论底苏铅锌矿床的“双源”沉积改造成矿模式

底苏铅锌矿床是近年来发现的。该矿床具“双源”沉积改造特征。同生沉积成岩成矿阶段同时存在海底热水和正常海水沉积作用,形成热水沉积矿石及矿源层。大气降水热液改造成矿阶段,大气降水沿岩石裂隙下渗被加热并淋滤早期沉积矿石及矿源层中的Ｐｂ、Ｚｎ,使之以［ＰｂＣｌ０２］、［ＺｎＣｌ０２］迁移,当含矿热液运移至有利构造部位时,Ｐｂ、Ｚｎ络合物交代地层中的黄铁矿或被有机质还原而再沉淀成矿。本文在矿床地球化学研究基础上,提出了底苏铅锌矿床的成矿模式     

新疆博格达山北麓山前断裂西段的断裂组成及其在全新世时期的活动

博格达山北麓山前断裂西段全长１４０ ｋｍ ,由５ 条雁列状排列的逆断裂组成。全新世时期,古牧地断裂的最新活动发生在６．８２±０．５４～４．８７±０．３９ Ｋａ Ｂ．Ｐ．之间;四工河口断裂切割Ⅱ级河流阶地,最新活动时间与古牧地断裂大体相同;泉泉子断裂切割Ⅰ级河流阶地,最新活动发生在３．７５±０．４１ Ｋａ Ｂ．Ｐ．;热水河断裂及东风牧场断裂由于缺乏断代年龄实测数据,无法对其最新活动时间作出判断,但是推断它们也是全新世活断裂     

新疆阿图什市近场区地震构造评价

在新疆阿图什市近场 2 5km范围内鉴别出全新世活断裂 1条 ,全新世活褶皱 5个。托特拱拜孜—阿尔帕雷克断裂在全新世时期曾有两次显示断错活动 ,累积铅直断距 170 cm,最新断错活动的 TL时间在 ( 8.6± 0 .0 3) Ka BP以内。该断裂历史上曾发生过 190 2年 8月 2 3日阿图什 8.2 5级地震 ,近期又发生了 1996年 3月 19日阿图什 6.9级地震 ,是一条地震断裂构造。由托特拱拜孜—阿尔帕雷克断裂与塔什皮萨克—阔诺勒果背斜褶皱构成的地震构造带所形成的潜在震源区距阿图什市工程场地以北 13km,其发生最大潜在地震的能力按 8.5级考虑 ,由全新世活褶皱构成的喀什—阿图什地震构造带所形成的潜在震源区的震级上限按 6.0级考虑     

Non‐local damage modelling of concrete: a procedure for the determination of model parameters

This paper presents a procedure for the determination of parameters of non‐local damage models. This is to assure a consistent response of a non‐local damage model, as choice of the internal length and other parameters of the model are varied. Correlations between the internal length and other parameters governing the local constitutive behaviour of the model are addressed and exploited. Focus is put on the relationship between the internal length of the non‐local model and the width of the fracture process zone. Numerical examples are used to demonstrate the rigour of the proposed method. Copyright © 2006 John Wiley & Sons, Ltd.     

平差系统模型误差补偿的配置法

利用大地测量数据分析地壳形变所建立的平差系统，不可避免地存在模型误差。给出了估计模型偏差的带权均方误差公式，提出了模型误差的识别、先验协方差的确定以及用最小二乘配置法对平差系统模型误差的补偿方法。     

Correlations between VIMS and RADAR data over the surface of Titan: Implications for Titan’s surface properties

We apply a multivariate statistical method to Titan data acquired by different instruments onboard the Cassini spacecraft. We have searched through Cassini/VIMS hyperspectral cubes, selecting those data with convenient viewing geometry and that overlap with Cassini/RADAR scatterometry footprints with a comparable spatial resolution. We look for correlations between the infrared and microwave ranges the two instruments cover. Where found, the normalized backscatter cross-section obtained from the scatterometer measurement, corrected for incidence angle, and the calibrated antenna temperature measured along with the scatterometry echoes, are combined with the infrared reflectances, with estimated errors, to produce an aggregate data set, that we process using a multivariate classification method to identify homogeneous taxonomic units in the multivariate space of the samples.In medium resolution data (from 20 to 100 km/pixel), sampling relatively large portions of the satellite’s surface, we find regional geophysical units matching both the major dark and bright features seen in the optical mosaic. Given the VIMS cubes and RADAR scatterometer passes considered in this work, the largest homogeneous type is associated with the dark equatorial basins, showing similar characteristics as each other on the basis of all the considered parameters.On the other hand, the major bright features seen in these data generally do not show the same characteristics as each other. Xanadu, the largest continental feature, is as bright as the other equatorial bright features, while showing the highest backscattering coefficient of the entire satellite. Tsegihi is very bright at 5 μm but it shows a low backscattering coefficient, so it could have a low roughness on a regional scale and/or a different composition. Another well-defined region, located southwest of Xanadu beyond the Tui Regio, seems to be detached from the surrounding terrains, being bright at 2.69, 2.78 and 5 μm but having a low radar brightness. In this way, other units can be found that show correlations or anti-correlations between the scatterometric response and the spectrophotometric behavior, not evident from the optical remote sensing data.     

The light curve of asteroid 2867 Steins measured by VIRTIS-M during the Rosetta fly-by

On 5 September 2008, the Rosetta spacecraft encountered the asteroid 2867 Steins on its way to the comet 67P/Churyumov-Gerasimenko. This was the first of two planned asteroid fly-bys performed by the probe, the second fly-by being with the much larger asteroid 21 Lutetia in July 2010. The VIRTIS imaging spectrometer (IFOV 0.250 mrad, overall spectral range 0.25-5.1 μm) onboard Rosetta acquired data of Steins already before the closest approach phase, when the target was spatially unresolved, in order to obtain a light curve of the asteroid in the infrared spectral range extending up to 5 μm, that was never explored before. The VIRTIS light curve campaign started at 11:30 UTC onboard time, when the spacecraft was about 221,377 km away from the target, and ended at 17:58 UTC, at a distance of 20,741 km away from Steins. During this timeframe, the solar phase angle of the asteroid was roughly constant, ranging from 38.2° to 36.3°.Assuming the most recent value derived for the rotational period of Steins (Lamy et al., 2008), the VIRTIS observations covered slightly more than one rotation of the asteroid. In this interval, VIRTIS collected 8 hyperspectral cubes where Steins was captured 119 times, both in the visual and in the infrared range. Given the low signal and the unresolved appearance of the source, for which the instrument was not designed, only a small subset of wavelengths turned out to be suitable to sample the light curve. Nevertheless, in both the VIS and NIR ranges we find a similar trend, with two different maxima and minima during one rotational period, and amplitudes consistent with the results in the visual range obtained in previous works, including the data set acquired by the OSIRIS camera onboard Rosetta. We also report the presence of a new broad feature centered at approximately 0.81-0.82 μm, which is seen in the visual data throughout the rotation of the asteroid.     

Numerical analysis and centrifuge modeling of shallow foundations

The influence of non-coaxial constitutive model on predictions of dense sand behavior is investigated in this paper. The non-coaxial model with strain softening plasticity is applied into finite-element program ABAQUS, which is first used to predict the stress-strain behavior and the non-coaxial characteristic between the orientations of the principal stress and principal plastic strain rate in simple shear tests. The model is also used to predict load settlement responses and bearing capacity factors of shallow foundations. A series of centrifuge tests for shallow foundations on saturated dense sand are performed under drained conditions and the test results are compared with the corresponding numerical results. Various footing dimensions, depths of embedment, and footing shapes are considered in these tests. In view of the load settlement relationships, the stiffness of the load-displacement curves is significantly affected by the non-coaxial model compared with those predicted by the coaxial model, and a lower value of non-coaxial modulus gives a softer response. Considering the soil behavior at failure, the coaxial model predictions of bearing capacity factors are more advanced than those of centrifuge test results and the non-coaxial model results;besides, the non-coaxial model gives better predictions. The non-coaxial model predictions are closer to those of the centrifuge results when a proper non-coaxial plastic modulus is chosen.