直线阵光学综合孔径成像中的子孔径尺寸效应

光学综合孔径阵列中的子孔径的位置和直径的大小对成像质量有着重要的影响。详细分析了几种不同优化排列的光学综合孔径直线阵列的无像差点扩展函数、光学传递函数和衍射成像特性．结果表明,子孔径的位置不同．光学传递函数的空间频率覆盖有很大的差异。增大子孔径的直径可以增大空间频率覆盖程度．但子孔径直径过大时义会产生空间频率冗余度和增加制造成本。直线阵光学综合孔径的衍射成像是多重像,子孔径直径的增大还可以减小重影的程度,提高成像质量。结果说明,在进行光学综合孔径阵列优化排列时必须考虑子孔径的直径大小这个重耍的因素。     

光学综合孔径望远镜成像分析及计算机仿真

阐述了光学综合孔径(OSA)望远镜成像原理以及综合孔径望远镜的几种实现形式；采用快速傅里叶变换(FFT)算法得到了任意子孔径综合模式下的点扩展函数(PSF)和光学传递函数(OTF)分布；从子孔径结构排列、共相位、图像恢复几个方面论述了光学综合孔径的成像特征。初步分析了稀疏率、填充因子、“实际截止频率”等因素对光学综合孔径望远镜成像的影响。分析和仿真结果表明：光学综合孔径通过相干成像不但可以突破传统单孔径系统的口径局限获得极高的成像分辨率，而且对于实现空间光学遥感系统轻量化和模块化都具有重要意义。     

光学综合孔径望远镜阵的光束组合器

光束组合器是光学综合孔径望远镜阵重要技术组成部分之一。从光束组合器所产生的光干涉条纹中提取中央条纹（主峰）相位和可见度信息，实现对望远镜状态、延迟线光程补偿与条纹跟踪，光束平行性伺服等进行精细馈控，从而高灵敏度、高效率地得到图像重构的闭合相位等数扭，最后获取高分辨率的目标图像。给出了一个用于光学综合孔径望远镜阵像面光束组合器方案的初步研究结果。     

二维圆周光综合孔径阵的优化排列及其成像特性研究

光综合孔径成像的原理是应用干涉原理在空间频率域中进行采样,并通过傅里叶反变换或其他数值变换方法得到空间分辨力远高于单个孔径成像系统的目标图像。由若干个相同的小孔径在二维圆周上优化排列组成的综合孔径成像系统可以在二维空间频率域中实现较为均匀分布的、具有无冗余度的采样点覆盖,为高质量实时成像提供了一个有效的途径。运用模拟退火算法对由7～16个子孔径组成的二维圆周综合孔径阵列进行优化排列。并依据光学衍射成像原理,从空域和频域两个方面详细分析了二维圆周上优化排列与均匀排列光综合孔径阵的成像特性。对7～16个子孔径组成的光综合孔径的仿真结果表明：无论是在空域还是频域上,子孔径直径增大、孔径数目增多以及综合孔径阵的优化排列都是有利于提高成像质量的。但综合后的子孔径的直径的增大,虽然能获得极高的角分辨力,却并不利于成像质量的提高。     

光学综合孔径望远镜中子望远镜平行性和光程差调整的研究

光干涉技术与天文望远镜技术的结合是提高天文观测分辨率的一种有效方法.采用望远镜阵代替单个大口径望远镜来集光观测,利用最大基线的概念来等效传统光学望远镜的最大口径,很大程度上解决了单个望远镜集光能力不足、角分辨率不高的问题.然而对于光干涉来说,在应用中,只有满足:两束光的相位差δ必须相对稳定、存在相互平行的振动分量、频率相同、两光波在相遇点所产生振动的振幅相差不悬殊和两光波在相遇点的光程差(OPD)应在相干长度之内等这些条件时才能部分相干.光学综合孔径(OAS)望远镜产生干涉条纹的前提条件是子望远镜之间必须两两相干.推导了双光束光干涉的要求,并从双光束干涉的平行性和光程差的要求出发,研究并得出光学综合孔径望远镜子望远镜的平行性和光程差的要求.结合双光束干涉的恒星光干涉仪的光束平行性和光程差的调整方案,研究并得到了光学综合孔径望远镜子望远镜的平行性和光程差调整的光学方案,并讨论了该系统的改进措施.     

基于遗传算法的光综合孔径圆周阵优化

从光综合孔径圆周阵列成像的基本原理出发,建立了圆周阵列的优化模型;采用改进的实数编码方法对子孔径阵列位置进行编码,运用遗传算法进行子孔径阵列的优化;以阵列的u-v覆盖点间距最大化及最小冗余度来设计目标函数,实现了8~16个子孔径二维圆周阵的优化排列;分析了二维圆周光综合孔径阵列成像系统的点扩展函数、光学传递函数和衍射成像的基本原理;对优化结果与模拟退火算法的结果进行对比,使用仿真成像程序分析其点扩展函数,并与均匀排布的圆周阵列进行对比。结果表明,采用改进的实数编码的遗传算法可以很好地解决综合孔径阵列优化的问题,相对于模拟退火算法,该方法的计算时间更短,结果更优。     

基于混合算法的光学合成孔径成像系统孔径优化

结合模拟退火算法和遗传算法的优点,在遗传算法中加入模拟退火算子,运用这种混合算法对子孔径结构进行了优化。以阵列的子调制传递函数覆盖点间距最大化及最小冗余度来设计目标函数,实现了单圆周孔径阵列和双圆周孔径阵列的优化排列。使用仿真程序对优化阵列的光学传递函数进行了分析,将优化结果与相同子孔径数目的单圆周结构进行仿真实验和比较。结果表明,采用这种混合算法是可以很好的解决光学合成孔径结构的优化问题,优化结果接近全局最优解,优化后的双圆周阵列接近Golay阵列,具有更大的实际空间截止频率。     

光学综合孔径空间探索波前干涉理论研究

由光学综合孔径干涉模型深入研究了光学综合孔径空间探索波前干涉理论.在观测目标相当遥远及准单色观测条件下,根据光学综合孔径光学传递函数以及傅里叶变换性质建立了一个简化的像面干涉光强分布数学模型,此数学模型的物理含义符合光学综合孔径成像观测的实际情况；根据光学综合孔径瞳面干涉条件,在光学综合孔径像面干涉数学模型的基础上得到瞳面干涉的数学模型.最后根据光学综合孔径数学模型分别对像面干涉模型和瞳面干涉模型进行了计算机仿真.     

光学稀疏孔径系统的成像及其图像复原

由多个小口径成像系统通过特殊排列综合而成的光学稀疏孔径系统是实现高分辨率天文目标成像观测的一种新方法.建立了光学稀疏孔径系统的衍射受限非相干成像模型,并针对某一具体的光学稀疏孔径系统,运用图像复原维纳滤波器完成了系统成像和图像恢复处理的计算机仿真实验.结果表明,光学稀疏孔径系统可以等效实现单个大口径成像系统的成像观测效果.     

子孔径拼接干涉检测离轴非球面研究

将子孔径拼接技术与干涉技术相结合提出了一种新的检测离轴非球面的方法,该方法无需其他辅助光学元件就可以实现对大口径、离轴非球面的测量.对其基本原理进行了分析和研究;并基于齐次坐标变换、最小二乘拟合建立了综合优化和误差均化的拼接数学模型;开发了子孔径拼接检测非球面的算法软件,并设计和搭建了子孔径拼接干涉检测装置;利用综合优...     

关于"太阳在银河系中所受引力与到银心距离r的关系"的讨论

讨论了银道面内的引力场强分布和太阳在银河系中所受引力与到银心距离r的关系，指出引力场强g并不是与r的平方成反比，这是由于银河系的大小和形状不能忽略造成的．强调了万有引力定律的适用条件．     

On the predictability of the positions of the convergence zones in the ocean

The disagreement between the experimental and calculated positions of the first convergence zone are known from many publications. The most probable cause for such a disagreement, namely, the incorrect specification of the input data for the calculations, is considered. The lack of simultaneity between the hydrological surveys of the region and the acoustic experiments is emphasized. The experimental data obtained by the author in five ocean regions are presented. These data characterize the diurnal variability of the distance from the source to the nearest boundary of the convergence zone. The relations proposed by different researchers for calculating the sound speed from the temperature, salinity, and hydrostatic pressure are analyzed. It is shown that these relations lead to a substantial difference in the estimated depth dependence of the hydrostatic gradient of the sound speed. The position of the first convergence zone is calculated for the propagation conditions determined by vertical temperature and salinity profiles with the subsequent recalculation of these profiles into sound speed profiles by using eight different formulas known from the literature. It is shown that different formulas lead to different values of the distance to the first zone; this difference is substantially greater than that between the calculations and experiment. The necessity of improving the recalculation relations in view of the experimental data on sound propagation in natural oceanic waveguides, including the data on the actual positions of the convergence zones, is emphasized.     

On the calculation of the bremsstrahlung in the region of the plasma frequency

On the basis of the classical theory of radiation produced in incomplete Coulomb interaction, a formula is derived for the coefficient of the bremsstrahlung of fully ionized plasma. In the region of rectilinear approximation a comparison is made with the results of the quantum formula derived from the Born approximation. Furthermore, the influence of dispersion upon the emission coefficient is taken into account; some relations for the region of dispersion are given.     

Dependence of the Intensity of the Spectral Lines and the Composition of the Sample and the Plasma Parameters of the Unipolar Arc

The investigation was made of the dependence of the intensity of Tl, Ga, Mo, Mg, Mn, Sn, Bi, Ni, Zn, Pt and Au spectral lines and the plasma parameters (temperature T, electron concentration n_e, degree of 6 ionnization α) from concentration of lithium additive.     

Extracting the wavefunction of the LSP at the LHC

We consider associated production of squarks and gluinos with the lightest supersymmetric particle (LSP), or states nearly degenerate in mass with it. Though sub-dominant to pair production of color SU(3)-charged superpartners, these processes are directly sensitive to the wavefunction composition of the lightest neutralinos. Exploiting event-shape variables - including some introduced here for the first time - we are able to identify the composition of the LSP by selecting events involving a single high-pT jet recoiling against missing transverse energy. We illustrate the proposed technique on a set of benchmark cases and propose methods for applying these results in more realistic experimental environments.     

Set the controls for the heart of the Sun

In this paper we describe experiments conducted with high-power lasers that are attempting to replicate, for a very short time and in miniature, conditions found in the Sun. Experiments to date have reached conditions in the outer part of the Sun. To reach the Sun's centre requires compression of material to very much greater than solid density and heating to over ten million degrees. To achieve this, a new class of experiments and a new generation of high-power lasers are required.     

On the Question of the Source of the Apokamp

Technical Physics - The object of this work is the apokamp—a new type of plasma jet, which is formed from a bright offshoot emerging at the bending point of a channel of a high-voltage...