Discrimination of sedimentary facies by association analysis

The ability of association analysis to discriminate sedimentary facies was tested on Purdy's modal analyses of modern sediments of the Great Bahama Bank. Purdy's data set has served in the past as a standard reference for evaluating various multivariate classification algorithms. In order to adapt Purdy's data to association analysis, the percent abundance of the 12 constituents was converted to binary form by dichotomizing each variable on its mean value. The results obtained by association analysis are virtually identical to those obtained by Purdy and other authors. The same four main sedimentary facies were discriminated; 86% of the samples were identically classified (97% when misclassified borderline cases are counted as matches); the total partition variance of the classification is only negligibly greater (4%); and the grouping of the variables yielded the same four groups. The rank order of the three division-attributes responsible for the sample classification is fines, oolites, and corals. Association analysis has been employed by other authors to differentiate meaningful facies groups in studies of ancient reef carbonates, modern reef sediments, and heavy minerals in stream sediments. In all these studies, the results were found to be compatible with those obtained by using the continuous quantitative measurements, indicating that qualitative binary data may often be sufficient for the purpose of facies discrimination in many branches of geology and that association analysis is an effective method for this purpose.     

The acceleration of minor ion species in the solar wind

This paper provides a comprehensive analysis of the dynamics of the flow of minor ion species in the solar wind under the combined influences of gravity, Coulomb friction (with protons), rotational forces (arising from the Sun's rotation and the interplanetary spiral magnetic field) and wave forces (induced in the minor ion flow by Alfvén waves propagating in the solar wind). It is assumed that the solar wind can be considered as a proton-electron plasma which is, to a first approximation, unaffected by the presence of minor ions. In the dense hot region near the Sun Coulomb friction accelerates minor ions outwards against the gravitational force, part of which is cancelled by the charge-separation electric field. Once the initial acceleration has been achieved, wave and rotational forces assist Coulomb friction in further increasing the minor ion speed so that it becomes comparable with, or perhaps even exceeds, the solar wind speed. A characteristic feature of the non-resonant wave force is that it tends to bring the minor ion flow into an equilibrium where the radial speed matches the Alfvén speed relative to the solar wind speed, whereas Coulomb friction and rotational forces tend to bring the flow into an equilibrium where the radial speed of the minor ions equals the solar wind speed. Therefore, provided that there is sufficient wave energy and Coulomb friction is weak, the minor ion speed can be trapped between these two speeds. This inteststing result is in qualitative agreement with observational findings to the effect that the differential flow speed between helium ions and protons is controlled by the ratio of the solar wind expansion time to the ion-proton collision time. If the thermal speeds of the protons and minor ions are small compared to the Alfvén speed, two stable equilibrium speeds can exist because the rapid decrease in the Coulomb cross-section with increasing differential flow speed allows the non-resonant wave force to balance Coulomb friction at more than one ion speed. However, it must be emphasized that resonant wave acceleration and/or strong ion partial pressure gradients are required to achieve radial speeds of minor ions in excess of the proton speed, since, as is shown in Section 4, the non-resonant wave acceleration on protons and minor ions are identical when their radial speeds are the same, with the result that, in the solar wind, non-resonant wave acceleration tends (asymptotically) to equalize minor ion and proton speeds.     

Observations of the structure and evolution of solar flares with a soft X-ray telescope

132 soft X-ray flare events have been observed with The Aerospace Corporation/Marshall Space Flight Center S-056 X-ray telescope that was part of the ATM complement of instruments aboard Skylab. Analyses of these data are reported in this paper. The observations are summarized and a detailed discussion of the X-ray flare structures is presented. The data indicated that soft X-rays emitted by a flare come primarily from an intense well-defined core surrounded by a region of fainter, more diffuse emission. Loop structures are found to constitute a fundamental characteristic of flare cores and arcades of loops are found to play a more important role in the flare phenomena than previously thought. Size distributions of these core features are presented and a classification scheme describing the brightest flare X-ray features is proposed. The data show no correlations between the size of core features and: (1) the peak X-ray intensity, as indicated by detectors on the SOLRAD satellite; (2) the rise time of the X-ray flare event, or (3) the presence of a nonthermal X-ray component. An analysis of flare evolution indicates evidence for preliminary heating and energy release prior to the main phase of the flare. Core features are found to be remarkably stable and retain their shape throughout a flare. Most changes in the overall configuration seem to be the result of the appearance, disappearance or change in brightness of individual features, rather than the restructuring or re-orientation of these features. Brief comparisons with several theories are presented.     

MODIS数据在乌鲁木齐地区植被景观动态监测中的应用

根据EOS／MODIS卫星时次高覆盖面广的特征，选取从4．10月的MODIS晴空资料，对整个乌鲁木齐地区植被景观进行动态监测，利用植被指数最大合成法制作了每月植被指数专题图。为了能够结合物候更好地分析乌鲁木齐地区植被随季节变化趋势以及不同时期植被生长状况，我们还制作了植被景观专题图及其变化评价图。评价图的优势在于能直观地反映植被变化的趋势，并能将变化的程度数字化，还可以根据不同的评价图叠加DEM做相应的分析。为乌鲁木齐地区植被变化研究提供有效的依据。     

潍坊"5.19"强对流天气过程分析

利用常规气象资料、T213实况分析资料、全国雷达拼图资料、济南多普勒雷达和潍坊本市雷达资料及自动站资料，对2003年5月19日一次强对流天气过程进行分析，结果表明，快速东移南下的横槽极其槽后的冷空气使不稳定层结加强，是触发此次对流发生的原因。而低层暖湿气流的存在为其发展提供了必要的动力和水汽条件。     

YTT事件在洛川黄土中的记录:来自固定铵和速效钾的证据

Toba火山活动是第四纪最大的火山事件,其中最年轻的约0．074Ma的火山活动被称为YTT事件（The Youngest Toba Tuff）。已有的研究表明,YTT事件对第四纪的环境气候变化具有重要的影响,黄土S1／L1界面处的磁化率和粒度等因子突变所反映的夏季风迅速回撤可能响应了这一事件。对洛川黄土S1／L1界面处的固定铵和速效钾进行了研究,结果表明,YTT在洛川黄土S1／L1界面处有很清楚的记录,具体表现为固定铵和速效钾的特殊异常。固定铵的异常主要记录了YTT事件所产生的酸雨沉降,速效钾的异常则是由于YTT微细火山灰尘在黄土剖面及其广阔的物源区伴随酸雨沉降的结果,厚达1m的异常带表明末次冰期冬季风逐渐强盛和南移的过程。     

浙西南淡竹花岗闪长岩中锆石的成因研究及其地质意义

本文对浙西南地区淡竹花岗闪长岩中的锆石群进行了形态学、地球化学和年代学的系统研究。研究结果表明, 该花岗闪长岩中存在两种不同类型的锆石: 岩浆锆石和变质锆石。前者为自形—半自形的长柱状晶体, 无色透明, 富含岩浆和矿物包裹体, 其背散射电子图像 (BSE图像) 显示出均匀的内部构造 (少数具有韵律环带构造), 其晶型指数落在钙碱性系列花岗闪长岩的范围内; 后者大多数以增生边的形式围绕岩浆锆石生长, 极少量呈他形的粒状晶体, 呈黄褐色—半透明, 其BSE图像亦呈现均匀的内部构造。这两类锆石在化学成分上有较大的差异, 表现为岩浆锆石比变质锆石明显地富U、Th、Y等阳离子置换元素。锆石LAICPMS UPb定年分析结果表明, 岩浆锆石和变质锆石分别形成于1875±33 Ma和209±12 Ma两个不同的时代, 为浙闽运动和印支运动在浙西南地区的表现提供了有力的客观证据。     

东北冷涡引发的局地暴雨数值模拟研究

利用CDAS-NCEP/NCAR 再分析资料,应用Penn State/NCAR的高分辨率中尺度模式MM5V3-7,成功模拟出2005年7月9—12日东北冷涡诱发的一次连续雷雨过程,重点分析了7月9日造成沈阳及周边地区的一次局地暴雨过程,并对其中的一个连续发展的中β尺度对流系统的演变、中尺度结构特点进行了研究。结果表明：冷涡总是以水平旋转的中高层的干冷空气堆作为其结构特点。在冷涡的东南侧高空干冷堆的边缘区域,轨迹呈直立状,从行星边界层向上穿越整个对流层,显示出该地区存在强对流。干冷堆的边缘区域下方的低层暖湿输送是冷涡局地强对流发展的关键。局地对流发展时,出现干冷堆的边缘区域的S_e上下层接近或者打通现象。