多光谱遥感相机光学系统设计

设计了谱段位于450~900nm,焦距f=6 000mm,F数为10的大F数、矩形视场、长焦距的折轴三反光学系统.光学系统视场角为1.6°,光学系统的畸变优于0.5%,中心面遮拦为6%时,Nyquist频率(25lp/mm)处各谱段调制传递函数优于0.65,整个光学系统成像质量达到衍射极限.同时根据所采用的多光谱时间延迟积分CCD分析了相机各谱段的静态调制传递函数,可以满足多光谱遥感相机的设计使用要求.     

基于滤光片阵列分光的无人机载多光谱相机研制

介绍一款适用于轻小型无人机的多光谱相机。将多个独立的滤光片依次拼接成滤光片阵列在成像探测器前放置由多个滤光片依次排列而成的滤光片阵列,一次曝光得到地物目标分条带区域的分波段图像,通过飞行平台的前向运动获得每个条带区域的多光谱图像。利用平台的前向运动代替了旋转、扫描等机械运动,减轻了相机重量和体积,适用于轻小型无人机平台,由于采用较大的探测器件,能够获得更多的旁向像素数(约4300)和更宽的旁向幅宽。利用研制的多光谱相机,在中国科学院怀来遥感站进行了无人机飞行试验,获取了站区周边的6波段多光谱图像。数据处理结果表明该相机的数据质量能够满足植被指数计算等相关要求。     

基于非共轴阵列照明的小型化眼底相机光学系统设计

建立了非共轴阵列照明下的眼底成像数学模型,采用照明光路与成像光路独立设计方法,提出了一种微小型眼底相机光学系统,以避免传统眼底相机中人眼角膜与网膜物镜反射杂光对视网膜图像的干扰.设计了6阵列环形光源照明光路系统,长度仅17.9 mm,实现眼底视网膜有效照明线视场不小于12 mm;成像光路系统采用二次成像设计,光学调制传递函数优于0.2@91 lp/mm,畸变小于5%,长度仅为75 mm.仿真与设计结果表明,该眼底相机光学系统有效抑制了光路中的杂散光,有利于获得高对比度视网膜图像.研究结果可为高像质、小型化以及低杂光眼底相机发展提供设计参考.     

新型三反射光学系统设计

随着空间光学技术的发展,对于空间相机地元分辨率的要求越来越高,而且必须具有多光谱成像能力,因此空间相机光学系统的设计要满足视场大和畸变小的要求.本文以共轴三反射光学系统为基础,研究了一种新型的三反射光学系统.该系统不仅中心遮拦小、光学畸变低,而且实现了全色和多光谱CCD的合理排布.设计结果表明:当光学系统的焦距为f=12 000 mm、F数为12、成像谱段位于450~900 nm时,视场角可以达到1.6°,光学系统的线中心遮拦比低于1/3,光学畸变量小于0.5%,在50 lp/mm处调制传递函数优于0.47,成像质量达到衍射极限,可以满足多光谱高分辨率空间相机对地遥感的使用需求.     

磁镜阵列像增强器的调制传递函数研究

基于三代近贴式像增强器,设计了磁镜阵列装置的结构,从理论上计算了该装置的调制传递函数以及将其引入像增强器后整体的调制传递函数,以此来分析对成像质量的影响.通过对实际参量绘制的调制传递函数曲线分析,得出磁镜阵列装置在X、Y方向的极限分辨率分别为117 lp/mm、121 lp/mm,奈奎斯特频率处的调制传递函数值分别为0.55、0.59,同时磁镜阵列像增强器的极限分辨率也分别达到了87 lp/mm、89 lp/mm,相应的奈奎斯特频率处的调制传递函数值为0.49和0.52.结果表明X和Y方向的调制传递函数曲线之间差异较之磁镜阵列装置变小,这对保证成像质量起到了积极的作用.文章为进一步深入研究磁镜阵列像增强器提供了重要的理论依据.     

磁镜阵列像增强器的调制传递函数研究

基于三代近贴式像增强器,设计了磁镜阵列装置的结构,从理论上计算了该装置的调制传递函数以及将其引入像增强器后整体的调制传递函数,以此来分析对成像质量的影响.通过对实际参量绘制的调制传递函数曲线分析,得出磁镜阵列装置在X、Y方向的极限分辨率分别为117lp/mm、121lp/mm,奈奎斯特频率处的调制传递函数值分别为0.55、0.59,同时磁镜阵列像增强器的极限分辨率也分别达到了87lp/mm、89lp/mm,相应的奈奎斯特频率处的调制传递函数值为0.49和0.52.结果表明X和Y方向的调制传递函数曲线之间差异较之磁镜阵列装置变小,这对保证成像质量起到了积极的作用.文章为进一步深入研究磁镜阵列像增强器提供了重要的理论依据.     

一种空间相机热控调焦机构的设计与分析

为满足空间相机成像质量的要求,设计了一种热控调焦机构来修正离焦量.首先,根据光学系统确定调焦方式,并通过驱动次镜沿光轴方向移动的方式设计了调焦机构,该结构占用空间小且质量较轻.然后,根据调焦需求,选取热膨胀系数较高的铝作为主要材料,采用在镜座背面贴加热片等措施保证次镜在恒温下工作,并通过有限元方法对调焦机构性能进行了建模分析.最后,对调焦机构工作状态进行分析验证,利用Zernike多项式对其工作时所产生温度变化引起的镜面变形进行拟合,把变形后的面形输入到Zemax软件中,以调制传递函数作为光学系统成像质量评价指标,分析了调焦机构在正常工作时次镜面形变化对相机成像质量的影响.结果表明,调焦机构符合设计指标,且工作时次镜面形的变化对光学系统成像质量的影响可以忽略,与传统调焦机构相比,具有质量轻、结构简单等优点.     

消畸变、长焦距相机光学系统设计

随着空间光学技术的不断发展,时间延时积分电荷耦合器件(TDI-CCD)相机得到了广泛的应用,TDI-CCD图像传感器的应用不仅提高了相机系统的信噪比而且使相机的光机结构更加紧凑,但光学系统的畸变在推扫过程中会造成像移,并最终导致图像模糊,因此对光学系统的设计提出了新的要求。分析了光学系统畸变对TDI-CCD推扫成像时的影响,研究了空间相机光学系统设计中消除畸变的方法,并进行了光学系统设计。设计了谱段位于450～900nm,焦距f=6000mm,F数为10的三反射消畸变光学系统。设计结果表明,当光学系统视场角为1.6°时,光学系统的畸变量小于0.01%,当面中心遮拦为0.06时,Nyquist频率(50lp/mm)处调制传递函数优于0.50,成像质量达到衍射极限,可以满足高分辨率TDI-CCD空间相机的使用要求。该光学系也适用于多光谱、立体成像和立体测绘等对光学系统畸变有严格要求的相机系统。     

基于LCTF的新型多光谱成像光学系统设计

设计了一种基于液晶可调谐滤光片（Liquid Crystal Tunable Filter,LCTF）的新型多光谱成像光学系统。该光学系统工作谱段为400~720nm,光谱分辨率为10nm,可对216mm×216mm幅面大小的物面成像清晰。根据多光谱成像系统的总体方案,对光学系统分析,确定各光学参数,设计结果表明,成像系统在空间频率91lp/mm处,各个波段处的轴上和轴外调制传递函数均大于0.3,全视场畸变低于0.1%,成像质量良好,可以满足多光谱成像的总体要求。     

宽覆盖高分辨率机载相机光学系统设计

针对机载相机广域高效航拍作业需求,采用新型级联光学成像结构,设计了一种宽覆盖高分辨率机载相机光学系统。该系统由对称前置同心物镜和中继转像透镜阵列组成,对称前置同心物镜获取剩余像差均匀的宽视场曲面像,中继转像透镜阵列对该曲面像进行视场细分、剩余像差校正及中继成像。所设计的机载相机光学系统焦距为60 mm、F数为3.4、视场角可达132°。基于一阶理论和像差特性,在不同飞行高度对地观测时,研究了机载相机光学系统的成像质量与宽视场曲面像的关系,获得系统在不同飞行高度实现清晰成像的方法。通过像质评价,结果表明,优化设计的系统在低空、中空及高空进行对地观测时,像面光线追迹点列图方均根半径均优于1.6μm,在奈奎斯特频率为230 lp/mm处,调制传递函数均达0.4,系统成像性能优异且像质均匀。新型级联光学成像系统适用于不同飞行高度的机载相机。     

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...