砒砂岩地区小流域毛沟侵蚀特性分析

为探讨砒砂岩地区毛沟的形成机理,以内蒙鄂尔多斯市东一支沟小流域2005-05地形及毛沟特征要素详细测量数据为基础,分析了该流域的毛沟分布规律。结果表明,该流域毛沟数量和单位面积毛沟长度从下游到上游呈递增趋势;按毛沟的成因将其划分为自侵式毛沟和汇入式毛沟两类,并从毛沟数量、沟底比降、毛沟长度、沟底宽、沟深等方面分析了这两类毛沟的主要特征。研究结果有利于深化人们对砒砂岩地区小流域毛沟侵蚀特性的认识。     

黄土区细沟侵蚀过程中输沙能力确定的解析法

 输沙能力是坡面细沟侵蚀过程预报模型中所需的重要参数,确定坡面输沙能力一直是土壤侵蚀研究关注的问题。解析法是用数学上的积分和积分变换等方法直接求数学模型的解,其优点是把表征坡面土壤运动规律的变量和时空变化包含在一个表达式内,可以分析土壤侵蚀的过程运动规律。由细沟侵蚀室内模拟试验得出的剥蚀率和含沙量之间的函数关系,推导得到了计算细沟输沙能力的解析式。将由解析方法计算求得的水流输沙能力与由试验数据直接估算出来的结果进行了对比,验证了该解析式的合理性。     

Discovery of vapor deposits in the lunar regolith

Lunar soils contain micrometer-sized mineral grains surrounded by thin amorphous rims. Similar features have been produced by exposure of pristine grains to a simulated solar wind, leading to the widespread belief that the amorphous rims result from radiation damage. Electron microscopy studies show, however, that the amorphous rims are compositionally distinct from their hosts and consist largely of vapor-deposited material generated by micrometeorite impacts into the lunar regolith. Vapor deposits slow the lunar erosion rate by solar wind sputtering, influence the optical properties of the lunar regolith, and may account for the presence of sodium and potassium in the lunar atmosphere.     

Of time and the moon

Considerable information concerning lunar chronology has been obtained by the study of rocks and soil returned by the Apollo 11 and Apollo 12 missions. It has been shown that at the time the moon, earth, and solar system were formed, approximately 4.6 approximately 10(9) years ago, a severe chemical fractionation took place, resulting in depletion of relatively volatile elements such as Rb and Pb from the sources of the lunar rocks studied. It is very likely that much of this material was lost to interplanetary space, although some of the loss may be associated with internal chemical differentiation of the moon. It has also been shown that igneous processes have enriched some regions of the moon in lithophile elements such as Rb, U, and Ba, very early in lunar history, within 100 million years of its formation. Subsequent igneous and metamorphic activity occurred over a long period of time; mare volcanism of the Apollo 11 and Apollo 12 sites occurred at distinctly different times, 3.6 approximately 10(9) and 3.3 approximately 10(9) years ago, respectively. Consequently, lunar magmatism and remanent magnetism cannot be explained in terms of a unique event, such as a close approach to the earth at a time of lunar capture. It is likely that these phenomena will require explanation in terms of internal lunar processes, operative to a considerable depth in the moon, over a long period of time. These data, together with the low present internal temperatures of the moon, inferred from measurements of lunar electrical conductivity, impose severe constraints on acceptable thermal histories of the moon. Progress is being made toward understanding lunar surface properties by use of the effects of particle bombardment of the lunar surface (solar wind, solar flare particles, galactic cosmic rays). It has been shown that the rate of micrometeorite erosion is very low (angstroms per year) and that lunar rocks and soil have been within approximately a meter of the lunar surface for hundreds of millions of years. Future work will require sampling distinctly different regions of the moon in order to provide data concerning other important lunar events, such as the time of formation of the highland regions and of the mare basins, and of the extent to which lunar volcanism has persisted subsequent to the first third of lunar history. This work will require a sufficient number of Apollo landings, and any further cancellation of Apollo missions will jeopardize this unique opportunity to study the development of a planetary body from its beginning. Such a study is fundamental to our understanding of the earth and other planets.     

Incised river meanders: evolution in simulated bedrock

A flume 60 feet (18.28 meters) long was employed to study the controls of lateral and vertical incision of a sinuous stream in simulated bedrock. When 100 percent of the available sediment load was entrained the flow incised vertically at bends. When less than 100 percent of the load was entrained the flow downcut laterally outward at bends. The effects of helicoidal currents and shear stress localization explain the loci of erosion and deposition.     

Farmers’ Views of Soil Erosion Problems and their Conservation Knowledge at Beressa Watershed, Central Highlands of Ethiopia

Farmers’ decisions to conserve natural resources generally and soil and water particularly are largely determined by their knowledge of the problems and perceived benefits of conservation. In Ethiopia, however, farmer perceptions of erosion problems and farmer conservation practices have received little analysis or use in conservation planning. This research examines farmers’ views of erosion problems and their conservation knowledge and practices in the Beressa watershed in the central highlands of Ethiopia. Data were obtained from a survey of 147 farm households managing 713 fields during the 2002/2003 cropping season. In-depth interviews and group discussions were also held with the farmers to obtain additional information. The results show that 72% of the farmers reported erosion problems, and they recognized that conservation was necessary. However, they considered erosion to be severe mostly when visible signs – rills and gullies – appeared on their fields. The majority of the farmers believe that erosion could be halted, and they use a range of practices for erosion control and fertility improvement. These include contour plowing (83%), drainage ditches (82%), and stone terraces/bunds (73%). Nevertheless, despite decades of conservation intervention in the area, it appears that most farmers have developed negative attitudes towards externally recommended measures. The research concludes that under the conditions present in the Ethiopian central highlands, soil and water conservation interventions should consider farmers’ conservation knowledge and practices to improve acceptance and adoption of the recommendations. Aklilu Amsalu is a lecturer in the Department of Geography and Environmental Studies of Addis Ababa University, Addis Ababa, Ethiopia. He is currently doing his PhD research on best land management practices in highland watershed management in Ethiopia in the Department of Environmental Sciences of Wageningen University, Wageningen, The Netherlands. Jan de Graaff is a senior lecturer and researcher in the Erosion and Soil and Water Conservation Group of Wageningen University, Wageningen, The Netherlands. His expertise is on impact assessment and economic evaluation of soil and water conservation.     

Solar particle tracks in glass from the surveyor 3 spacecraft

A glass filter from Surveyor 3 has a surface density of approximately 1 x 10(6) tracks per square centimeter from heavy solar flare particles. The variation with depth is best fitted with a solar particle spectrum dN/dE = 2.42 x 10(6) E(-2) [in particles per square centimeter per year per steradian per (million electron volts per nucleon)], where E is the energy and N is the number of particles, from 2 million electron volts per nucleon to approximately 7 million electron volts per nucleon and dN/dE = 1.17 x 10(7) E(-3) at higher energies. Not much difference is observed between 0.5 and 5 micrometers, an indication that there is a lack of track-registering particles below 0.5 million electron volts per nucleon. The Surveyor data are compatible with track results in lunar rocks, provided an erosion rate of approximately 10(-7) centimeter per year is assumed for the latter. The results also suggest a small-scale erosion process in lunar rocks.     

Mariner IV: Analysis of Preliminary Photographs

Comparison of the distributions of Martian and lunar crater diameters indicates that the visible surface of Mars is 2.2 to 3 x 10(9) years old. This result implies that in the early history of Mars large-scale subaerial erosion occurred. Of 69 Martian craters with diameters greater than 10 kilometers, 13 percent have central peaks. This compares favorably with the frequency (11.7 percent) of central peaks among lunar craters and may indicate that the central peaks are a direct result of the impact mechanism rather than post-impact volcanism. A well-defined system of lineaments is shown in the Mariner photographs. The presence of these lineaments may indicate that Mars has lost appreciable angular momentum during its history.     

Cosmic-ray record in solar system matter

The energetic nuclei in cosmic rays interact with meteoroids, the moon, planets, and other solar system matter. The nuclides and heavy nuclei tracks produced by the cosmic-ray particles in these targets contain a wealth of information about the history of the objects and temporal and spatial variations in the particle fluxes. Most lunar samples and meny meteorites have complex histories of cosmicray exposure from erosion, gardening, fragmentation, orbital changes, and other processes. There appear to be variations in the past fluxes of solar particles, and possibly also galactic cosmic rays, on time scales of 10(4) to 10(7) years.     

Water vapor from a lunar breccia: implications for evolving planetary atmospheres

The exposure of a typical complex lunar breccia to hydrogen after a thorough outgassing produces a fully reduced surface state. Subsequent outgassing over a wide temperature range results in the production of water vapor formed from the chemisorbed hydrogen and oxygen from the lunar sample; the proposed mechanism has been confirmed in terms of the chemisorption of deuterium and the release of heavy water. Since the conditions of the experiments are consistent with those on the lunar surface, it is postulated that water vapor will be produced on the moon through the interaction of the solar wind with lunar soil. It is also proposed that such a process could play an important role in the early history of many planets where an oxygen-rich soil is exposed to a reducing atmosphere.     

Surveyor v: lunar surface mechanical properties

The mechanical properties of the lunar soil at the Surveyor V landing site seem to be generally consistent with values determined for soils at the landing sites of Surveyor I and III. These three maria sites are hundreds of kilometers apart. However, the static bearing capability may be somewhat lower than that at the previous landing sites (2 x 10(5) to 6 x 10(5) dynes per square centimeter or 3 to 8 pounds per square inch). The results of the erosion experiment, the spacecraft landing effects, and other observations indicate that the soil has significant amounts of fine-grained material and a measurable cohesion.     

The Lunar Laser Ranging Experiment: Accurate ranges have given a large improvement in the lunar orbit and new selenophysical information

The lunar ranging measurements now being made at the McDonald Observatory have an accuracy of 1 nsec in round-trip travel time. This corresponds to 15 cm in the one-way distance. The use of lasers with pulse-lengths of less than 1 nsec is expected to give an accuracy of 2 to 3 cm in the next few years. A new station is under construction in Hawaii, and additional stations in other countries are either in operation or under development. It is hoped that these stations will form the basis for a worldwide network to determine polar motion and earth rotation on a regular basis, and will assist in providing information about movement of the tectonic plates making up the earth's surface. Several mobile lunar ranging stations with telescopes having diameters of 1.0 m or less could, in the future, greatly extend the information obtainable about motions within and between the tectonic plates. The data obtained so far by the McDonald Observatory have been used to generate a new lunar ephemeris based on direct numerical integration of the equations of motion for the moon and planets. With this ephemeris, the range to the three Apollo retro-reflectors can be fit to an accuracy of 5 m by adjusting the differences in moments of inertia of the moon about its principal axes, the selenocentric coordinates of the reflectors, and the McDonald longitude. The accuracy of fitting the results is limited currently by errors of the order of an arc second in the angular orientation of the moon, as derived from the best available theory of how the moon rotates in response to the torques acting on it. Both a new calculation of the moon's orientation as a function of time based on direct numerical integration of the torque equations and a new analytic theory of the moon's orientation are expected to be available soon, and to improve considerably the accuracy of fitting the data. The accuracy already achieved routinely in lunar laser ranging represents a hundredfold improvement over any previously available knowledge of the distance to points on the lunar surface. Already, extremely complex structure has been observed in the lunar rotation and significant improvement has been achieved in our knowledge of lunar orbit. The selenocentric coordinates of the retroreflectors give improved reference points for use in lunar mapping, and new information on the lunar mass distribution has been obtained. Beyond the applications discussed in this article, however, the history of science shows many cases of previously unknown, phenomena discovered as a consequence of major improvements in the accuracy of measurements. It will be interesting to see whether this once again proves the case as we acquire an extended series of lunar distance observations with decimetric and then centimetric accuracy.     

Very heavy solar cosmic rays: energy spectrum and implications for lunar erosion

The energy spectrum of solar cosmic-ray particles of the iron group has been determined for the first time over the energy range from 1 to 100 million electron volts per nucleon by the use of glass removed from the Surveyor 3 spacecraft. The difference between the observed (energy)(-3) spectrum and the limiting spectrum derived previously from tracks in lunar rocks gives an erosion rate of 0 to 2 angstroms per year. High-energy fission of lead, induced by galactic cosmicray protons and alpha particles, has also been observed.     

Fluorometric examination of a lunar sample

We have been unable to detect porphyrins in 13 grams of the bulk fine lunar sample from the Sea of Tranquillity under conditions in which less than 10-(1J) mole per gram of lunar sample could have been detected. By appropriate extraction, however, the lunar sample yields a material which exhibits absorption maxima at 310 and 350 nanometers and a fluorescence maximum at 410 nanometers.     

Lunar gravity: the first farside map

A global lunar gravity field has been determined from data on the long-term motion of the Apollo 15 and Apollo 16 subsatellites and Lunar Orbiter 5. The nearside gravity map resolves major mascon basins and, in general, is in excellent agreemnent with the results of Muller and Sjogren. The farside gravity map is characterized by broad positive gravity in the highland regions with interspersed, localized, negative anomalies corresponding to major ringed basins. A comparison between global gravity and topography indicates that a thicker farside crust could be responsible for these gravitational differences between the two lunar hemispheres.     

野外土壤风蚀定量观测方法的研究

[目的]介绍野外土壤风蚀定量观测的新方法。[方法]在综合分析土壤风蚀量评估主要方法和手段优缺点的基础上,提出一种野外土壤风蚀量定量观测的新方法———风蚀圈法。[结果]风蚀圈的最大优点是简单实用、容易携带,可长期放置在野外,实现土壤风蚀的定量观测;其镶嵌在土壤中,表面基本与地面持平,可防止局部微地形对风蚀过程的影响;底部尼龙布透水通气性好,可保持风蚀圈内土样与周围土壤状态一致,观测数据接近实际;最大弊端是放、取土时部分土样容易跑出圈外,影响观测值的准确性。[结论]风蚀圈法是野外观测比较实用的方法,可用于测定单位面积的土壤风蚀量,实现风沙区风蚀季节的定量连续监测。     

Rare Earth elements in returned lunar samples

A linear correlation between concentrations of Sm and ratios of Sm to Eu for nine lunar samples suggests that those samples could correspond to liquids from equilibrium partial melting of a common source. On the basis of partition coefficients in terrestrial systems, the fraction of melting would not have exceeded about 15 percent and the immediate source could have been composed of olivine, orthopyroxene, and opaque minerals plus at least 25 percent feldspar, with at most a few percent calcic clinopyroxene and less than 1 percent apatite. The large Eu depletions could also have been produced by fractional crystallization if the ratio of Eu(2+) to Eu(3+) in lunar magmas significantly exceeds the values for terrestrial magmas.     

Shoreline forms and shoreline dynamics

Atlantic coast barrier-island shorelines are sinuous in plan view, with curvatures ranging in size from cusps to capes. The orientation of shoreline segments within the larger of these sinuous features (10 to 15 kilometers between apexes) is significantly related to shoreline dynamics.     

Abundances of 30 elements in lunar rocks, soil, and core samples

Abundances of 30 elements in seven lunar rocks and soil were determined by instrumental and radiochemical activation analysis. Seven major and minor elements in chips from 27 rocks were determined by instrumental activation analysis. Abundances of ten bulk elements overlap for the breccia rocks and soil samples. All lunar rare earth elements distribution patterns resemble those found in terrestrial abyssal subalkaline basalt, but with Eu depleted by about 60 percent in all lunar samples compared to the adjacent rare earth elements. Precipitation of plagioclase and hypersthene achondritic-like minerals from a melt could account for Eu depletion and the observed distribution of rare earth elements. Abundances of Ti, Al, Ca, Na, and Mn determined by instrumental activation analysis in five core-tube soil samples indicate uniformity for Al and Mn and apparent differences (10 to 20 percent) for Ti, Ca, and Na at 7.8 and 10.5 centimeters as compared to 0to5.2 centimeter depths.     

Search for porphyrins in lunar dust

Evidence for porphyrins was obtained in the Apollo 11 bulk sample of lunar dust by fluorescence spectrometry and analytical demetallation. The indicated porphyrins showed major fluorescence excitation at 390 nanometers. Abundance was about 10(-10) gram of porphyrin per gram of dust. Similar pigments were found in exhaust products from tests of a lunar descent engine. The similarity of results suggests that most if not all of the indicated porphyrin aggregate of the lunar sample probably was synthesized from rocket fuel during the landing of the lunar module. These compounds may be the product of a novel high-temperature synthesis of cosmochemical interest.