站式全景遥感影像展示方法与应用技术研究

虚拟漫游技术已成功应用到社会各个领域,传统漫游技术如VRML(Virtual Reality Modeling Language)、Quick Time、PTGui(Panorama Tools)等存在集成难度大、建模时间长、投入成本高等问题。本文基于全景相机以及Pano2vr、Dynamic-Photo HDR、Photoshop等软硬件环境,研发搭建了一整套旅游景区全景影像采集与展示平台。该平台具有良好的沉浸性、多视角浏览、实现方法简单、搭建快速等优点,为旅游景点、酒店、历史文化名胜等场景的360度实景展示提供了有效地工程化解决途径。     

全景深度图像精度分析及优化方法研究

针对三维激光点云数据生成360°全景深度图像存在像素分辨率不均匀的问题,提出一种顾及目标量测精度及可见度的全景深度图像生成方法,在保证全景影像表达地物的完整性的前提下提高其数据的存取精度。通过坐标转换和投影变换生成与全景影像匹配的全景深度图像;基于摄影成像原理分析摄影中心高度、深度值和像素分辨率之间的关系,得到不同深度处目标分辨率随摄影中心升高趋于一致的结论;综合分析地面目标分辨率和杆状目标尤其是树冠对树干的遮挡问题,确定特定场景下生成全景深度图像的最佳摄影中心位置并重新生成深度图像。实验分析表明,该方法能够在保证杆目标可见度的前提下提高地面目标量测精度。     

Numerical estimation of effective diffusion coefficients for charged porous materials based on micro-scale analyses

In order to describe diffusive transport of solutes through a porous material, estimation of effective diffusion coefficients is required. It has been shown theoretically that in the case of uncharged porous materials the effective diffusion coefficient of solutes is a function of the pore morphology of the material and can be described by the tortuosity (tensor) (Bear, 1988 [1]). Given detailed information of the pore geometry at the micro-scale the tortuosity of different materials can be accurately estimated using homogenization procedures. However, many engineering materials (e.g., clays and shales) are characterized by electrical surface charges on particles of the porous material which strongly affect the (diffusive) transport properties of ions. For these type of materials, estimation of effective diffusion coefficients have been mostly based on phenomenological equations with no link to underlying micro-scale properties of these charged materials although a few recent studies have used alternative methods to obtain the diffusion parameters (Jougnot et al., 2009; Pivonka et al., 2009; Revil and Linde, 2006 2, 3 and 4). In this paper we employ a recently proposed up-scaled Poisson–Nernst–Planck type of equation (PNP) and its micro-scale counterpart to estimate effective ion diffusion coefficients in thin charged membranes. We investigate a variety of different pore geometries together with different surface charges on particles. Here, we show that independent of the charges on particles, a (generalized) tortuosity factor can be identified as function of the pore morphology only using the new PNP model. On the other hand, all electro-static interactions of ions and charges on particles can consistently be captured by the ratio of average concentration to effective intrinsic concentration in the macroscopic PNP equations. Using this formulation allows to consistently take into account electrochemical interactions of ions and charges on particles and so excludes any ambiguity generally encountered in phenomenological equations.     

一类信号恢复问题的投影迭代硬阈值算法

本文给出了基于L₀模求解该问题的非凸模型,借助于稀疏正则化方法来克服问题的不适定性。该模型利用紧小波框架对信号进行稀疏逼近,并利用L₀模度量稀疏性。提出了求解该模型的投影迭代硬阈值算法,并证明了算法的全局收敛性。该算法每一步都有闭式解,计算过程简洁高效。数值实验表明,方法在重建信号的视觉质量和量化指标方面均优于所对比的pFISTA方法。     

梅汛期区域性暴雨的多尺度分析及临近预警

利用常规观测数据、NECP1°×1°逐6 h再分析资料、FY2E卫星黑体亮度温度TBB资料以及南京、常州多普勒天气雷达产品,对2012年江苏出梅之前的最后一场区域性暴雨过程进行多尺度分析。在此基础上,探索该类暴雨的临近预警线索,结果表明:(1)此次过程的雨带呈准纬向分布,属于典型的梅汛期静止锋降水。过程中主要有两次降水集中时段,两个阶段的降水性质存在差异,但都具备较高的降水效率。(2)中高纬大范围稳定的阻塞形势,为此次持续性暴雨过程的产生提供了有利的大尺度环流背景。而在此过程中,两段降水集中期的形成与地面触发系统的出现和维持有着较为密切的联系。(3)此次过程中两段降水集中期内的物理量特征以及TBB的演变情况和其对应的降水特征存在异同。(4)雷达特征分析表明,此次过程具有较高的降水效率和较长的持续时间。实际业务工作中可以通过判断回波的质心高度和边界层风速有无跃增来估计降水效率的潜势。当推断较高的降水效率潜势将持续较长时间时,应及时发布暴雨警报。     

The symbiotic star CH Cygni – I. Non-thermal bipolar jets

Very Large Array surface brightness and spectral index maps of the evolving extended emission of the triple symbiotic star CH Cygni are presented. These are derived from observations at 4.8, 8.4 and 14 GHz between 1985 and 1999. The maps are dominated by thermal emission around the central bright peak of the nebula, but we also find unambiguous non-thermal emission associated with the extended regions. Our observations confirm that this is a jet. The central region has been associated with the stellar components through Hubble Space Telescope imaging. If the jets are the result of ejection events at outburst, expansion velocities are consistent with those from other measurement methods. We propose that the non-thermal emission is caused by material ejected in the bipolar jets interacting with the circumstellar wind envelope. The resulting shocks lead to local enhancements in the magnetic field from the compact component of the order of 3 mG.