钛合金表面抗激光涂层损伤特性及热效应影响研究

实验研究了钛合金和高反射型陶瓷涂层材料抗连续型激光烧蚀的损伤及温度分布特性，并从热效应影响角度对比分析了二者在抗激光损伤效果方面的差异性。研究结果表明：相比于钛合金，高反射型陶瓷涂层材料能有效增强钛合金基底抗激光损伤的能力；在同等激光功率密度辐照下，陶瓷涂层材料能有效提升钛合金基底耐受激光辐照的时间长度。实验结果表明该陶瓷涂层材料的激光损伤阈值比钛合金高约5.8倍。实验发现陶瓷涂层温升速率高于钛合金，但由于陶瓷材料具有较高的反射特性，以及良好的热吸收和热传导特性，因此能使由激光辐照产生的热量在其表面较快地扩散，而降低向基底方向传导的程度，最终提升陶瓷涂层的抗激光损伤阈值。     

提高图像轮廓清晰度的快速插值放大方法

分析了当前主要的高清晰度图像插值放大方法,为实现快速放大而选择了基于图像轮廓插值改善清晰度的技术路线,并在已有算法的基础上开展了进一步的研究.提出了新的图像轮廓线光顺数值算法,对轮廓线划分的两类子区域提出了精度更高的插值算法.最后,以典型平面图形的图像和由3DMax生成的三维渲染图像为例对本文方法进行检验,与双线性插值结果的对比说明,该方法可以明显改善插值放大效果.     

一种基于高分辨率距离像自动目标识别新方法

提出了一种基于高分辨率距离像的联合对准与识别新方法。该方法结合功率变换的使用，在利用8米雷达目标实测数据进行的识别实验中，获得了较高的正确识别率。     

谐波传动共轭齿廓的运动学仿真研究

根据包络理论，通过建立谐波齿轮传动共轭齿廓分析的通用数学模型，在已知柔轮齿廓的条件下可求得与之共轭的刚轮理论齿廓的离散点，通过最小二乘拟合的方法求得刚轮的工作齿廓，并通过啮合区段干涉检验法来校验齿廓的重叠干涉，最后通过计算机程序对所求的刚、柔轮工作齿廓进行运动学仿真以验证所求工作齿廓的合理性，还通过实例对程序进行了验证。本文的方法为探索谐波齿轮用新型工作齿廓提供一条可行的途径，并使小速比谐波齿轮传动变得可行。     

UVCS/SOHO Observations of Spectral Line Profiles in Polar Coronal Holes

Ultraviolet emission line profiles have been measured on 15-29 September 1997 for H I 1216 Å, O VI 1032, 1037 Å and Mg X 625 Å in a polar coronal hole, at heliographic heights ? (in solar radii) between 1.34 and 2.0. Observations of H I 1216 Å and the O VI doublet from January 1997 for ? = 1.5 to 3.0 are provided for comparison. Mg X 625 Å is observed to have a narrow component at ? = 1.34 which accounts for only a small fraction of the observed spectral radiance, and a broad component that exists at all observed heights. The widths of O VI broad components are only slightly larger than those for H I at ? = 1.34, but are significantly larger at ? = 1.5 and much larger for ? > 1.75. In contrast, the Mg X values are less than those of H I up to 1.75 and then increase rapidly up to at least ? = 2.0, but never reach the values of O VI.     

基于中性层偏移的Z型材滚弯成形回弹预测

以提高大截面Z型材四轴滚弯成形精度为目的，通过综合考虑材料属性、几何特征和成形半径等因素对回弹的影响，建立了引入中性层偏移的大截面Z型材弯曲回弹解析模型，研究了7075-O和7475-O铝合金Z型材在不同滚弯成形半径下的回弹规律，并进行滚弯成形实验验证。结果表明，与忽略中性层偏移影响的型材回弹预测经验模型相比，基于中性层偏移的回弹预测模型能够准确预测大截面Z型材的回弹量，在相同的曲率半径下，预测回弹变形的最大相对误差从11.681%减小到3.347%。     

On kinematics of gas clouds in the broad-line region of active galactic nuclei and quasars

The kinematics of gas clouds in broad-line region of active galactic nuclei and quasars is considered. The motion of the clouds is governed by three forces — gravitational influence from the central supermassive body, radiational pressure from the continuum radiation, and resistance of the intercloud medium. Clouds moves radial but only outward motion gives a velocity field, which is in accordance with the observational data. The profiles of the permited lines are obtained in some simplify assumptions for the emissive capacity of the gas in clouds, and are in good agreement with the observational data. In the framework of the model under consideration there is a possibility to estimate some physical parameters of the nuclei such as mass of the central body and density of the intercloud medium.     

星载微波传感器大气温湿度物理反演算法研究

针对我国下一代静止轨道微波探测器资料应用的需求,对微波50~60GHz和183GHz的温湿遥感通道开展了不同大气条件下探测敏感高度的模拟,发现大气散射对微波探测影响明显,尤其是近地面通道,在未来数据应用时需加以注意。提出一种基于一维变分的大气温湿度廓线物理反演算法。以美国最新一代气象卫星Suomi NPP搭载的ATMS(Advanced Technology Microwave Sounder)获取的观测资料为研究对象,RTTOV(Radiative Transfer for TOVS)快速辐射传输模式为前向算子,利用一维变分算法开展了温湿度廓线反演单点试验。研究发现:地表参数对微波亮温,尤其是地面通道影响较大。同时,反演所需背景场对反演结果影响较明显,反演所得温度与背景场较接近。     

Probing the origin of the iron Kα line around stellar and supermassive black holes using X-ray polarimetry

Asymmetric, broad iron lines are a common feature in the X-ray spectra of both X-ray binaries (XRBs) and type-1 Active Galactic Nuclei (AGN). It was suggested that the distortion of the Fe Kα emission results from Doppler and relativistic effects affecting the radiative transfer close to the strong gravitational well of the central compact object: a stellar mass black hole (BH) or neutron star (NS) in the case of XRBs, or a super massive black hole (SMBH) in the case of AGN. However, alternative approaches based on reprocessing and transmission of radiation through surrounding media also attempt to explain the line broadening. So far, spectroscopic and timing analyzes have not yet convinced the whole community to discriminate between the two scenarios. Here we study to which extent X-ray polarimetric measurements of black hole X-ray binaries (BHXRBs) and type-1 AGN could help to identify the possible origin of the line distortion. To do so, we report on recent simulations obtained for the two BH flavors and show that the proposed scenarios are found to behave differently in polarization degree and polarization angle. A relativistic origin for the distortion is found to be more probable in the context of BHXRBs, supporting the idea that the same mechanism should lead the way also for AGN. We show that the discriminating polarization signal could have been detectable by several X-ray polarimetry missions proposed in the past.