The Doppler Effect and Spectral Energy Distribution of Blazars

The relativistic beaming model is adopted to discuss quantitatively the observational differences between radio-selected BL Lac objects (RBLs) and X-ray-selected BL Lac objects (XBLs), and between BL Lac objects and flat spectrum radio quasars (FSRQs). The main results are the following:(1) In the Doppler corrected color-color(αro^in-αox^in) diagram,XBLs and FSRQs occupy separated regions, while RBLs bridge the gap between them. These properties suggest that similar intrinsic physical processes operate in all the objects under a range of intrinsic physical conditions. (2) Our results are consistent with the results of Sambruna, Maraschi and Urry (1996) from other methods. We show the αxox introduced by Sambruna to be a good index for describing the energy distribution because it represents the intrinsic energy distribution and includes the Doppler correction. (3)The Doppler effect of relativistic beaming is the main mechanism, and the physical differences(such as magnetic fields, electron energies) are also important complementary factors for understanding the relation between XBLs and RBLS.     

基于PCA和极限学习机的高光谱遥感分类研究

针对高光谱遥感分类研究中面临的数据处理效率低、分类结果精度不高等难题,本文在引入极限学习机(ELM)算法的基础上,顾及其在噪声影响下出现稳健性降低的现象,进一步将主成分分析(PCA)应用于ELM的前端,从而构建了一种基于PCA和ELM的联合算法。将该算法与目前常用的神经网络和支持向量机进行对比分析发现:PCA-ELM分类结果的精度最高,其数据处理效率也较高,该算法具有较强的稳健性和泛化能力,适用于高光谱遥感信息的高效提取。     

一种基于NPA的加权“1 V m”SVM高光谱影像分类算法

根据支持向量机(SVM)的计算理论,结合高光谱影像的数据特点,利用最近点算法(NPA)求两类最优超平面,为每类设立一个合理的权指标,提出了基于NPA的加权“1 V m”SVM算法来实现高光谱遥感影像多分类,降低了计算的复杂度和计算量,提高了SVM高光谱遥感影像分类的可操作性和分类效率。     

内蒙古东乌旗沙麦钨矿床成矿机制：来自流体包裹体及稳定同位素的证据

内蒙古东乌旗沙麦钨矿床位于中亚巨型缝合带的最东段,矿床内广泛发育云英岩化,钨矿体主要受NW向断裂构造控制,呈黑钨矿-石英脉状产出在燕山期沙麦岩体（岩性主要为黑云母二长花岗岩）和泥盆系围岩地层（岩性主要为角岩化砂岩、砂砾岩）中。成矿阶段从早到晚分别为：石英-黄玉阶段（Ⅰ）、云英岩-黑钨矿阶段（Ⅱ）和晚期硅化阶段（Ⅲ）。本文对矿床流体包裹体及C-H-O-S同位素进行了研究,结果显示：矿床中普遍发育CO2-H2O包裹体及水溶液气液两相流体包裹体。从成矿早期至成矿晚期,矿床流体中富CO2包裹体逐渐减少,CO2含量逐渐降低。成矿早期可见熔体包裹体与流体包裹体共存的现象,属低盐度、富CO2的岩浆来源流体。矿床成矿作用从早到晚,流体包裹体均一温度分别为279~341℃、196~286℃、103~201℃;流体盐度分别为(1.6~9.1)%NaCleq、(3.0~11.1)%NaCleq、(0.9~4.7)%NaCleq。激光拉曼光谱分析结果显示,流体中的气相主要是CO2,部分含有H2O和CH4。成矿流体从早期中高温、中盐度流体向晚期低温、低盐度流体演化,属NaCl-H2O-CO2±CH4热液体系。矿床稳定同位素研究表明,沙麦钨矿床的成矿流体主要来源于岩浆水,并在成矿晚期混入了大气水。矿床硫的来源与早白垩世岩浆-热液系统或深部幔源岩浆相关,并混入了部分地层硫。综合分析认为,沙麦钨矿为一岩浆期后热液型钨矿床。燕山期侵入体从深部携带成矿物质,经历了岩浆分异和流-熔体相互作用等过程,形成区内岩浆-热液成矿系统。流体的不混溶是导致含钨络合物分解乃至最后沉淀成矿的主要原因。     

偏振激发能量色散X荧光法在地球化学分析中应用及其与波长色散X荧光法的比较

偏振激发能量色散X射线荧光光谱(P-EDXRF)技术是20世纪末出现的新分析技术。国内采用X-Lab2000型仪器的初步研究表明，在总计数时间为600秒时，可以对近30种元素进行定量，检出限为0．5-30μg／g，与国际上发表的文献值基本一致。本工作通过约100个实际样品分析，并与波长色散X射线荧光法(WDXRF)分析结果的比较，对P-EDXRF的分析性能进行了评价。与WDXRF相比，P-EDXRF法具有分析速度快、设备购置费用低、运行成本低、全谱同时采集(有利于发现元素含量异常)等优点，因此特别适合地球化学填图样品的快速分析。而WDXRF在精度要求较高的分析中更具竞争力。     

几种气象因素对云台太阳光谱仪成像质量的影响规律

在多年的太阳光谱观测中，通过观察各种天气条件的变化对光谱仪成像质量的影响，初步总结出使像质优良的几条规律：1）在连续刮风过程中当风突然停止或减弱的短暂时间内像质明显变好；2）当夜间通宵有风而次日天气晴朗时像质变好；3）多云过后的短暂晴天成像优良；4）连接阴雨几天后的开始晴天像抽较好。     

两种北极微型浮游植物的荧光差异性分析

为了利用荧光技术对北极浮游植物的生理生态信息进行系统研究, 本文以实验室培养条件下的两种北冰洋微型浮游植物——柔弱伪菱形藻(Pseudo-nitzschia delicatissima)和海链藻(Thalassiosira sp.)为研究对象, 先采用流式细胞术(Flow Cytometry, FCM)和全荧光光谱法对其活体中色素的静态荧光进行测量, 后利用脉冲调制方法(Pulsed Amplitude Modulation, PAM)对其叶绿素动态荧光信息进行测定, 对两种浮游植物的三类荧光信息进行综合比较分析, 结果表明: 柔弱伪菱形藻的丰度、基础荧光(F0)、光合系统Ⅱ(PSⅡ)光化学的有效量子产量(ΦPSⅡ)及光合电子传递效率(ETR)分别为22×105cell/mL、844、0.247和42.8, 皆高于海链藻的相应值(8×105cell/mL、464、0.185及33.0); 静态荧光和基础荧光分析表明柔弱伪菱形藻细胞内叶绿素a (chl a)含量较高; 海链藻细胞内则具有较高含量的类胡萝卜素, 其对光保护机制依赖性较强。本文初步展示了三类荧光分析法在极地微型浮游植物生理生态研究方面的联合应用。     

Can the bump in the composite spectrum of GRB 910503 be an emission line feature of gamma-ray bursts？

Appearing in the composite spectral data of BATSE, EGRET and COMPTEL for GRB 910503, there is a bump at around 1600 keV. We perform a statistical analysis on the spectral data, trying to find out if the bump could be accounted for by a blue-shifted and significantly broadened rest frame line due to the Doppler effect of an expanding fireball surface. We made an F-test and adopted previously proposed criteria. The study reveals that the criteria are well satisfied and the feature can be interpreted as the blue shifted 6.4 keV line. Prom the fit with this line taken into account, we find the Lorentz factor of this source to be P = 116-9+9 (at the 68% confident level,△x2 = 1) and the rest frame spectral peak energy to be E0,p- 2.96-0.18+0.24 keV. Although the existence of the emission line feature requires other independent tests to confirm, the analysis suggests that it is feasible to detect emission line features in the high energy range of GRB spectra when taking into account the Doppler effect of fireball expansion.