闭式整体叶盘通道五坐标分行定轴加工刀轴矢量规划方法

闭式整体叶盘是新一代航空发动机实现减重增效的关键零件,其通道结构属于典型多约束复杂通道结构。针对闭式整体叶盘通道精加工,提出了一种基于五坐标分行定轴加工的刀轴矢量规划方法。从加工原理上给出了分行定轴加工方法的基本概念,并分析了闭式整体叶盘通道五坐标加工的特征;在刀具预定义和建立检查面球体包围盒层次树结构的基础上,给出了刀轴矢量无干涉区域的计算方法;基于刀位点最短刀长的计算与分析,进行了叶盘通道加工区域划分,建立了分行定轴加工刀轴矢量规划方法。实验验证表明:分行定轴相对五轴联动加工方法不仅可明显提高加工过程中的稳定性和叶片加工表面质量,还可提高叶片精加工效率。     

Characteristics of the telescope Gamma-1 in the coded aperture mode

The efficiency of using the coded aperture on the Gamma-1 telescope to solve a variety of astrophysical problems has been considered. The coded aperture technique is shown to be at a disadvantage in relation to the conventional one so far as discriminating a source from the background is concerned. However, for powerful sources the coded aperture technique has an advantage from the viewpoint of accuracy of source location on the celestial sphere, the resolution of closely spaced sources and the determination of the sizes of sources.     

The polarization of celestial X-rays

The processes by which X-radiation may be emitted by celestial sources are investigated, and the net polarization such radiation would possess is predicted. The amount of polarization observed at the Earth would depend both on the mechanism producing the radiation and on the fractional extent of the source over which it is coherently polarized. Highly polarized X-radiation would suggest synchrotron emission as the source mechanism. Radiation whose polarization is low but nonzero would be produced by synchrotron emission from a source whose magnetic fields are inhomogeneous on a large scale, or by bremsstrahlung of electrons whose velocity vectors lie in one predominant direction. Nonobservable polarization would result from sources of synchrotron radiation whose magnetic fields show small-scale irregularities, from the bremsstrahlung of electrons whose velocity vectors are either random or spherically symmetric in direction over the entire source, or from sources whose mechanism of producing the radiation imparts no net polarization, e.g., thermal radiation from neutron stars, line radiation from electronic shell transitions within atoms, and the inverse Compton effect. Measurement of the net polarization of the X-rays from the several known celestial sources could thus lead to the specification of the mechanisms capable of producing the radiation from such sources.     

一种新的高精度天文导航方法

介绍了一种新的高精度天文导航方法,该方法构建了在天球坐标系中的天文导航姿态与航向解算模型。该模型在不利用惯导姿态数据的前提下进行计算,通过构建的模型演变得到运载体的精确姿态及航向,可以有效校正惯导设备因惯性陀螺漂移而导致的姿态误差与航向误差。     

基于QTM的导航星库划分方法

为了提高星敏感器观测星的检索速度,提出了一种基于球面四元三角网(Quaternary Triangular Mesh,QTM)的导航星库划分方法.该方法首先利用天球的内接正八面体把全天球划分成8个子天区,然后在每个子天区中进行与经纬度相关的剖分和编码,最后扫描恒星星表,把每颗导航星信息划归到相应的子天区内存储.利用此星库进行的局部天球星图识别仿真实验表明该星库具有很高的检索效率.     

Rapid Star Tracking Algorithm for Star Sensor

A rapid star tracking algorithm is proposed. In order to speed up the tracking, three techniques includng parallel star centroiding, sorting, and star catalogue partition are designed for three time-consuming portions in tracking algorithms. The parallel star centroiding is implemented with Field Programmable Gate Array (FPGA) which avoid image storage and transmission. Update rate of star sensor is improved. Sorting star coordinates in star image plane, and then matching, which avoid matching between stars with a long distance in image plane. Star catalogue partition divides the celestial sphere into many small partitions. In star mapping, guide stars are searched in the partitions near the direction of star sensor's boresight is not in the whole celestial sphere and therefore reduced the total number of searched guide stars. The software and hardware performance of tracking algorithms are simulated. Tracking robustness and the tracking speed comparison are tested in the software simulation. In hardware tests, the tracking time in every step is obtained.     

基于球体描述Vague决策的模拟电路故障诊断方法(英文)

提出一种基于球体描述Vague决策的模拟电路故障诊断方法。首先,采用小波变换预处理待测电路输出的电压故障特征。然后,每类样本集训练成一个最小超球体。最后,测试样本由本文定义的模糊决策规则进行判断,其中该规则由测试样本和描述球体中心之间的Vague加权距离得到。该模糊决策规则融合了测试样本正反隶属度值和描述球体的权值,可以有效地处理不确定信息。本文从理论上证明了该决策方法的可靠性。将该诊断方法应用于两种实际电路的测试,并与其他两种诊断方法进行对比。实验结果表明本文方法取得了良好的诊断性能,并减少诊断时间。     

飞机螺桨声场的数值模拟方法

本文给出了预测飞机螺桨在自由空间内幅射的气动声场的一种数值方法。即时域内进行延迟时间积分的一类方法。在该方法中使用片条假设,并考虑厚度声源和负荷声源项作为非紧致声源。计算与实验结果对比表明,该方法和相应软件可作为一种工程手段来使用。      

双轴惯导轴系非正交误差全空间补偿技术研究

旋转调制技术实现了捷联惯导的高精度长航时导航,但轴系非正交误差的存在影响着导航姿态精度。传统轴系非正交误差补偿方法是针对旋转轴停留在固定位置完成的,提出一种全空间的轴系非正交误差补偿方法,不限定旋转轴的转停位置。试验结果证明该误差补偿方法较传统方法更优,对惯导姿态精度提升明显。     

等离子体合成射流对钝头激波的控制与减阻

为了验证等离子体合成射流对超声速流动的流动控制和减阻效果,在考虑热完全气体效应的情况下,工程拟合等离子体热力学属性和输运系数,利用能量源项模型对超声速平板和球头等典型流场结构进行了数值模拟,并取得了与实验较为一致的结果。研究结果表明：对于马赫数为2的超声速平板流动,等离子体合成射流能有效干扰边界层的发展,并诱导产生一系列大尺度结构;对于马赫数为3的球头流场,等离子体合成射流能显著改变激波脱体距离与球头的阻力特性;在放电后第1个周期内,合成射流能使球头平均阻力降低6.3%,而在射流峰值情况下使阻力降低32.0%,激波脱体距离增加2倍,实现了激波控制和流动减阻的预期效果。     

数字闭环光纤陀螺死区机理研究与抑制

在数字闭环光纤陀螺中,死区产生及其附近噪声特性恶化的主要因素可以归结于施加在相位调制器上信号的串扰。根据死区产生机理的不同,提出了偏置相位调制和阶梯波反馈调制两种死区串扰误差因素的观点。通过对这两种死区误差机理的分析和比较,提出了采用模拟相加反馈方案可以避免偏置相位调制死区误差的观点。采用速率转台法测试了光纤陀螺的死区特性,验证了理论仿真和计算的正确性。最后,通过采用三角波相位抖动抑制死区误差技术,将一种高精度光纤陀螺0.08(°)/h的死区误差抑制到0.001(°)/h以下。     

激波风洞气动力试验不确定度影响因素分析

参考北大西洋公约组织和AIAA推荐的风洞试验数据不确定度计算方法,结合激波风洞运行特点,确定激波风洞气动力试验的主要误差源,计算激波风洞13-2标模气动力测量结果的不确定度。采用改变单一变量的方法计算主要误差源对测量结果不确定度的影响程度,辨析对不确定度起主要作用的基本参数。计算结果表明：皮托压力和总压的测量结果对流场参数影响显著,皮托压力的测量结果比总压测量结果对流场参数与气动力测量结果影响更大;降低皮托压力和总压的偏离极限,有利于提高激波风洞气动力试验数据的质量。     

射流中速度和温度的脉动关联及耗散规律

本文采用X热线-冷线组合探头及全速度偏航角标定法,对非等温圆形射流中的脉动关联量以及脉动量的耗散规律进行了实测和分析。得到了Reynolds应力、脉动热通量和Prandtl数的分布。对耗散率的测量结果证实了由满足自模条件导出的Taylor微尺度和湍动能耗散率在中心线上的变化关系是成立的,并且推导了中心线上湍流温度耗散率的表达式。本文的研究还表明,以往模拟计算中,将脉动温度场的时间尺度与脉动速度场的时间尺度之比取为常数的假定是缺乏实验依据的。     

微小型无人机三轴磁强计现场误差校正方法

详细分析微小型无人机导航用三轴磁强计的误差来源,建立三轴磁强计的等效误差模型,提出基于两步估计算法和圆约束非对准误差估计算法的三轴磁强计现场误差校正方法.在充分考虑地磁场偏转和倾斜特性的基础上,提出适合微小型无人机应用的现场数据采样策略,能够在较少的旋转操作下获得较好的采样数据.仿真表明:在所有磁场误差都存在的情况下,...     

Thermal cyclotron radiation from a hot coronal loop with helical magnetic field

The spectral and polarization properties of thermal cyclotron radio emission from a hot coronal loop with a current along the axis are computed. The magnetic field is supposed to have a component along the loop axis as well as a poloidal part due to the current, both components being of comparable magnitude. In this specific configuration a helical magnetic field is present with a remarkable minimum of its absolute value along the loop axis and a maximum at its periphery. The presence of one or two maxima of magnetic field value along the line of sight results in increasing optical thickness of the gyroresonance layers at appropriate frequencies in the microwave band and, therefore, in enhanced radio emission at those harmonics which are optically thin (for example,s=4). These cannot be observed in models with the commonly employed magnetic field configuration (longitudinal along the loop axis).We show that the frequency spectrum of thermal cyclotron radiation from a hot coronal loop with a helical magnetic field differs from that of the standards-component source (with smooth frequency characteristics and polarization corresponding toe-mode) in that plenty of fine structures (line-like features and cut-offs) are present and theo-mode is prevalent in some frequency intervals. The enhanced radio emission at high harmonics and the complicated form of frequency spectrum in the model considered imply that some microwave sources, which are poorly explained in traditional models of solar active regions, may be associated with helical magnetic fields in hot coronal loops. Computations allow one to indicate spectral and polarizational peculiarities of local sources testifying to the presence of a helical magnetic field.     

内嵌高斯白噪声模块的可编程卫星信号模拟源

由于卫星通信的遥测参数和数据格式的多样性,为满足不同卫星测试的要求,需要提供不同的信号源。考虑到成本因素,采用遥测参数和数据格式均可编程卫星信号模拟源。给出了内嵌高斯白噪声模块的可编程卫星信号模拟源的系统组成及工作原理,对其中关键模块——已调副载波生成模块和高斯白噪声生成模块进行了分析讨论,前者采用包括直接数字频率合成方法在内的全数字方法,后者采用延时斐波那契算法和公式法的算法组合。试验结果表明:本方案实现的可编程卫星信号模拟源能够满足多数卫星测试的需要。     

一种高精度小型化星敏感器设计

星敏感器是以恒星为参照系,以星空为工作对象的高精度空间姿态测量装置,提供准确的空间方位和基准,具有高精度、无漂移、工作寿命长等特点.针对星敏感器高精度和小体积的应用需求,基于小型化镜头设计、分体式结构、高集成度电路、"FP GA+ARM"软件等内容,提出了一种高精度小型化星敏感器,解决了狭小空间高度集成的小型化问题,实现了测姿0.6″(3σ)的高精度预期目标.星敏感器样机通过了试验考核,性能符合设计要求,具备全天球搜索恒星定姿的能力.     

The modulation collimator in x-ray astronomy

Modulation collimators have been used in recently reported work to determine the angular sizes and celestial positions of the X-ray sources Sco X-1 and Taurus XR-1 (Crab Nebula) with precisions of 15 to 30. The measurements were made by means of four-grid collimators, star photography and optical imaging of the collimators. In the present paper we discuss (1) the principles and uses of various forms of the modulation collimators as they pertain to X-ray astronomy, (2) several methods for determining the celestial positions of X-ray sources with these collimators, (3) the techniques for the alignment and calibration of these detection systems, (4) an image-forming collimator, and finally, (5) some of the optical properties of these grid systems. The modulation collimator is quite versatile and is particularly suited for measurements from spacecraft with relatively poor pointing capability. Thus it should be a useful tool in X-ray astronomy for some years to come.This work was supported in part by the National Aeronautics and Space Administration under contracts NASw-1284 and NASw-1535 and grant NSG-386 and in part by the United States Atomic Energy Commission under contract AT (30-1)2098. In addition, certain portions were carried out at California Institute of Technology under National Aeronautics and Space Administration grant NSG-426 and at the Institute of Space and Aeronautical Sciences, Tokyo.     

高分辨率有限差分—有限元混合方法及其在气动热计算中的应用

在文献［１］结合ＮＮＤ格式思想＾［２］提出的有限元格式基础上，给出一种有限差分－有限元混合方法。通过求解完全Ｎａｖｉｅｒ－Ｓｔｏｋｅｓ方程，得到了高超声速情况下钝头体轴对称绕流的较满意结果，同时讨论了网格Ｒｅ数对驻点热流的影响。     

Far ultraviolet imaging from the IMAGE spacecraft. 2. Wideband FUV imaging

The Far Ultraviolet Wideband Imaging Camera (WIC) complements the magnetospheric images taken by the IMAGE satellite instruments with simultaneous global maps of the terrestrial aurora. Thus, a primary requirement of WIC is to image the total intensity of the aurora in wavelength regions most representative of the auroral source and least contaminated by dayglow, have sufficient field of view to cover the entire polar region from spacecraft apogee and have resolution that is sufficient to resolve auroras on a scale of 1 to 2 latitude degrees. The instrument is sensitive in the spectral region from 140–190 nm. The WIC is mounted on the rotating IMAGE spacecraft viewing radially outward and has a field of view of 17° in the direction parallel to the spacecraft spin axis. Its field of view is 30° in the direction perpendicular to the spin axis, although only a 17°×17° image of the Earth is recorded. The optics was an all-reflective, inverted Cassegrain Burch camera using concentric optics with a small convex primary and a large concave secondary mirror. The mirrors were coated by a special multi-layer coating, which has low reflectivity in the visible and near UV region. The detector consists of a MCP-intensified CCD. The MCP is curved to accommodate the focal surface of the concentric optics. The phosphor of the image intensifier is deposited on a concave fiberoptic window, which is then coupled to the CCD with a fiberoptic taper. The camera head operates in a fast frame transfer mode with the CCD being read approximately 30 full frames (512×256 pixel) per second with an exposure time of 0.033 s. The image motion due to the satellite spin is minimal during such a short exposure. Each image is electronically distortion corrected using the look up table scheme. An offset is added to each memory address that is proportional to the image shift due to satellite rotation, and the charge signal is digitally summed in memory. On orbit, approximately 300 frames will be added to produce one WIC image in memory. The advantage of the electronic motion compensation and distortion correction is that it is extremely flexible, permitting several kinds of corrections including motions parallel and perpendicular to the predicted axis of rotation. The instrument was calibrated by applying ultraviolet light through a vacuum monochromator and measuring the absolute responsivity of the instrument. To obtain the data for the distortion look up table, the camera was turned through various angles and the input angles corresponding to a pixel matrix were recorded. It was found that the spectral response peaked at 150 nm and fell off in either direction. The equivalent aperture of the camera, including mirror reflectivities and effective photocathode quantum efficiency, is about 0.04 cm². Thus, a 100 Rayleigh aurora is expected to produce 23 equivalent counts per pixel per 10 s exposure at the peak of instrument response.