A NEW RECEPTOR MODEL:A DIRECT TRILINEAR DECOMPOSITION FOLLOWED BY A MATRIX RECONSTRUCTION

In many cases,monitoring data for ambient airborne particles can be organized in the form of a three-way data table with one way for chemical species,one for sampling periods and one for sites.A directtrilinear decomposition followed by a matrix reconstruction(DTDMR)is developed to analyze such adata table as a whole.The three-way data set is composed into three two-way matrices by a direct trilineardecomposition(DTD).The column vectors of each of the matrices are called‘source profiles’,‘emissionpatterns’and‘site coefficients’respectively.Particulate sources are identified by examining both theirsource profiles and emission patterns.After the sources have been identified,emission patterns and sitecoefficients are used to produce a three-way matrix that gives estimates of mass contributions of sourcesto the samples collected at every site in every period.By simulation study,not only has the method beenverified,but a good indicator has been found that shows the number of factors(i.e.sources)in thesystem.Unlike other receptor models,DTDMR does not require source profile data and does not involvetrial-and-error procedures.Since DTDMR identifies sources based on variations in two dimensions,it hasa higher potential to distinguish two sources that have similar chemical compositions.The DTDMRmodel has provided excellent results with simulated data and has been applied in a real world three-waydata set.     

直接解释地表地质构造的重力异常剖面的近似方法

前言关于求解引起重力异常的地质体形状的问题,在一般情况下还没有直接的解法.对这种问题.为了求得严格的解必须求助于尝试法(迭代法).对于二度地质体,博特(1960)、福尔尼埃和克鲁皮卡(1973)等人曾较详细地讨论过这一问题.对某些理想化的物体,斯基尔斯(1963)还提出了估计最大深度的方法.对于异常地质体的一般形状和密度差作     

Impacts of the Detection of Cassiopeia A Point Source

Very recently the Chandra first light observation discovered a point-like source in the Cassiopeia A supernova remnant. This detection was subsequently confirmed by the analyses of the archival data from both ROSAT and Einstein observations. Here we compare the results from these observations with the scenarios involving both black holes (BHs) and neutron stars (NSs). If this point source is a BH, we offer as a promising model a disk-corona type model with a low accretion rate in which a soft photon source at approximately 0.1 keV is Comptonized by higher energy electrons in the corona. If it is an NS, the dominant radiation observed by Chandra most likely originates from smaller, hotter regions of the stellar surface, but we argue that it is still worthwhile to compare the cooler component from the rest of the surface with cooling theories. We emphasize that the detection of this point source itself should potentially provide enormous impacts on the theories of supernova explosion, progenitor scenario, compact remnant formation, accretion to compact objects, and NS thermal evolution.     

磁层顶的法向和形状

利用ISEE1& 2 ,AMPTE/IRM和IMP8的高分辨率数据 ,以及MV和TD分析法首次给出了在同一辨认原则下找到的所有磁层顶穿越的法线方向 .在此基础上 ,用分段拟合法研究了磁层顶的平均位形 .结果表明 :(ⅰ )大多数磁层顶穿越是切向间断面 ;(ⅱ )赤道面内的磁层顶存在着某种不对称性 ;(ⅲ )无论行星际磁场南向还是北向 ,夜间一侧的磁层顶截面的张角明显大于白天一侧 ,现有经验模型采用的简单单一曲线可能难以完整描述整个磁层顶的位形 .     

加勒比海的一次非加深扰动的诊断研究(节译)

2、天气形势a、天气和云的分布文章中扰动例子是发生在1966年7月5日小安的列斯群岛的东南方。它开始增强向西北方向移到加勒比海,在那里五天内完全消失。选择7月6日和7日来研究,因为在这个时期里,扰动曾达到它最大强度,     

中国稻田甲烷产生和排放研究 Ⅱ.模式研究和减排措施

主要介绍了近 2 0年来稻田甲烷排放的模式研究和排放量的估算以及减少稻田甲烷排放的措施。数值模式是估算稻田甲烷排放量的一条有效途径 ,模式的研究现在正处于发展阶段。介绍了几个主要的模型 ,既有物理过程模型也有经验模型。年排放量的估算范围为 6 79～ 4 1 4Tg ,随着技术的发展和大量实验的进行估算值的精度正得到不断的提高。减排措施是减少稻田甲烷排放的必要手段 ,但是目前的减排技术均处于研究阶段 ,应用还不成熟     

磁暴期间极光椭圆与极盖区电离层效应比较研究--F区负暴

联合利用EISCAT和E-Svalbard非相干散射雷达数据,研究l997年5月强磁暴期间向阳侧极盖与极光椭圆区电离层F区负暴.发现在磁暴主相和恢复相初期,极光椭圆和极盖区电离层都在大约l90km高度出现类似F1的峰,F2主峰完全消失,F区电子密度大幅度下降.但离子温度的变化在两个区域很不相同,在极光椭圆区大幅度升高,而在极盖区没有显著变化,反映出引起F区负暴的主要机制在两个区域不尽相同.强对流电场引起大气焦耳加热与离子增温而使O+离子消失的化学反应速率增大所导致的电离损失,对极光椭圆区负暴起主要作用;而输运过程,特别是持续长达数小时的沿场上行离子流,对极盖区负暴起重要作用.磁暴主相期间,当EISCAT雷达位于等离子体对流涡旋转换区下方时,在无焦耳加热与离子摩擦增温的情况下,观测到由顶部电离层O+离子沿场高速外流引起的F区电子密度耗空.