光吸收对冰晶粒子散射相函数的影响

本文利用射线跟踪法对冰晶粒子散射、吸收进行了研究。从理论上对一些常见的近似处理方法进行了讨论，计算了长为300μm，半径为30μm的六棱柱状冰晶粒子在不同波段的光散射相函数以及在波长2.2μm时，五种不同大小冰晶粒子的单次散射反照率。结果表明，即使在有吸收情况下，Snell公式和Lambert公式仍是近似成立的，而吸收效应对散射相函数有明显影响。     

参数化的多次散射激光雷达方程和它的反演理论 Ⅰ:方程

本文提出了一个参数化的多次散射激光雷达方程,该方程基于本文引出的四个因子,即几何消光因子、消光分布因子、前向散射因子和后向散射因子.前两个因子表征多次散射成分对大气消光系数分布、激光的发散角和接收视场角以及接收孔径的依赖关系,后两个因子表征多次散射成分对散射相函数的依赖关系.这个参数化多次散射雷达方程在241个数值试验中得以检验,这些试验包含很宽的大气条件和雷达几何参数,包括14个大气散射相函数,均匀和不均匀的大气消光系数分布,0.5至1之间变化的一次散射反照率,地基和空间站激光雷达两种情形.数值试验表明,在小于4的光学厚度内参数化的解和Monte-Carlo解之间的标准偏差小于27％,而本模式的计算时间比Monte-Carlo方法偏小4个数量级左右.本模式不仅适合于研究多次散射对激光回波信号和激光大气遥感的效应,而且对于考虑多次散射的激光大气探测而言,是一个合适的应用模式.     

气溶胶散射相函数的单站观测研究

利用2014年夏季在河北饶阳开展的“华北区域光化学立体试验”观测得到气溶胶辐射特性,根据三波长角散射浊度仪Aurora 4000测量获取的前向角散射系数（10°~90°）和后向散射系数,提出了一种基于浊度仪直接测量的气溶胶角散射系数和改进的HG相函数近似获取气溶胶散射相函数、不对称因子的拟合估算方法。分析了2014年6月16日—8月18日夏季观测试验期间河北饶阳地区大气气溶胶细粒子（PM_2.5）在635 nm,525 nm,450 nm 3个波段的不对称因子、相函数等的变化特征。结果表明:用改进的HG相函数近似能够较好地拟合河北饶阳实际观测的PM_2.5的气溶胶散射相函数。拟合得到河北饶阳地区观测期间干气溶胶细粒子在3个波段的平均不对称因子（g）分别为0.53±0.04（635 nm）,0.57±0.05（525 nm）和0.57±0.07（450 nm）。     

对流层与平流层大气气溶胶粒子的若干散射特性

本文应用Ｍｉｅ散射理论，采用简洁方案计算了ＩＡＭＡＰ提出的大气气溶胶主要粒子的散射效率因子及散射相函数，结果表明，大颗粒的散射能力以７５％硫酸液滴最强，其次是水滴，冰晶，沙尘性粒子；小粒子的散射能力仍以７５％硫酸滴最强，其次是沙尘性粒子，小颗粒相函数的前向后向基本对称；大粒相函数随Ｘ值增大而不对称加大；折射率实部不同，则相函数最小值出现在不同的散射角，折射率虚部较大的煤烟，相函数起伏较小，约在１０     

An easy algorithm for solving radiative transfer equation in clear atmosphere

An accurate and rapid method for solving radiative transfer equation is presented in this paper. According to the fact that the multiple scattering component of radiance is less sensitive to the error of phase function than the single scattering component is, we calculate the multiple scattering component by using delta-Eddington approximation and the single scattering component by solving radiative transfer equation. On the ground, when multiple mattering com-ponent is small, for example, when the total optical depth τ is small, the accurate radiance can be obtained with this method. For the need of the space remote sensing, the upward radiance at the top of the atmosphere is mainly studied, and an approximate depression is presented to correct the multiple scattering component. Compared with the more precise Gauss-Seidel method, the results from this method show an accuracy of better than 10% when zenith angle θ < 50o and τ ≤ 1. The computational speed of this method is, however, much faster than that of Gauss-Seidel method.     

Calculation on the light scattering function of hexagonal ice crystals

Hexagonal ice crystal is a basic form of the particles in cirrus. The emphasis in this paper is on discussing the computational results of scattering phase matrices for infrared absorptive band by making use of the model developed by the authors. Comparisons have been made between infrared and visible light as well as between hexagonal columns and plates and equivalent spheriods and spheres. It is found that the effects of light absorption on phase function may cause the decreases of scattering energy in side direction and the directions near backscattering, and weaken halo and rainbow peaks which are induced by the refractions and internal reflections. There is a general agreement in the phase functions for ice crystals with different shapes. However, the scattering intensity in side direction for spheres and in backward and backside directions for spheroids is weaker as compared with hexagons. It is believed that these features would, doubtless, have influences on the detection of cirrus by laser and radiation transfer in the atmosphere.     

大气粒子散射相函数的参数化方案比较及其改进

大气粒子散射相函数的参数化是大气辐射传输参数化的重要组成部分。文中全面比较了大气粒子的HenyeyGreenstein(HG)方案和双Henyey-Greenstein(DHG)方案,并在四流球谐函数展开累加法中,应用这两种相函数参数化方案计算气溶胶、云、霾粒子的反射率、透射率或吸收率。该研究结果表明:HG方案无法表现相函数的后向峰值,因而其计算的大气粒子反射率和透射率精度较差;DHG方案能较好地表征相函数的整体特征,但是该方案计算的相函数易出现后向异常峰值或为负值,并导致计算得到的气溶胶、云、霾粒子的反射率和透射率精度甚至会低于HG方案。对DHG方案进行进一步研究,提出了改进的DHG方案(MDHG)。MDHG方案计算结果稳定,并能很好表征相函数的前向和后向峰值的特征,其计算的大气粒子的反射率和透射率精度也较高。因此,MDHG方案是一种理想的相函数参数化方案。     

The solution of the vector radiative transfer equation using the discrete ordinates technique: Selected applications

The paper is devoted to the presentation of a newly developed radiative transfer code SCIAPOL_1.0 for a plane-parallel turbid slab illuminated by the monodirectional wide beam. The SCIAPOL_1.0 is based on the discrete-ordinates solution of the vector radiative transfer equation.The code is applied to a number of problems, including studies of the applicability of the scalar approximation for the calculation of light reflectance from aerosols, clouds, and molecular atmospheres. We also study the accuracy of the single scattering approximation as applied to the calculation of light reflection from molecular and cloudy atmospheres and propose new approximations for the calculation of the reflection function and the degree of light polarization under unpolarized light illumination conditions.     

参数化的多次散射雷达方程和它的反演理论 Ⅱ:反演理论

本文根据参数化的多次散射雷达方程,分析了激光多次散射对激光回波信号和一次散射雷达方程反演结果的效应,提出了迭代前向积分法和迭代后向积分法以求解参数化的多次散射雷达方程,并根据多次散射信号对云和气溶胶的前向散射相函数的高度敏感性提出了一个从双接收视场的多次散射激光回波信号,同时确定云和气溶胶消光系数分布和前向散射相函数的方法.此外,本文还根据数值试验分析了这些反演方法在地基激光雷达和空间站激光雷达两种情形下的适用性.     

小旋转椭球粒子群的微波散射特性

文中从不同方向线性偏振的入射波对小旋转椭球状降水粒子极化产生的散射出发 ,推导出散射能流密度函数 ,以及降水粒子群旋转轴处于不同状态下的散射截面 ,得出散射截面随降水粒子相态和入射波波长变化的一些曲线 ,其结果可供遥感反演计算使用。     

A Polarized Radiative Transfer Model Based on Successive Order of Scattering

Based on Successive Order of Scattering approach, a full Vector Radiative Transfer model (SOSVRT) for vertically inhomogeneous plane-parallel media has been developed. To overcome computational burden of convergence, a simple approximation technique by truncating scattering orders with a geometry serial is used to reduce computational time. Analytical Fourier decomposition of phase matrix with three symmetry relationships and two mutual inverse operators has been implemented to further improve the computation efficiency. To improve the accuracy, a post-processing procedure is implemented to accurately interpolate the Stokes vector at arbitrary angles. Comparisons with the benchmarks for an atmosphere of randomly orientated oblate spheroids show excellent agreement for each stokes parameter (within 0.1%). SOSVRT has been tested for different atmospheric condition against RT3, which is based on doubling-adding method, the results approve that SOSVRT is accurate and much more efficient in vector radiative transfer modeling, especially for optical thin atmosphere, which is the most cases in polarized radiative transfer simulation. SOSVRT is written in fortran 90 and the code is freely accessible by contacting the author.     

Measurements of desert dust optical characteristics at Porte au Sahara during SAMUM

Main optical characteristics of desert dust, such as phase function and single scattering albedo, have been derived from combinations of sun-/sky-radiometer and satellite measurements during the SAMUM experiment (10 May–10 June 2006) at the site Porte au Sahara (30.237°N, 5.607°W) in South Morocco. Scattering phase functions have been retrieved using combined data of spectral aerosol optical thickness (AOT) and spectral sky brightness in the almucantar, considering non-spherical light scattering. Intercomparisons of modelled top-of-atmosphere (TOA) reflectance with satellite observations of the Medium Resolution Imaging Spectrometer (MERIS) and Scanning Imaging Absorption Spectrometer for Atmospheric Chartography () instrument have been used for the estimation of spectral single scattering albedo. For the radiative transfer calculations scattering phase functions and AOT from ground-based observations have been used. The spectral single scattering albedo ranges from 0.93 in the blue to 0.98 at 753 nm.     

Polarising properties of the aerosols in the north‐eastern tropical Atlantic Ocean, with emphasis on the ACE‐2 period

Measurements of the polarisation state of the atmosphere were performed at Tenerife in June–July 1997, in the framework of ACE‐2 (second Aerosol Characterization Experiment), by 2 ground‐based instruments: RefPol (a LOA prototype) which took measurements at 445, 665, 870, 1610 nm in the solar principal plane; and an automatic CIMEL (CE 318) sun/sky‐photometer which measured polarised radiation at 870 nm in the same observational geometry. Measurements acquired during the campaign, as well as AERONET (AErosol RObotic NETwork) measurements acquired at the sites of Cape Verde and M'Bour, are processed with an algorithm determining the polarised single‐scattering sky‐radiance due to aerosols, directly proportional to the aerosol polarised phase function (representing the probability to scatter polarised radiation in the direction of the scattering angle). A good correlation between the Ångström exponent α, representing the spectral dependence of the extinction measurements, and the polarised phase function is observed on each set of data. The uncertainty of retrievals at 445 nm makes the determination of the spectral dependence of polarisation inconclusive but does not prevent confirming the dependence of the aerosol polarised phase function on α, at all wavelengths. An Ångström exponent of 1 corresponds to a polarised phase function of around 0.1 (±0.04), at 870 nm and at a scattering angle of 60°. For α between 0 and 0.4, the average value of the polarised phase function is 0.05. The correlation shows that polarisation is more sensitive to small particles than to large particles. The discrepancy between retrievals and Mie calculations from an AERONET size distribution, inverted from Izaña measurements acquired during a dust event, suggests the presence of small particles, not detected by total sky‐radiance measurements.     

Theoretical analysis of retrieving atmospheric columnar mie optical depth from downward total solar radiative flux

In this paper, the principle to determine the atmospheric columnar Mie optical depth from downward total solar radiative flux is theoretically studied, and the effect on Mie optical depth solution of the errors in surface albedo, single scattering albedo, asymmetrical factor of scattering phase function, instrumental constant and the approximate expression of diffusion flux is analyzed, and then a method for determining, surface albedo in shorter wavelength range is presented.     

求解非球形大粒子光散射问题的一种简明数值计算方法

对于实际大气中传输的非偏振自然光的散射问题,所关心的散射参量通常为散射强度和线偏振度。本文通过对光子沿随机抽样人射路径的散射几率进行统计,建立了计算多粒径大粒子系统单次散射相函数及线偏振度的一种简明数值方法。对于粒子表面具有曲率的情况,该方法可以避免处理由表面曲率引入的“发散因子”。由于大气中液滴的形状一般近似为旋转扁椭球,本文也根据所建立的数值计算方法,计算和讨论了旋转扁椭球形液滴的散射相函数和线偏振度。     

卫星对地遥感应用中的邻近效应研究

利用Monte-Carlo地气耦合辐射传输模式比较系统地进行了卫星视反射率对地表、大气和卫星参数的敏感性数值试验,重点研究了邻近效应对地表反射水平非均一分布的敏感性、邻近效应有效地表范围以及邻近效应与卫星高度的关系三个方面的问题.在定量分析的基础上,揭示了影响邻近效应的主要因子及其影响机制,给出了一些重要结论,包括:地表非均一引起的邻近效应的影响是非常重要的,特别是当目标反射率小于环境反射率时;气溶胶光学厚度越大,散射相函数对称性越强,卫星视反射率对环境反射率越敏趑感,邻近效应越明显;邻近效应的有效地表范围可达到几十公里,同样光学厚度条件下,与气溶胶相比,分子的有效地表范围更大,邻近效应也更强;卫星观测同一目标物时,邻近效应随着探测器高度增高而变大等.     

Derivation of scattering phase function from clear sky brightness distribution

Iteration procedure have been applied to obtain the scattering phase function from measurements of sky brightness on solar almucantar. The principle and calculating examples have been discussed.     

用于空间对地遥感的一个参数化辐射传输计算模式

一个足够精度的参数化向上亮度模式对空间对地遥感的大气订正应用是很有意义的。依据向上天空亮度对大气散射相函数、光学厚度、太阳天顶角、空间方位和天顶角等有关参数的依赖特性,基于大量的天空亮度数值模拟计算资料,本文发展了一个关于向上天空亮度的参数化模式。39440组的数值模拟对比资料表明,在气溶胶光学厚度#Aτt≤1,太阳天顶角小于72°,μ≤0.432 （天顶角小于65°）以及无云的条件下,由现在的参数化的模式所计算的向上亮度的误差一般小于6%。地表反射率越大,参数化模式的精度越高。参数化模式的精度一般随着光学厚度和太阳天顶角的增大而变差。