气温日较差研究进展:变化趋势及其影响因素

从日较差的变化趋势、影响因素以及人类活动对气候变化影响的指示3个方面对日较差的研究进行了总结和概括。观测数据以及气候模式模拟的结果表明,全球气温日较差在近半个多世纪以来呈下降趋势,而这种下降趋势不仅仅是自然变化的结果,还受到人类活动的影响。辐射、云量、气溶胶、下垫面的变化、水汽、降水以及航迹云等因素都能对日较差的变化造成影响。日较差的"周末效应"以及城市化过程中日较差的变化相对于平均气温的变化,能够更有效地指示人类活动对气候变化的影响。     

Microscopic morphology and size distribution of particles in PM<Subscript>2.5</Subscript> of Guangzhou City

Samples of airborne PM_2.5 particles in Guangzhou urban area were collected during the autumn of 2006 and the spring of 2007. The morphologies and elemental compositions of individual particles were determined by Scanning Electron Microscopy coupled with Energy Dispersive X-ray Spectrometer (SEM-EDX). The obtained images were further analyzed for size distribution by an image analysis system. Based on the morphology, particles in PM_2.5 were classified into four groups: soot aggregates, minerals, fly ash and others. The amount of soot aggregates and minerals were higher than that of fly ashes. The distributions of particles by number and size in two seasons were bimodal with 90% less than 1.0 μm in diameter. The primary peak from the autumn samples was in the size range of 0.4 ~ 0.5 μm, and 0.3 ~ 0.4 μm for the spring samples. More soot aggregates (36.1%) and minerals (61.5%) were found than fly ash (2.4%) in autumn, but soot aggregates (89.9%) was the dominant particle type in spring. The size distribution of particles according to the volume was generally opposite to that according to the number. Particles less than 1.0 μm were as high as 89.5% in number but contributed only 18.9% in volume, indicating that fine particles contributed relatively little in volume although existing in large numbers.     

红外焦平面探测器信息获取与预处理电路设计

针对中国科学院上海技术物理研究所研制的1500元红外线列焦平面探测器的输出特性,提出了以低噪声运放为核心的信息获取电路和以FPGA(Field Programmable Gate Array)为核心的数据预处理的设计方案,实现了驱动电路和探测器的良好匹配,较好地发挥了探测器高灵敏度的特性.测试结果表明,该方案不仅对系统获得优于50 mK噪声等效温差的高灵敏度成像起到了重要作用,足够宽的量化设计还保证了系统的动态范围和图像的丰富层次.该设计方案已成功应用在一些其他类型的红外焦平面探测器中.     

TM图象数字镶嵌的几何精度分析及镶嵌方法的探讨

本文对ＴＭ数字镶嵌图象的内部几何精度进行分析后指出，传统的利用选取控制点建立图象间坐标转换方程，并利用此方程对图象进行处理，实施图象镶嵌的方法，在保证镶嵌图象几何精度方面存在着不足，用此方法得到的ＴＭ镶嵌图象的内部几何误差约８个象元；在对传统的图象数字镶嵌方法进行分析的基础上，笔者总结大量工作的经验并参照前人的作法，在选定的地图投影下利用旋转方法对ＴＭ图象进行处理，进而完成镶嵌工作、这种方法舍去了控制点选取的繁复过程，使镶嵌工作变得简单，同时可保证ＴＭ镶嵌图象的几何畸变很小，经检测，镶嵌后的ＴＭ图象内部几何误差小于２个象元。     

Self-similar solution of hot accretion flows with ordered magnetic field and outflow

Observations and numerical magnetohydrodynamic (MHD) simulations indicate the existence of outflows and ordered large-scale magnetic fields in the inner region of hot accretion flows. In this paper, we present the self-similar solutions for advection-dominated accretion flows (ADAFs) with outflows and ordered magnetic fields. Stimulated by numerical simulations, we assume that the magnetic field has a strong toroidal component and a vertical component in addition to a stochastic component. We obtain the self-similar solutions to the equations describing the magnetized ADAFs, taking into account the dynamical effects of the outflow. We compare the results with the canonical ADAFs and find that the dynamical properties of ADAFs such as radial velocity, angular velocity and temperature can be significantly changed in the presence of ordered magnetic fields and outflows. The stronger the magnetic field is, the lower the temperature of the accretion flow will be and the faster the flow rotates. The relevance to observations is briefly discussed.     

A steady-state solution for warped accretion discs

We consider a thin accretion disc warped due to the Bardeen–Petterson effect, presenting both analytical and numerical solutions for the situation in which the two viscosity coefficients vary with radius as a power law, with the two power-law indices not necessarily equal. The analytical solutions are compared with numerical ones, showing that our new analytical solution is more accurate than the previous one, which overestimated the inclination change in the outer disc. Our new analytical solution is appropriate for moderately warped discs, while for extremely misaligned discs only a numerical solution is appropriate.     

Variability of Extended Bipolar Regions

Using NSO/Kitt Peak synoptic charts from 1975 to 2003, we group the main solar magnetic fields into two categories: one for active regions (ARs) and the other for extended bipolar regions (EBRs). Comparing them, we find that there exist three typical characteristics in the variability of EBRs: First, there exists a correlation between ARs and EBRs. The phase of EBR flux has a delay nearly two CRs. Second, we find that the EBR flux has two prominent periods at 1.79 years and 3.21 years. The 1.79-year period seems to only belong to large-scale magnetic features. Lastly, the North – South asymmetry of EBR flux is not very significant on a time scale of one solar cycle. However, during solar maxima, its dominance is found to shift from one hemisphere to the other.