Undrained dynamic-loading ring-shear apparatus and its application to landslide dynamics   总被引：26，自引：17，他引：9  

Kyoji Sassa  Hiroshi Fukuoka  Gonghui Wang  Naohide Ishikawa 《Landslides》2004,1(1):7-19

Landslides are gravitational mass movements of rock, debris or earth. Some move very slowly, thus conforming to the field of statics, but some move rapidly. Study of the initiation and motion of rapid landslides needs to develop Landslide Dynamics involving dynamic loading and dynamic generation/dissipation of excess pore-water pressure. New developments in science can be facilitated by new technological advances. This study aimed to develop a new apparatus that can geotechnically simulate the formation of the shear zone and the following long and rapid shear displacement that occurs in high-velocity landslides. Professor K. Sassa and his colleagues at DPRI (Disaster Prevention Research Institute), Kyoto University, have worked to develop an undrained dynamic-loading ring-shear apparatus for this purpose. A series of different types of apparatus (DPRI-3, 4, 5, 6, 7) have been developed from 1992 to the present. This paper describes the development of this apparatus and its application to the study of earthquake-induced landslides and the latest landslide-triggered debris flow in Japan. Also, tests of the latest version (DPRI-7) with a transparent shear box for direct observation of the shear zone during a rapid shearing are described.  相似文献   

电子政务空间信息服务:需求、技术与应用   总被引：9，自引：2，他引：7  

刘纪平  王亮 《测绘科学》2006,31(2):54-56

本文总结了空间信息服务的现状,讨论了电子政务与空间信息服务的关系,提出了电子政务空间信息服务的要求,讨论了空间信息服务关键技术,介绍了电子政务空间信息服务的应用情况。  相似文献   

中国海岸带分布规律及其海部要素变化检测   总被引：2，自引：1，他引：1  

冯伍法  潘时祥  张朝阳  张俊华 《测绘科学技术学报》2006,23(5):370-373,377

在海岸带图测绘完成后,海部要素的变化是导致海岸带图使用价值降低的重要因素.根据我国海岸的组成物质将其归纳为淤泥质海岸、沙砾质海岸、基岩海岸、红树海岸和珊瑚海岸,并归纳总结了每一种海岸的空间分布规律.分析了影响海岸线、干出滩以及近海水深等海部要素变化的主要因素,海岸要素变化的因素和变化规律,进而提出了海部要素实质性变化的检测统计方法,对提高海岸带图测绘效率、缩短成图周期、确定更新周期和制定更新方案都具有重要的意义.  相似文献   

面向e-GeoScience的地学数据共享研究进展   总被引：1，自引：0，他引：1  

诸云强  孙九林 《地球科学进展》2006,21(3):286-290

在总结比较国内外e-GeoScience研究进展的基础上,介绍了中国科学院地理科学与资源研究所自20世纪80年代以来开展的相关工作。提出了按“圈层—学科—数据类别”三级模式的地球系统科学数据分类体系,以主体数据库为核心,初步构建了“主体数据库—数据资源点”为支撑的地球系统科学数据资源体系。在J2EE环境下,采用Web Services、地理信息等技术开发了地球系统科学数据共享平台。最后,探讨了e-GeoScience未来的研究方向。  相似文献   

Light-toned layered deposits in Juventae Chasma, Mars     

David C. Catling  Stephen E. Wood  David R. Montgomery  Christopher R. Glein 《Icarus》2006,181(1):26-51

We examine hypotheses for the formation of light-toned layered deposits in Juventae Chasma using a combination of data from Mars Global Surveyor's Mars Orbiter Camera (MOC), Mars Orbiter Laser Altimeter (MOLA), and Thermal Emission Spectrometer (TES), as well as Mars Odyssey's Thermal Emission Imaging System (THEMIS). We divide Juventae Chasma into geomorphic units of (i) chasm wall rock, (ii) heavily cratered hummocky terrain, (iii) a mobile and largely crater-free sand sheet on the chasm floor, (iv) light-toned layered outcrop (LLO) material, and (v) chaotic terrain. Using surface temperatures derived from THEMIS infrared data and slopes from MOLA, we derive maps of thermal inertia, which are consistent with the geomorphic units that we identify. LLO thermal inertias range from ∼400 to 850 J m⁻² K⁻¹ s^−1/2. Light-toned layered outcrops are distributed over a remarkably wide elevation range () from the chasm floor to the adjacent plateau surface. Geomorphic features, the absence of small craters, and high thermal inertia show that the LLOs are composed of sedimentary rock that is eroding relatively rapidly in the present epoch. We also present evidence for exhumation of LLO material from the west wall of the chasm, within chaotic and hummocky terrains, and within a small depression in the adjacent plateau. The data imply that at least some of the LLO material was deposited long before the adjacent Hesperian plateau basalts, and that Juventae Chasma underwent, and may still be undergoing, enlargement along its west wall due to wall rock collapse, chaotic terrain evolution, and exposure and removal of LLO material. The new data allow us to reassess possible origins of the LLOs. Gypsum, one of the minerals reported elsewhere as found in Juventae Chasma LLO material, forms only at low temperatures () and thus excludes a volcanic origin. Instead, the data are consistent with either multiple occurrences of lacustrine or airfall deposition over an extended period of time prior to emplacement of Hesperian lava flows on the plateau above the chasm.  相似文献   

Evolution of the dusty rings of Uranus     

Imke de Pater  Seran G. Gibbard 《Icarus》2006,180(1):186-200

We present high quality images of the uranian ring system, obtained in August 2002, October 2003, and July 2004 at 2.2 μm with the adaptive optics camera NIRC2 on the Keck II telescope. Using these data, we report the first detection in backscattered light of a ring (which we refer to as the ζ ring) interior to Uranus' known rings. This ring consists of a generally uniform sheet of dust between 37,850 and 41,350 km with an equivalent width (in 2004; or ), and extends inward to 32,600 km at a gradually decreasing brightness. This ring might be related to the Voyager ring R/1986 U 2, although both its location and extent differ. This could be attributed to a difference in observing wavelength and/or solar phase angle, or perhaps to temporal variations in the ring. Through careful modeling of the I/F of the individual rings at each ansa, we reveal the presence of narrow (few 100 km wide) sheets of dust between the δ and ε rings, and between rings 4 and α. We derived a typical anisotropy factor g≈0.7 in the scattering behavior of these particles. The spatial distribution and relative intensity of these dust sheets is different than that seen in Voyager images taken in forward scattered light, due either to a difference in observing wavelength, and/or solar phase angle or to changes over time. We may have detected the λ ring in one scan at , but other scans provided upper limits below this value. A single detection, however, would be consistent with azimuthal asymmetries known to exist in this ring. We further demonstrate the presence of azimuthal asymmetries in all rings. We confirm the eccentricity of ∼0.001 in rings 4, 5, 6, which in 2004 are ∼70 km closer to Uranus in the north (near periapse; lower I/F) than in the south. We find a global optical depth of τ∼0.3 in the main rings, and of τ=0.25±0.05 in the ε ring.  相似文献   

Thermal emission spectroscopy (5.2-38 μm) of three Trojan asteroids with the Spitzer Space Telescope: Detection of fine-grained silicates     

J.P. Emery  D.P. Cruikshank 《Icarus》2006,182(2):496-512

We present thermal emission spectra (5.2-38 μm) of the Trojan asteroids 624 Hektor, 911 Agamemnon, and 1172 Aneas. The observations used the Infrared Spectrograph (IRS) on board the Spitzer Space Telescope. Emissivity spectra are created by dividing the measured Spectral Energy Distribution (SED) by a model of the thermal continuum. We employ the Standard Thermal Model (STM), allowing physical parameters (e.g., radius and albedo) to vary in order to find the best thermal continuum fit to the SED. The best-fit effective radius (R) and visible geometric albedo (pv) for Hektor (R=110.0±7.3, ) and Aneas (R=69.1±5.1, ) agree very well with previous estimates, and for Agamemnon (R=71.5±5.2, ) we find slightly a smaller size and higher albedo than previously derived. Other thermal models (e.g., thermophysical) result in estimates of R and pv that vary a few percent from the STM, but the resulting emissivity spectra are identical. The emissivity spectra of all three asteroids display an emissivity plateau near 10-μm and another broader rise from ∼18 to 28 μm. We interpret these as indications of fine-grained silicates on the surfaces of these asteroids. The emissivity spectra more closely resemble emission spectra from cometary comae than those from solid surfaces and measured in the laboratory for powdered meteorites and regolith analogs. We hypothesize that the coma-like emission from the solid surfaces of trojans may be due to small silicate grains being imbedded in a relatively transparent matrix, or to a very under-dense (fairy-castle) surface structure. These hypotheses need to be tested by further laboratory and theoretical scattering work as well as continued thermal emission observations of asteroids.  相似文献   

基于广义3S技术的森林资源经营管理系统建设   总被引：8，自引：0，他引：8  

冯仲科  臧淑英  姚山 《测绘工程》2006,15(2):1-6

针对我国森林资源经营管理处于比较粗放的水平,将现代测绘科学与林业相结合,构建基于广义3S技术的森林资源经营管理系统。  相似文献   

温度对陀螺经纬仪稳定性影响的一种测试方法     

马小辉  田育民  王华 《测绘科学》2012,37(5):58-60

本文提出了一种温度对陀螺经纬仪稳定性影响的测试方法,引入了单因素方差分析的数理统计方法,评价陀螺经纬仪在高低温环境下的稳定性;对高低温稳定性测试过程中观测窗变形的影响进行了分析和实验研究,认为本文中采用的高低温室观测窗的变形量,对中低精度的陀螺经纬仪高低温稳定性测试而言可以忽略;最后通过实际测试数据验证了该方法的可行性。  相似文献   

TM影像的变化检测方法探究     

孙金萍  翟亮 《测绘科学》2012,(4):157-159

变化检测是遥感应用中的一项重要内容。随着遥感技术的发展,变化检测技术也有了很大的进步,出现了很多的研究方法和研究成果。本文在总结前人研究的基础上,提出了TM影像变化检测的基本流程,并简单介绍了各个流程,包括数据预处理、变化信息的提取以及变化区域的确定,重点介绍了变化检测的方法尤其是目前最新的研究方法,最后对变化检测的前景提出了展望。  相似文献