteorites. A 350 × 600 nm² Al₂O₃ grain has a large ¹⁷O enrichment and a slight ¹⁸O depletion, as well as a ²⁶Mg excess due to the decay of extinct ²⁶Al. Because of its relatively large size and prominent location within the IDP, this presolar Al₂O₃ grain is well characterized by SEM-EDX analyses. A second, much smaller presolar grain has a diameter of 150 nm and a ¹³C enrichment of more than 300%. Isotopic anomalies in C are rarely found in IDPs and the magnitude of this anomaly is unprecedented. This grain also has a ¹⁵N-rich composition and its isotopic makeup as well as its secondary ion yields identify it as a SiC grain. The discovery of presolar Al₂O₃ and SiC in IDPs seamlessly complements earlier notions of interplanetary dust particles as the most primitive extraterrestrial material currently available for laboratory analysis. Both Al₂O₃ and SiC are common presolar grain types in primitive meteorites, but they appeared conspicuously absent from the presolar grain inventory in interplanetary dust particles, which is dominated by silicate stardust. Not finding these presolar grain types in interplanetary dust would have been difficult to explain. Abundance estimates of the new presolar grain types in IDPs are hampered by limited statistics, but both Al₂O₃ and SiC are less common than presolar silicates which have been found at relatively high abundances in IDPs. The particle in which these presolar grains have been found belongs to the ‘isotopically primitive subgroup’ of IDPs, yet does not contain any presolar silicates.     

Formation of planets during the evolution of single and binary stars

Current views of the origin and evolution of single and binary stars suggest that the planets can form aroundmain-sequence single and binary stars, degenerate dwarfs, neutron stars, and stellarmass black holes according to several scenarios. Planets can arise during the formation of a star mainly due to excess angular momentum leading to the formation of an accretion-decretion disk of gas and dust around a single star or the components of a binary. It is the evolution of such disks that gives rise to planetary systems. A disk can arise around a star during its evolution due to the accretion of matter from dense interstellar clouds of gas and dust onto the star, the accretion of mass froma companion in a binary system, and the loss of matter during the contraction of a rapidly rotating star, in particular, if the star rotates as a rigid body and the rotation accelerates with its evolution along the main sequence. The fraction of stars with planetary systems is theoretically estimated as 30–40%, which is close to the current observational estimate of ∼34%.     

Finite Prandtl number 2-D convection at high Rayleigh numbers

Finite Prandtl number thermal convection is important to the dynamics of planetary bodies in the solar system. For example, the complex geology on the surface of the Jovian moon Europa is caused by a convecting, brine-rich global ocean that deforms the overlying icy “lithosphere”. We have conducted a systematic study on the variations of the convection style, as Prandtl numbers are varied from 7 to 100 at Rayleigh numbers 106 and 108. Numerical simulations show that changes in the Prandtl number could exert significant effects on the shear flow, the number of convection cells, the degree of layering in the convection, and the number and size of the plumes in the convecting fluid. We found that for a given Rayleigh number, the convection style can change from single cell to layered convection, for increasing Prandtl number from 7 to 100. These results are important for determining the surface deformation on the Jovian moon Europa. They also have important implications for surface heat flow on Europa, and for the interior heat transfer of the early Earth during its magma ocean phase. Electronic Supplementary Material is available if you access this article at . On that page (frame on the left side), a link takes you directly to the supplementary material. Electronic Supplementary Material is available if you access this article at . On that page (frame on the left side), a link takes you directly to the supplementary material.