太阳模拟器光斑自动对焦系统设计

为提升多光源太阳模拟器复合光斑的对焦精度,以构建的多光源太阳模拟器为实验研究对象,采用机器视觉的方法提取聚焦光斑中心世界坐标,将太阳模拟器简化为关节机器人,利用D-H法得到灯单元反向运动学参数,进而完成光斑自动对焦系统设计,对光斑自动对焦系统进行了简单实验。结果表明:多光源太阳模拟器聚焦光斑中心对焦精度误差在1mm以内,可以满足预期的太阳模拟器实验需求。     

球面阵列LED太阳模拟器光学系统设计

针对氙灯太阳模拟器光电转换效率低、寿命短、辐照强度低,均匀性差等不足,基于LED太阳模拟器光学系统,提出了一种球面阵列LED太阳模拟器光学系统,包括准直光学系统、匀光系统以及光源系统的设计方法。利用同轴透射式光学系统技术设计了双分离结构的准直光学系统, 在分析比较常用匀光系统的性能与组成形式的基础上,阐述积分器与视场光阑的设计过程, 然后基于球面光源的设计思想完成光源系统的设计, 利用LightTools光学设计软件对LED太阳模拟器光学系统进行仿真分析与验证。实验结果表明:球面阵列LED太阳模拟器在工作距离100 mm,输出辐照面积为100 mm×100 mm范围内,其辐照强度大于1 100 W/m2,辐照不均匀度优于3.86%。     

座舱热载荷太阳辐射模拟器设计研究

针对特定机型座舱热载荷实验,提出太阳辐射模拟器光学系统的设计方法,并在此基础上研制出一套太阳辐射模拟器。设计了单只太阳辐射灯,完成了空间灯阵设计。采用提出的预调节方法,获得了合理的单灯安装位置。根据设计方案完成了光学系统的加工和安装,并对其开展了性能测试。结果表明:辐照度分布计算误差为12.0%,证明提出的预调节方法可行;根据预调节方法得到的座舱透明件表面热效应,与设计热效应偏差为-3.1%,说明达到了目标辐照环境;光学系统辐照不稳定度为±0.52%,具有较好的稳定性。研究结果对太阳辐射模拟器的设计具有参考价值。     

基于光斑调制的汇聚光源焦距测量系统

为实现对汇聚光源聚焦位置快速准确测量,搭建了基于光斑调制的汇聚光源焦距测量系统,通过精密调节待测光源在系统中前后位置,将一定距离处光屏上接收到的光斑调整到对照尺寸,读取位置数据,得到光源的系统测量数值.根据成像理论,推导出实验理论误差公式,依据系统初始参量,计算生成数据处理界面,将测量数值输入系统,直接输出焦距准确值.此系统可用于对LD光源是否合格进行快速筛选,及对微小差别光源焦距进行准确测量,焦距值精确到0.05mm.整个系统结构简单,仅需对光斑大小进行简单调整,专业技术要求低,测量数据误差小,成本低,能实现快速准确测量.     

运动式太阳模拟器LED阵列光源及其准直光学系统设计

运动式太阳模拟器是编码式太阳敏感器在装星阶段用于现场测试的一种重要设备,为敏感器测试提供模拟的太阳光信号和太阳光矢量信号。论述了运动式太阳模拟器的结构组成与工作原理,着重对其LED阵列光源和准直光学系统进行研究与设计。通过功率计算确定了LED数量,依据Sparrow判据分析了LED间距对辐照均匀性的影响,确定了阵列间距。基于边缘光线原理,建立了圆柱面镜的数学模型,设计了准直光学系统,借助LightTools软件进行仿真。实验结果表明:设计的运动式太阳模拟器在工作距离为50 mm处的辐照范围为10 mm×50 mm,最低辐照度为393 W·m~(-2),在-13°、0°、38°三种光线入射角下的辐照不均匀度均优于±7.3%,出射张角为0.78°,满足编码式太阳敏感器装星后现场测试的要求。     

太阳模拟器中椭球面聚光镜参数的确定

椭球面聚光镜是太阳模拟器设备的重要组成部分,其能量收集的效率决定着太阳模拟系统的能量传递效率,而太阳模拟器光学系统中的椭球面聚光镜参数一直没有理论上的设计依据,结合氙灯的发光特性并通过对MATLAB 中建立的椭球面聚光镜聚光过程数值分析模型给出了椭球面聚光镜包括第一焦距、最大成像放大倍率、包容角范围及前后开口直径的确定依据,并通过在Lighttools 中建立的4种仿真模型验证了理论分析的正确性。第一焦距由光源光中心高确定,最大成像放大倍率由光学积分器相对孔径及椭球镜包容角范围共同确定,椭球镜包容角范围不小于30°～120°,前开直径口由椭球镜的最大孔径角确定,后开口直径由最小孔径角和光源的径向调节量共同确定。该结论给椭球面聚光镜的设计提供了理论支撑,有利于设计完成高能量收集效率的椭球面聚光镜。     

太阳模拟器中椭球面聚光镜参数的确定

椭球面聚光镜是太阳模拟器设备的重要组成部分,其能量收集的效率决定着太阳模拟系统的能量传递效率,而太阳模拟器光学系统中的椭球面聚光镜参数一直没有理论上的设计依据,结合氙灯的发光特性并通过对MATLAB 中建立的椭球面聚光镜聚光过程数值分析模型给出了椭球面聚光镜包括第一焦距、最大成像放大倍率、包容角范围及前后开口直径的确定依据,并通过在Lighttools 中建立的4种仿真模型验证了理论分析的正确性。第一焦距由光源光中心高确定,最大成像放大倍率由光学积分器相对孔径及椭球镜包容角范围共同确定,椭球镜包容角范围不小于30～120,前开直径口由椭球镜的最大孔径角确定,后开口直径由最小孔径角和光源的径向调节量共同确定。该结论给椭球面聚光镜的设计提供了理论支撑,有利于设计完成高能量收集效率的椭球面聚光镜。     

新型LED太阳模拟器光学系统设计及仿真

针对现有LED太阳模拟器同时解决准直性、辐照度均匀性、光谱匹配性三大技术指标的难度较高的问题,基于光电一体化二次光学设计,提出一种简便、高效且可实现大功率的LED太阳模拟器光学系统设计方法。采用小角度准直透镜和抛物面镜来整合光源,通过混光棒和微结构进行匀光,最后利用抛物面镜实现光线的准直输出,基于同轴准直的设计思想完成LED太阳模拟器的设计。利用光学软件LightTools对LED太阳模拟器光学系统进行模拟仿真与分析优化,实验结果表明:在直径为260 mm的有效辐照面上辐照不均匀度为2.5%、准直角为1.5°。     

新型LED太阳模拟器光学系统设计及仿真

针对现有LED太阳模拟器同时解决准直性、辐照度均匀性、光谱匹配性三大技术指标的难度较高的问题，基于光电一体化二次光学设计，提出一种简便、高效且可实现大功率的LED太阳模拟器光学系统设计方法。采用小角度准直透镜和抛物面镜来整合光源，通过混光棒和微结构进行匀光，最后利用抛物面镜实现光线的准直输出，基于同轴准直的设计思想完成LED太阳模拟器的设计。利用光学软件LightTools对LED太阳模拟器光学系统进行模拟仿真与分析优化，实验结果表明:在直径为260 mm的有效辐照面上辐照不均匀度为2.5%、准直角为1.5°。     

一种高性能太阳敏感器复合光学系统设计

以夫朗禾费衍射理论为基础,结合微透镜,设计了一种高性能的数字式太阳敏感器复合光学系统。分析了光学系统的组成,建立了光学系统的数学模型,设计了光学系统的焦距、孔径和微透镜参量,并进行了成像的数值仿真。仿真结果表明,与基于掩模的光学系统相比,这种新型的复合光学系统成像光斑能量分布集中,保证计算光斑中心位置的高精度,使敏感器具有大视场和高精度的特点。     

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 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.     

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.     

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...