近红外白天恒星探测对比度分析

红外波段可以探测到足够多的星体用以导航。恒星-背景对比度是白天恒星探测时的一个重要指标,分析近红外波段,6星等恒星对比度随太阳天顶角、探测器高度和探测方位角的变化情况。结果显示,恒星-背景对比度随太阳天顶角近似于指数增长,40太阳天顶角时对比度是20时的2.69倍左右;一定高度时,对比度随探测器高度的增加近似指数增加,低于15 km时对比度仍小于3, 80 km时对比度达到60左右;随着探测方位角的增大,恒星-背景对比度基本上线性增大,30探测方位角时的对比度是0探测方位角时对比度的2.38倍。     

水-气界面参数和二向性影响因素交互作用研究

基于光学辐射传输软件HYDROLIGHT,模拟不同外界和水质条件下水气界面透射率T,Gordon模型参数f和二向性因子Q,研究风速、太阳天顶角、单次反照率和拉曼散射对T、f和Q及其组合f/Q的影响和交互作用,确定T、f、Q和f/Q的主导影响因子,以期为确定水色反演算法误差来源以及减小反演误差提供定量的依据。研究结果表明,T、f和Q的主导影响因素为太阳天顶角,单次反照率和风速对T、f和Q的影响相对较小,而对f/Q影响最大是单次反照率,其次是太阳天顶角,风速最小,且各影响因素之间具有较强的交互作用。高散射特性水体中,拉曼散射对f、f/Q和T的影响可忽略不计;黄质(CDOM)和叶绿素的荧光特性对f和f/Q的影响随着叶绿素和CDOM浓度的增加不断减小,但在高CDOM和叶绿素浓度的富营养化水体中该影响仍难以忽略。     

沙尘气溶胶粒子群的散射和偏振特性

根据Mie散射理论,以对数正态分布函数描述沙尘气溶胶粒子群的粒径尺度分布,计算了沙尘气溶胶粒子群在0.2～40μm波段间对太阳短波辐射和地球大气长波辐射的单次散射反照率、散射相矩阵函数,揭示了不同相对湿度时,沙尘粒子群对入射辐射的散射和偏振的特征。结果表明,沙尘粒子群的单次散射反照率随着入射波长的增加有较大起伏,不同相对湿度条件下,变化趋势基本一致;在可见光、近红外波段单次散射反照率随湿度增加而变大,湿度95%时非常接近于1;大于10μm的热红外波段单次散射反照率随相对湿度增加而减小,具有较强的吸收辐射能力。散射辐射强度受湿度影响较小,随散射角的增加呈现先减小后增大的趋势,且增大的趋势随着波长的增加而减弱;不同波段上,线偏振和圆偏振随散射角和相对湿度变化存在差异;在前向和后向仅对入射辐射为圆偏振辐射产生圆偏振散射;散射光的偏振特性及其湿度差异主要表现在后向散射区,多以拱形形式体现。拱顶峰值散射角位置存在差异,且峰值散射角随相对湿度的降低向后向漂移。     

Q值的影响因素分析及其参数化

针对高散射特性的二类水体中难以测量的双向性函数Q,利用HYDROLIGHT模拟观测角为太阳天底角下440 nm处的Q值,并分析环境及水体光学特性对Q值的影响.结果表明,在高散射特性的近岸水体或内陆湖泊水体中,由于散射次数的增加,使得风速、散射相函数等影响因素对Q值影响相对减小,单次散射反照率W.和太阳天顶角θ成为Q值的主要影响因素;随着深度的增加,双向性函数Q受边界条件和光线入射状况影响的程度逐渐减少,直至不受其影响,而成为只与固有光学量相关的内秉光学量;利用Q值的主要影响因素W<,0>、θ和上行辐亮度的漫衰减系数K<,L<,u>>分别对Q值进行参数化,得到Q值的2种参数表达式.     

沙尘天气下大气能见度对激光光强的影响

基于米氏理论,分别研究了不同波长的激光信号在沙尘天气中发生单次散射和多次散射时光强与能见度间的变化关系.推导出发生单次散射时光强与能见度间的解析表达式,同时采用蒙特卡洛方法分析了发生多次散射时光强与能见度间的关系,并与单次散射时的结果进行对比.结果表明:在激光信号波长固定时,接收光强会随着沙尘能见度的增大而增加,并趋于稳定值;在能见度固定时,接收光强会随着激光信号波长的增大而减小;随着传输距离的增加,多次散射的影响会越来越明显.     

水下航行器热尾流目标海平面探测红外成像仿真

红外成像是探测水下航行器海平面热尾流目标的重要方法。采用建模仿真的方法，基于尾流区海平面温度分布特征，结合三维坐标变换和投影映射方法实现热尾流目标的红外成像仿真过程，得到在相同探测条件下热尾流的辐射能量随波段的分布，以及不同探测方位角与高度下热尾流在像平面内的形态及红外辐射亮度的变化规律。论证了噪声对典型工况条件的热尾流与背景海面的对比度和清晰度，以及热尾流目标的探测和识别难度的影响。仿真结果表明:相同探测条件下，热尾流在8 μm~12 μm波段的辐射能量远远大于3 μm~5 μm波段；随着探测高度的增加，热尾流区域的红外辐射观测亮度逐渐减小；探测路径长度一定时，探测天顶角增大，热尾流红外辐射观测亮度减小，并且热尾流在像平面内所占区域逐渐减小。     

基于组合拟合法的冰晶粒子的光散射计算

利用组合拟合法计算了冰晶粒子的单次散射特性。给出了消光效率因子、单次散射反照度及非对称因子的拟合公式,利用拟合公式对有效粒子尺度为20μm和120μm的六种冰晶粒子的消光效率因子、单次散射反照度及非对称因子进行了计算。结果表明,粒子的消光效率因子、单次散射反照率和非对称因子随着入射波长的增加有着较大的起伏,后两者随着波长的增加而变化趋势基本一致;对于单次散射反照率来说,在可见光波段,反照率非常接近于1;在短波段,粒子的非对称因子变化较小,并且随着波长的增加,非对称因子会逐渐增大。     

基于微扰近似的圆锥表面光散射*

由Hueygen原理出发,介绍了粗糙表面的光散射特性.基于微扰近似,在不考虑遮蔽效应和圆锥顶点的散射情况下,分析了圆锥物体的光散射特性,推导了圆锥物体对平面光的散射场解析表达式.计算了圆锥表面在高度起伏均方根不同情况下对1.06μm光波的散射,并且得到了入射角一定的情况下,不同观察方向的散射光强分布曲线.结果表明,在观察方位角不变时,圆锥的散射光强随观察角顶角的增加先增大后减小|在观测方位角一定时,散射光强随高度起伏均方根的增加而减小,且随观察方位角呈对称分布.     

基于微扰近似的圆锥表面光散射

由Hueygen原理出发,介绍了粗糙表面的光散射特性.基于微扰近似,在不考虑遮蔽效应和圆锥顶点的散射情况下,分析了圆锥物体的光散射特性,推导了圆锥物体对平面光的散射场解析表达式.计算了圆锥表面在高度起伏均方根不同情况下对1.06μm光波的散射,并且得到了入射角一定的情况下,不同观察方向的散射光强分布曲线.结果表明,在观察方位角不变时,圆锥的散射光强随观察角顶角的增加先增大后减小;在观测方位角一定时,散射光强随高度起伏均方根的增加而减小,且随观察方位角呈对称分布.     

空间斜程能见度的影响因素分析

 空间斜程能见度是空间目标识别的重要参量。水平能见度与大气消光参数有明确的关系，而斜程能见度与大气消光参数、观测方向、太阳天顶角等多种因素有关，目前尚未有明确的结果。从辐射传输理论出发，通过δ-Eddington近似求解辐射传输方程，尝试推导了空间斜程能见度的表达式，探讨了斜程能见度与观察者视角、太阳高度角以及大气光学特性之间的关系。     

Interior radiances in optically deep absorbing media—III. Scattering from haze L

The interior radiances are calculated within an optically deep absorbing medium scattering according to the Haze L phase function. The dependence on the solar zenith angle, the single scattering albedo, and the optical depth within the medium is calculated by the matrix operator method. The development of the asymptotic angular distribution of the radiance in the diffusion region is illustrated through a number of examples; it depends only on the single scattering albedo and on the phase function for single scattering. The exact values of the radiance in the diffusion region are compared with values calculated from the approximate equations proposed by Van de Hulst. The variation of the radiance near the lower boundary of an optically thick medium is illustrated with examples. The attenuation length is calculated for various single scattering albedos and compared with the corresponding values for Rayleigh scattering. The ratio of the upward to the downward flux is found to be remarkably constant within the medium. The heating rate is calculated and found to have a maximum value at an optical depth of two within a Haze L layer when the sun is at the zenith. The location of this maximum moves toward the top of the haze layer as the solar zenith angle increases and also as the single scattering albedo decreases. When the single scattering albedo is less than 0·8, the downward flux is so small within the diffusion region that experimental measurements are probably not possible.     

Influence of the vertical profile of Saharan dust on the visible direct radiative forcing

The vertical profile of Saharan dust in the atmosphere is generally characterized by a large aerosol concentration in the mid troposphere, differently from the climatological distribution of other types of particles, that show a peak at the surface and a rapid decrease with height. Saharan dust is also characterized by particles of relatively large size of irregular shape, and variable values of the single scattering albedo (the ratio between radiation scattering and extinction). The dust's peculiar vertical distribution is expected to produce an effect on the calculation of the direct aerosol radiative forcing at the surface and at the top of the atmosphere. This effect is investigated by comparing estimates of aerosol direct visible radiative forcing at the surface and at the top of the atmosphere for dust vertical profiles measured in the Mediterranean, and for the climatological profile. The radiative forcing is estimated by means of an accurate radiative transfer model, and for the ocean surface. The sensitivity of the results on the solar zenith angle, aerosol optical depth, and aerosol absorption is also investigated. The aerosol radiative forcing at the surface shows a very small dependency on the aerosol vertical profile. At the top of the atmosphere, the radiative forcing is weakly dependent on the vertical profile (up to 10% variation on the daily average forcing) for low absorbing particles; conversely, it shows a strong dependency (the daily radiative forcing may vary up to 100%) for absorbing particles. The top of the atmosphere visible radiative forcing efficiency produced by dust having single scattering albedo <0.7 is higher by 4 W m⁻² when the observed vertical profile instead of the standard profile is used in the calculations (i.e. it produces a lower cooling). For values of the single scattering albedo around 0.67, the sign of the forcing depends on the vertical profile. The influence of the vertical distribution on the radiative forcing is largest at small values of the solar zenith angle, and at short wavelengths.     

激光在准球形边界卷云中传输的衰减和透过特性

高空卷云主要由各种不同形状的冰晶粒子组成,是地空链路上激光信号传输的重要影响因素。依据高空卷云中冰晶粒子的分布特征和散射特性,采用C版本的离散纵标法（CDISORT）,充分考虑地球球形曲率及云层冰晶粒子多次散射影响因素,研究准球形边界云层的激光透过率和衰减特性,并比较了太阳天顶角不同时平面平行模式和准球面模式下卷云大气激光透过率的差异,数值计算了三种激光波长（0.65,1.06和3.8 μm）在卷云中传输时的衰减和透过特性。计算结果表明：较小太阳天顶角（小于80°）入射时,两种模式下卷云大气激光透过率相对误差很小,其中0.65 μm激光波长入射时两种模式下的相对误差仅为1.72%,较大太阳天顶角（大于80°）入射时,两种模式下卷云大气激光透过率相对误差明显增大,0.65 μm激光波长入射时两种模式下的相对误差最大达到69%;卷云粒子单次散射时,激光在云层的衰减与卷云粒子有效半径、传输距离、光学厚度及激光波长等因素有关,随光学厚度的增加,云层的激光透过率减少,1.06 μm激光波长入射时透过率最大,3.8 μm激光波长入射时透过率最小;0.65和1.06 μm激光波长入射时,随云层粒子有效半径的增加激光透过率逐渐增加,而3.8 μm波长激光,随云层粒子有效半径的增加激光透过率逐渐减少,随相对方位角的增加,云层的激光透过率减少,且不同卷云传输模型对激光透过率也存在不同的影响。该研究工作将为开展地空链路星载、机载激光通信、激光雷达探测等工程系统中的激光信号云层传输特性的应用提供理论支持,同时也可进一步拓展为地空链路激光遥感、制导和预警等应用提供预先理论研究基础。     

Interior radiances in optically deep absorbing media—II Rayleigh scattering

The interior radiances are calculated within an optically deep absorbing medium scattering according to the Rayleigh phase function. The accuracy of the matrix operator method is improved by many orders of magnitude through the use of accurate starting values obtained by the Runge-Kutta method rather than from the single scattering approximation. The radiance and flux are given for a range of solar zenith angles and for single scattering albedos of 1, 0.99, 0.9, 0.5 and 0.1. The development of the asymptotic angular distribution of the radiance is illustrated. It is shown that this asymptotic distribution is probably physically unobservable when ω₀ < 0.8, since the flux is less than 10^-8 of its original value at the beginning of the asymptotic region. The ratio of the upward to downward flux is calculated and is shown to be remarkably constant within the medium except very close to the boundaries. The heating rate within the medium is found to be very nearly proportional to the downward flux, except near the boundaries. When the single scattering albedo is small, a number of examples illustrate the significant contribution of the direct solar flux to the total flux even at great optical depths within the medium. The total downward flux decreases exponentially with optical depth away from boundaries when the single scattering albedo is greater than or equal to 0.9; when it is less than or equal to 0.5 only an approximate exponential fit can be obtained within the region accessible to experimental observation.     

我国北方不同类型下垫面地表反照率特征

地表反照率反映了地面对太阳辐射的反射能力,在地表能量平衡中起着非常重要的作用,本文利用"中国北方协同观测"的资料,分析了不同下垫面10个站点7-9月的反照率变化特征和对降水的响应,并讨论了榆中、通榆草地、通榆农田、密云、玛曲和锦州站地表反照率与太阳高度角和土壤湿度的关系,结果表明:反照率的相对关系是东北干旱草甸西北高寒草甸西北绿洲农田黄土高原自然植被东北半干旱草甸东北农田东北果林,并且反照率基本上和降水对应,降水量大的站点反照率小,降水量小的站点反照率大,反照率的日变化曲线分为早晚对称型,早上比较大、中午下午比较小和晚上最大、早上最小的不对称型三种,选取的6个观测站反照率的谷值一般出现在降水日,峰值一般出现在没有降水、太阳辐射比较强的日子,地表反照率随着太阳高度角的增大而减小,当太阳高度角大于40°时,地表反照率基本不变,榆中和通榆农田地表反照率随着土壤湿度增大减小较明显,其次是通榆草地,玛曲、密云和锦州地表反照率随着土壤湿度变化不明显。     

冬小麦冠层光谱的方向性特征分析

二向性反射因入射和观测的角度变化而变化,合理选择遥感观测角度、太阳天顶角等为提高遥感应用精度提供可能。通过采用各向异性因子和各向异性指数定量分析了冬小麦冠层窄波段二向性反射率及NDVI的方向性特征。分析结果表明：主平面内二向性反射率的各向异性最强,垂直主平面最弱,其他平面介于前两者之间;可见光波段反射率随观测天顶角的敏感性大于近红外波段;反射率对太阳天顶角的敏感性随着观测天顶角的增大而增大。前向NDVI整体上大于后向,且NDVI随着太阳天顶角的增大呈增大趋势。为了减少观测方式所带来的不确定性,应尽量选择近红外波段和小太阳天顶角,估算结构参数时应尽量选择主平面进行遥感观测,在利用NDVI估算生物物理参数时尽量远离“热点”区域。     

羊八井ARGO实验触发效率的地磁场效应

广延大气簇射(EAS)中次级带电粒子在地磁场中偏转,影响次级粒子的横向分布.本文简要分析了羊八井宇宙线观测站不同天顶角的地磁场因子随方位角的变化,表明地磁场对从北方来的宇宙线次级粒子横向分布的影响比对南方来的大.利用蒙特卡罗方法模拟了有无地磁场情况下两个大容量的EAS样本,采用ARGOG探测器模拟程序模拟羊八井ARGO阵列的触发效率.模拟结果表明在忽略地磁场影响时阵列的触发效率确是各向同性的,有地磁场时触发效率南高于北,且原初粒子的天顶角越大,这种南北不对称性越明显.     

Experimental observation of the effect of the Earth’s magnetic field on the EAS muon component

The dependence of the intensity of muon bundles recorded using the DECOR coordinate track detector on the angle between the directions of bundle arrival and the Earth’s magnetic field has been analyzed for several ranges of zenith angles. It is found that the intensity of muon bundles decreases with an increase in the transverse magnetic field component, in contrast to the results of the calculation performed on the assumption of flux azimuthal symmetry. The effect of coplanarity of particle tracks in the plane formed by the core of an extensive air shower and the Lorentz force vector is also observed.