利用Sentinel-3A OLCI可见光通道反演台湾岛气溶胶光学厚度

OLCI（Ocean Land Colour Instrument）作为MERIS（Medium Resolution Imaging Spectrometer）的后继升级版传感器,在气溶胶反演中存在潜在优势,但是目前利用OLCI数据进行气溶胶监测的研究较少。因此,本文针对OLCI多通道反射特征开发了OLCI云检测算法,并对传统查找表构建方法进行改进,根据观测几何特征提出动态查找表法,并通过光谱卷积方式等效转换MODIS和OLCI红蓝通道地表反射率并获取OLCI红蓝通道地表反射率固定关系,进而实现台湾岛550 nm处的AOD反演。与550 nm处AERONET level 2.0 AOD验证结果首先表明不同季节、不同站点的精度表现存在一定差异,其次相对于同期MOD04_3K AOD产品,本文反演结果与全球气溶胶自动观测网（AERONET）站点实测值之间表现出更显著 的相关性（R²=0.8199）,均方根误差（RMSE）从0.175下降到0.113,相对平均误差（RME）从33.6%下降到26.7%,且67.5%的OLCI AOD落在预测误差（EE）区间内,明显大于MOD04_3K AOD落在预测误差区间的百分比（55.7%）。此外,误差分析表明,当实际AOD值较低时,红蓝通道地表反射率之间关系的误判会导致较为明显的AOD反演相对误差。     

Can MODIS Detect Trends in Aerosol Optical Depth over Land?

The Moderate Resolution Imaging Spectroradiometer(MODIS) sensor onboard NASA's Aqua satellite has been collecting valuable data about the Earth system for more than 14 years, and one of the benefits of this is that it has made it possible to detect the long-term variation in aerosol loading across the globe. However, the long-term aerosol optical depth(AOD)trends derived from MODIS need careful validation and assessment, especially over land. Using AOD products with at least 70 months' worth of measurements collected during 2002–15 at 53 Aerosol Robotic Network(AERONET) sites over land,Mann–Kendall(MK) trends in AOD were derived and taken as the ground truth data for evaluating the corresponding results from MODIS onboard Aqua. The results showed that the AERONET AOD trends over all sites in Europe and North America, as well as most sites in Africa and Asia, can be reproduced by MODIS/Aqua. However, disagreement in AOD trends between MODIS and AERONET was found at a few sites in Australia and South America. The AOD trends calculated from AERONET instantaneous data at the MODIS overpass times were consistent with those from AERONET daily data, which suggests that the AOD trends derived from satellite measurements of 1–2 overpasses may be representative of those from daily measurements.     

基于FY-2D的新疆强对流云的识别

利用2007-2013年新疆的十场强对流天气过程以及与之相应的FY-2D静止气象卫星数据,分析了强对流云红外一通道、红外二通道、水汽通道及通道差的光谱特征,提取强对流云团样本点,采用统计方法确定判识指标的阈值范围,构建多通道多阈值判识方法。利用三场天气过程的地面实测降水资料分别验证了单时次和整场天气过程强对流云判识的准确性,结果表明：单时次强对流云的识别区域与发生降雨台站一致的准确率为83%;在整个天气过程中,强对流频次分布与降水实况吻合度较高,说明随着对流云团的移动和发展,判识区域与地面降水区域保持一致,验证了判识方法有效,阈值选取合理,可以为监测暴雨天气系统的发生、发展提供支持。     

光学观测小波方法的比较研究

本文系统地分析国外几十年来用光学方法对海面微尺度波浪观测的研究方法和观测装置,从中比较各自的优缺点,对于今后在此方面的研究工作提供帮助。     

南黄海浮游植物与水色透明度之间相关关系的研究

本文根据 １９９５ 年 ９ 月在南黄海获取的资料,分析和讨论了该水域浮游植物现存量（叶绿素 ａ （ Ｃ Ｈ ））、初级生产力（ Ｐ Ｐ） 和海水光学参数（透明度（ Ｓ Ｔ））、水色（ Ｗ Ｃ）） 之间的相关关系。分析结果表明,夏末秋初南黄海 Ｃ Ｈ 与 Ｐ Ｐ, Ｃ Ｈ 与 Ｗ Ｃ 和 Ｐ Ｐ 与 Ｗ Ｃ 以及悬浮物（ Ｓ Ｓ） 与 Ｗ Ｃ 之间均有良好的正相关关系。相关式分别为： Ｐ Ｐ ＝ ２２５１９ｌｎ（ Ｃ Ｈ ） ＋ ４８８９１ 或 Ｐ Ｐ ＝ ５ Ｅ－ ０５ Ｃ Ｈ １６４６４（ Ｒ２ ＝ ０７０３７）; Ｗ Ｃ ＝ ４０３ｌｎ（ Ｃ Ｈ ） ＋ ８９７６８ 或 Ｗ Ｃ ＝ ７１３０６ Ｃ Ｈ ０４７４７ （ Ｒ２ ＝０７９２１）; Ｃ Ｈ ＝ １５４３７ｌｎ（ Ｓ Ｓ） ＋ １３６４７ 或 Ｃ Ｈ ＝ ０７４９９ Ｓ Ｓ１２５２（ Ｒ２ ＝ ０７２２３）; Ｐ Ｐ ＝３３２８６ｌｎ Ｓ Ｓ＋ １５２２２ 或 Ｐ Ｐ ＝ ３３０２９ Ｓ Ｓ０５６９４ （ Ｒ２ ＝ ０５４７６）; Ｐ Ｐ ＝ ４２５８８ｌｎ（ Ｗ Ｃ） － ３７０７１或 Ｐ Ｐ ＝ ６６５１２ Ｗ Ｃ０８６６５（ Ｒ２ ＝ ０６７３１） 以 及 Ｓ Ｓ ＝ １４０１９ｌｎ（ Ｗ Ｃ） － １３３６３      

四种海水透明度现场测量方法的对比分析及发展趋势研究

随着海洋探测的不断发展,海水透明度作为海水光学性质的一个重要参量,也越来越受到人们的关注。文章对比分析了4种海水透明度现场测量方法:透明度盘法~([1])、光纤式高光谱剖面测量法~([2])、激光衰减测量法~([3])和基于双光路原理的海水IOPs高光谱测量法~([4]),主要分析了4种方法的测量原理,对比各自的优缺点,并提出了海水透明度测量未来发展设想。     

Spectral Reflectance Analysis of the Caribbean Sea

Reflectance spectral curves were analysed by a derivative method. Derivative reflectance spectra revealed concealed peaks of both reflectance and absorption curves of Caribbean seawater and elements contained within it. Reflectance curves showed a predominant blue colour (400–500 nm) characteristic of Caribbean oligotrophic waters, conspicuous peaks result from the optical properties of chlorophyll a and seawater. Reflectance curves had a similar spectral response. This paper analyses reflectance spectra of surface seawater at 31 stations in the Caribbean Sea during the summer of 2001.     

北冰洋中央密集冰区海冰对太阳短波辐射能吸收的观测研究

太阳辐射能是海冰融化的最主要能源,基于在2008年8月21~27日北极加拿大海盆中部为期8天的冰站考察中海冰光学观测数据,研究了北冰洋中央密集冰区海冰吸收的太阳辐射能。通过现场直接观测,确定了海冰透射率、反照率、吸收率及其随冰厚的变化,得出海冰对太阳短波辐射的吸收率大约为到达冰面太阳辐射的16%,大部分被冰雪表面反射。为期3天的对太阳辐射的观测表明,虽然到达北冰洋中央密集冰区的太阳辐射能并不少,但由于云和雾覆盖的时间所占的比例很大,有将近57%被大气削弱,其余的又有77%左右被冰雪表面反射回太空,海冰吸收的热量只有10.2 W/m²,相当于每天融化2.6 mm的冰,1 m厚海冰全部融化需要380天,不足以为海冰融化提供足够的热量。因此北冰洋中央密集冰区终年被海冰覆盖,即使在北冰洋海冰面积骤减的现状下,那里的海冰密集度仍然接近100%。然而,文章的结果指出：大气中云和雾大幅度减少、积雪层融化、海冰厚度减小、融池的比例增加等因素都会大幅度增加海冰吸收的热量,未来这些过程的发生有可能导致北冰洋密集冰区的海冰快速融化。     

中国3个典型城市气溶胶光学厚度地基观测及其MODIS气溶胶产品精度分析

利用中国太阳分光观测网的观测资料结合MODIS(中分辨率成像光谱仪)的气溶胶产品分析了北京、兰州、上海3个典型区域城市的气溶胶光学特性。结果表明:北京AOD(气溶胶光学厚度)年平均为0.41±0.35,春夏高,秋冬低,Angstrm波长指数α年平均为1.40±0.85表现为细模态粒子,MODIS的光学厚度为0.52±0.39与地面观测相关系数为0.91,存在系统性高估;兰州AOD年平均为0.55±0.21,夏季最低,秋冬较高,α年平均为0.95±0.20表现为粗模态粒子,MODIS光学厚度为0.43±0.21与地面观测相关系数仅为0.07,存在系统性低估;上海AOD年平均为0.55±0.21,无明显季节变化,α平均为1.03±0.25,MODIS光学厚度为0.74±0.30与地面观测相关系数为0.75,存在系统性高估。城市地理位置和复杂地表等原因造成反照率的不确定,MODIS气溶胶产品在这3个城市的反演效果仍有很大提升空间。     

A reanalysis of the Apollo light scattering observations, and implications for lunar exospheric dust

Conspicuous excess brightness, exceeding that expected from coronal and zodiacal light (CZL), was observed above the lunar horizon in the Apollo 15 coronal photographic sequence acquired immediately after orbital sunset (surface sunrise). This excess brightness systematically faded as the Command Module moved farther into shadow, eventually becoming indistinguishable from the CZL background. These observations have previously been attributed to scattering by ultrafine dust grains (radius ∼0.1 microns) in the lunar exosphere, and used to obtain coarse estimates of dust concentration at several altitudes and an order-of-magnitude estimate of ∼10⁻⁹ g cm⁻² for the column mass of dust near the terminator, collectively referred to as model “0”.We have reanalyzed the Apollo 15 orbital sunset sequence by incorporating the known sightline geometries in a Mie-scattering simulation code, and then inverting the measured intensities to retrieve exospheric dust concentration as a function of altitude and distance from the terminator. Results are presented in terms of monodisperse (single grain size) dust distributions. For a grain radius of 0.10 microns, our retrieved dust concentration near the terminator (∼0.010 cm⁻³) is in agreement with model “0” at z=10 km, as is the dust column mass (∼3–6×10⁻¹⁰ g cm⁻²), but the present results indicate generally larger dust scale heights, and much lower concentrations near 1 km (<0.08 cm⁻³ vs. a few times 0.1 cm⁻³ for model “0"). The concentration of dust at high altitudes (z>50 km) is virtually unconstrained by the measurements. The dust exosphere extends into shadow a distance somewhere between 100 and 200 km from the terminator, depending on the uncertain contribution of CZL to the total brightness. These refined estimates of the distribution and concentration of exospheric dust above the lunar sunrise terminator should place new and more rigorous constraints on exospheric dust transport models, as well as provide valuable support for upcoming missions such as the Lunar Atmosphere and Dust Environment Explorer (LADEE).