飞机结构X射线裂纹图像智能评定

飞机结构X 射线图像评定过程存在复杂背景下裂纹分割不准、检出难等问题。基于高效层聚合网络提出一种飞机结构X 射线裂纹图像智能评定模型（ELAN-Seg）,将ELAN-Seg 模型和DeepLabv3+模型的射线图像裂纹分割能力进行对比,结合图像处理技术对模型分割的裂纹长度进行评估,利用飞机强度试验及外场维护过程采集的X 射线图像对模型进行验证。结果表明：分割的最小裂纹长度约为3 mm,ELAN-Seg 模型对复杂背景射线图像裂纹分割更加准确,裂纹漏检率小于3.8%,该模型具有工程适用性。     

Solar X-ray Monitor (XSM) on-board Chandrayaan-2 orbiter

The remote X-ray fluorescence spectroscopy is a powerful technique to investigate the elemental abundances in the atmosphere-less planetary bodies. The experiment involves measuring spectra of fluorescent X-rays from lunar surface using a low energy X-ray detector onboard an orbiting satellite. Since the flux of fluorescent X-ray lines critically depend on the flux and spectrum of the incident solar X-rays, it is essential to have simultaneous and accurate measurement of X-ray from both Moon and Sun. In the context of Moon, this technique has been employed since early days of space exploration to determine elemental composition of lunar surface. However, so far it has not been possible to exploit it to its full potential due to various reasons. Therefore it is planned to continue the remote X-ray fluorescence spectroscopy experiment on-board Chandrayaan-2 which includes both lunar X-ray observations and solar X-ray observations as two separate payloads. The lunar X-ray observations will be carried out by Chandra Large Area Soft x-ray Spectrometer (CLASS) experiment; whereas the solar X-ray observations will be carried out by a separate payload, Solar X-ray Monitor (XSM). Here we present the overall design of the XSM instrument, the present development status as well as preliminary results of the laboratory model testing. XSM instrument will have two packages namely – XSM sensor package and XSM electronics package. XSM will accurately measure spectrum of Solar X-rays in the energy range of 1–15 keV with energy resolution ∼200 eV @ 5.9 keV. This will be achieved by using state-of-the-art Silicon Drift Detector (SDD), which has a unique capability of maintaining high energy resolution at very high incident count rate expected from Solar X-rays. XSM onboard Chandrayaan-2 will be the first experiment to use such detector for Solar X-ray monitoring.     

脉冲星导航中最优脉冲星组合选取方法

分析了X射线脉冲星导航原理,发现脉冲星的位置和脉冲到达时间(Time of Arrival,TOA)的测量误差直接影响导航精度.为优选导航脉冲星组合,在误差协方差分析的基础上,提出了一种导航脉冲星组合优选方法.该方法分别定义了优选指标位置精度因子(Positioning Dilution of Precision,PDOP)和脉冲星优选指标(Pulsars Select Criteria,PSC),不仅考虑了脉冲星空间位置分布,还考虑了测量噪声差异对导航误差的影响.最后以25颗信号品质较好的脉冲星为例,仿真验证了所提方法的有效性.     

一种新颖的无人机侦察图像分区域压缩算法

针对无人机侦察图像及其在军事运用上的特点,分析并证明了基于小波变换的压缩技术在无人机侦察图像压缩方面是一种很好的解决方案,根据某型无人机侦察图像设计了一种基于小波变换的分区域压缩算法,取得了良好且满意的图像压缩效果和实时传输效果.最后,阐述了基于小波变换的侦察图像压缩的关键技术.     

磁扩散电弧运动图像实验研究

电弧等离子体与气体之间的相互作用机理研究一直在低温等离子领域受到关注。为了获得比较均匀的大面积直流电弧等离子流，设计了一种利用外磁场驱动电弧旋转的等离子发生器。利用高速摄影技术研究了大气压条件下氩电弧等离子体在弧室中的运动情况，得到了典型的螺旋型电弧照片，分析了外部磁场对电弧运动形状、电弧电压的影响和弧根附近的气流扰动情况，认为磁场分布的不均匀性是导致电弧形状多样性和不稳定性的主要原因，而阴极烧蚀引起了弧根区气流扰动的不对称性。     

序列图像中直线边缘快速提取和匹配

针时飞行器视觉导航等实时性较强的应用,给出了一种在航空序列图像中进行直线边缘快速提取和匹配的方案。在提取直线边缘时,运用了当前速度较快的邻接元素标记方法,从而提高了直线边缘提取速度。而在时直线边缘进行匹配时,给出了一种分三步走的方案,并提出了一种能够有效降低噪声影响的度量方式。首先选择3条直线边缘作为参考模型,在直线边缘的方向、位置以及物理特性的约束下构建候选匹配基,然后在基于矢量技术的基础上确定与参考模型基相对应的匹配模型,在此基础上再确定其他直线边缘之间的对应关系。试验结果表明,本文的直线边缘匹配方法比现有的方法速度提高了30倍以上,能够有效地满足一些实时性较强的应用。     

不同工件超光滑表面残余应力的测试研究

通过对玻璃、陶瓷、金属3个试件进行超精密加工,使试件表面粗糙度达到纳米级,采用非破坏性的X射线衍射sin2ψ法测量原理对不同试件的残余应力进行了测试研究。结果表明:在本试验条件下,3个试件都只存在残余压应力,并且陶瓷的残余压应力最大,金属残余压应力最小。     

HXMT satellite for space hard X-ray observation

In this paper, the Hard X-ray Modulation Telescope mission is introduced. Its primary objective is to perform the hard X-ray all sky survey of high resolution and high sensitivity. The expected angular resolution and position accuracy of the satellite are better than 10^′ and 2^′, respectively. The preliminary mission design is analyzed. And a new attitude subsystem scheme is presented to meet the high precision demand of attitude determination. A conclusion is drawn that the mission design is feasible. The possible launch of it will significantly advance the astrophysical study.     

Particle acceleration and kinematics in solar flares – A Synthesis of Recent Observations and Theoretical Concepts (Invited Review)

We review the physical processes of particle acceleration, injection, propagation, trapping, and energy loss in solar flare conditions. An understanding of these basic physical processes is inexorable to interpret the detailed timing and spectral evolution of the radiative signatures caused by nonthermal particles in hard X-rays, gamma-rays, and radio wavelengths. In contrast to other more theoretically oriented reviews on particle acceleration processes, we aim here to capitalize on the numerous observations from recent spacecraft missions, such as from the Compton Gamma Ray Observatory (CGRO), the Yohkoh Hard X-Ray Telescope (HXT) and Soft X-Ray Telescope (SXT), and the Transition Region and Coronal Explorer (TRACE). High-precision energy-dependent time delay measurements from CGRO and spatial imaging with Yohkoh and TRACE provide invaluable observational constraints on the topology of the acceleration region, the reconstruction of magnetic reconnection processes, the resulting electromagnetic fields, and the kinematics of energized (nonthermal) particles. This revised version was published online in June 2006 with corrections to the Cover Date.     

A magnetic explanation for the rapid burster

The observations of X-ray Type II bursts from the low-mass X-ray binary MXB 1730-335 can be explained by a particular form of magnetic gating in the presence of steady external accretion. The requirements are a strong magnetic field of the neutron star (7×10¹¹–2×10¹² gauss at the surface), rotational symmetry and alignment of the field axis with the axis of a steadily accreting disk to within 6°.