黄河三角洲水冰险情预警信息系统设计与分析应用探讨

本文探讨了黄河三角洲地区水冰灾情信息系统的建立方法及其应用问题。介绍了该系统的设计原则,数据结构,建立方法和程序,并对其应用进行了分析研究。该方法也适用于其它区域。     

嫦娥三号着陆区月海玄武岩的年龄、成因及地质意义

月海玄武岩主要分布在月海中,由斜长石、辉石和橄榄石组成,与地球玄武岩相比,富铁而贫钠和钾。月海玄武岩的成因,年代和成分研究是理解月岩形成与演化的基础。月球返回的岩石样品数量和覆盖面积有限,并且CE-3号着陆区没有月球样品返回,所以地球上的实验室样品分析方法不能应用到CE-3号着陆区玄武岩研究。本文对CE-3号着陆区月表和下伏玄武岩的组分、来源、分布、年代和层序进行反演和分析。主要使用的研究方法主要包括:玄武岩单元的撞击坑频率-分布函数定年,基于撞击坑的月壤下伏玄武岩单元识别、划分及厚度反演,基于遥感数据的元素含量和矿物成分分析等。结果表明:(1)CE-3号着陆区至少出现了6次较大规模的岩浆充填事件,由新到老分别为EIm、EIm_1、EIm_2、Im、Im_1和Im_2,其中EIm单元年龄约为3.17Ga,Im单元年龄为3.48Ga;(2)研究区玄武岩单元铁元素成分变化不大,而钛元素含量有较大变化。并且玄武岩越年轻,铁和钛元素更加富集。对指示月表硅酸盐矿物的克里斯蒂安参数(CF)和弯曲指数(CI)进行计算,发现研究区没有高硅物质的分布;(3)研究区月海玄武岩充填活动具有多期次性,每期月海玄武岩的充填流动大体上保持由南向北方向,并且活动规模逐步减小;(4)下伏玄武岩单元EIm_1、EIm_2、Im、Im_1和Im_2的平均厚度分别为68.3m,68.6m,81.8m,59.1m和52.1m,其中EIm_1单元的厚度最大为150m,从西到东逐渐减小;Im_1最大深度为224m,位于研究区的北部,向东西两侧依次减小。     

Periodicity in the crater formation rate and implications for astronomical modeling

Claim for periodicity in the crater formation rate is reinvestigated using a criterion proposed by Broadbent, and data sets of Rampino and Stothers and of Grieve are shown to satisfy the periodicity criterion (P 30 Myr).On the other hand, currently observed impactors are mainly asteroids, while long and short periodic comets whose fluxes may vary by external disturbances occupy only a small fraction. Using a Monte Carlo simulation, constraints are obtained for the dispersion Q(Myr) from an exact periodicity and for the periodic components (F _tp) in the signals for their periodicity to be detected. It is found that for = 5, 6 and 7 Myr, F _tp, would have to be 40% or greater, 60% or greater and 80% or greater, respectively. These constraints are used to discuss whether the giant molecular cloud perturbations can give rise to the periodicity in the impact events. The amplitude of the solar Z-motion need to be some 100pc for = 6 Myr, which requires the periodic component (SP and LP comets, if the former originate from the latter) to be 60%, while for = 7 Myr, the periodic component need to be 80%. The GMC perturbation model consistent with the periodicity appears to be the one where the amplitude is 100pc and the periodic component - 60% of the impactors. If SP comets mainly originate from a source such as the hypothetical Kuiper belt, the GMC perturbation would not be consistent with the periodicity.     

Seismic image of the Mount Spurr magmatic system

 The three-dimensional P-wave velocity structure of Mount Spurr is determined to depths of 10 km by tomographic inversion of 3,754 first-arriving P-wave times from local earthquakes recorded by a permanent network of 11 seismographs. Results show a prominent low-velocity zone extending from the surface to 3–4 km below sea level beneath the southeastern flank of Crater Peak, spatially coincident with a geothermal system. P-wave velocities in this low-velocity zone are approximately 20% slower than those in the shallow crystalline basement rocks. Beneath Crater Peak an approximately 3-km-wide zone of relative low velocities correlates with a near-vertical band of seismicity, suggestive of a magmatic conduit. No large low-velocity zone indicative of a magma chamber occurs within the upper 10 km of the crust. These observations are consistent with petrologic and geochemical studies suggesting that Crater Peak magmas originate in the lower crust or upper mantle and have a short residence time in the shallow crust. Earthquakes relocated using the three-dimensional velocity structure correlate well with surface geology and other geophysical observations; thus, they provide additional constraints on the kinematics of the Mount Spurr magmatic system. Received: 4 December 1997 / Accepted: 27 February 1998     

1：50000数据库的更新服务数据库系统设计与实现

1：50000数据库的更新工程数据库服务系统是以1：50000数据库更新成果为基础．建立了一个基于B／S结构的服务系统,满足更新数据快速发布、浏览、应急服务等需求。本文介绍了陔系统的设计思想、系统总体架构、数据库设计与建库、软件功能设计与实现,为其他地理信息数据系统建设提供借豁。     

Capability of the penetrator seismometer system for lunar seismic event observation

We developed a seismometer system for a hard landing “penetrator” probe in the course of the former Japanese LUNAR-A project to deploy new seismic stations on the Moon. The penetrator seismometer system (PSS) consists of two short-period sensor components, a two-axis gimbal mechanism for orientation, and measurement electronics. To carry out seismic observations on the Moon using the penetrator, the seismometer system has to function properly in a lunar environment after a hard landing (impact acceleration of about 8000 G), and requires a signal-to-noise ratio to detect lunar seismic events. We evaluated whether the PSS could satisfactorily observe seismic events on the Moon by investigating the frequency response, noise level, and response to ground motion of our instrument in a simulated lunar environment after a simulated impact test. Our results indicate that the newly developed seismometer system can function properly after impact and is sensitive enough to detect seismic events on the Moon. Using this PSS, new seismic data from the Moon can be obtained during future lunar missions.     

Reflectance spectra of analog anorthosites: Implications for lunar highland mapping

Lunar highland region and associated craters are mostly composed of anorthosite. In the present study, we studied the reflectance spectra of terrestrial anorthosites collected from Sittampundi Anorthosites Complex, which is considered as equivalent (simulant) of lunar highland anorthosites. The objective of the study is to interpret diagnostic spectral features of analog anorthosite for remotely exploring lunar highland region. Reflectance spectra of anorthosites were measured under two different environments, such as controlled field and laboratory conditions. In these two procedures, the laboratory spectra give clear, diagnostic spectral information in the present study. Reflectance spectra captured under 350-2500 nm covering UV, Visible, NIR, and SWIR part of the electromagnetic spectrum. The spectral characteristics of anorthosites measured under various parts of electromagnetic spectrum have diagnostic absorption features at 380-387, 700-740, 930-1100, 1160-1200, 1415, 1920, 2200 and 2330 nm correspondingly due to plagioclase UV absorption, Fe³⁺ electron transition absorption, Fe²⁺ pyroxene and olivine absorption, OH/Mn³⁺ crystal transition absorption, pyroxene absorption, Al-OH absorption and Mg-OH absorption. Mineralogical and chemical analyses were carried out for four anorthosites and compared with the results of chemical component of lunar anorthosite. The percentage of plagioclase content, relative abundance of low and high calcium pyroxene and olivine in different anorthosite samples are correlated with the albedo range, absorption shape, absorption centers and band depth. The similarity in the diagnostic spectral features of the anolog anorthosite with lunar anorthosites could be effectively utilized for remotely mapping the lunar highland region.     

Optical scattering processes observed at the Moon: Predictions for the LADEE Ultraviolet Spectrometer

The Lunar Atmosphere and Dust Environment Explorer (LADEE) spacecraft will orbit the Moon at an altitude of ≈50 km with a payload that includes the Ultraviolet Spectrometer (UVS) instrument, which will obtain high spectral resolution measurements at near-ultraviolet and visible wavelengths (≈231-826 nm). When LADEE/UVS observes the lunar limb from within the shadow of the Moon it is anticipated that it will detect a lunar horizon glow (LHG) due to sunlight scattered from submicron exospheric dust, as well as emission lines from exospheric gases (particularly sodium), in the presence of the bright coronal and zodiacal light (CZL) background. A modularized code has been developed at NMSU for simulations of scattered light sources as observed by orbiting instruments in lunar shadow. Predictions for the LADEE UVS and star tracker cameras indicate that LHG, sodium (Na) emission lines, and CZL can be distinguished based on spatial morphology and spectral characteristics, with LHG dominant at blue wavelengths (∼250-450 nm) and small tangent heights. If present, LHG should be readily detected by LADEE/UVS and distinguishable from other sources of optical scattering. Observations from UVS and the other instruments aboard LADEE will significantly advance our understanding of how the Moon interacts with the surrounding space environment; these new insights will be applicable to the many other airless bodies in the solar system.     

非开挖管理软件的设计与开发

利用VisualBasic 6．0语言开发非开挖管理软件,选择Microsoft Office Access 2000作为软件的数据库系统。该软件从公司领导层到公司各部门到作业班组,按照管理需求对非开挖工程数据资料的操作流程进行切合实际的逻辑设计,形成施工主体技术参数、相关辅助信息和人力、物力、财力数据的有机综合管理系统。而且可以直接从窗体输入数据资料,相应的输出Excel、Word形式的数据资料,方便了工程进展情况的查看和资料的整理。软件中根据非开挖工程的要求,相对应的窗体之间创建了关联。软件可以在Windows 9X操作平台下运行,具有窗体友好、操作方便、运行可靠稳定等优点。     

A Large Basin on the Near Side of the Moon

The differences between the surface structure of the near side and the far side of the Moon have been topics of interest ever since photographs of the far side have been available. One recurrent hypothesis is that a large impact on the near side has deposited ejecta on the far side, resulting in thicker crust there. Specific proposals were made by P.H. Cadogan for the Gargantuan Basin and by E.A. Whitaker for the Procellarum Basin. Despite considerable effort, no consensus has been reached on the existence of these basins. The problem of searching for such a basin is one of finding its signature in a somewhat chaotic field of basin and crater impacts. The search requires a model of the topographic shape of an impact basin and its ejecta field. Such a model is described, based on elevation data of lunar basins collected by the Lidar instrument of the Clementine mission and crustal thickness data derived from tracking Clementine and other spacecraft. The parameters of the model are scaled according to the principles of dimensional analysis and isostatic compensation in the early Moon. The orbital dynamics of the ejecta and the curvature of the Moon are also taken into account. Using such a scaled model, a search for the best fit for a large basin led to identification of a basin whose cavity covers more than half the Moon, including the area of all of the impact basins visible on the near side. The center of this basin is at 22 degrees east longitude and 8.5 degrees north latitude and its average radius is approximately 3,160 km. It is a megabasin, a basin that contains other basins (the far side South Pole-Aitken Basin also qualifies for that designation). It has been called the Near Side Megabasin. Much of the material ejected from the basin escaped the Moon, but the remainder formed an ejecta blanket that covered all of the far side beyond the basin rim to a depth of from 6 to 30 km. Isostatic compensation reduced the depth relative to the mean surface to a range of 1–5 km, but the crustal thickness data reveals the full extent of the original ejecta. The elevation profile of the ejecta deposited on the far side, together with modification for subsequent impacts by known basins (especially the far side South Pole-Aitken Basin) matches the available topographic data to a high degree. The standard deviation of the residual elevations (after subtracting the model from the measured elevations) is about one-half of the standard deviation of the measured elevations. A section on implications discusses the relations of this giant basin to known variations in the composition, mineralogy, and elevations of different lunar terranes.