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10.2W/m2,相当于每天融化2.6mm的冰,1m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.     

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。     

基于聚焦合成的显微三维成像系统

本文利用显微镜物镜焦深范围有限,显微三维样本成像时需要一序列图像才能聚焦清晰特点,研究开发利用图像处理技术扩展显微成像焦深范围,应用改进Laplacian聚焦算子实现序列图像的融合显示,同时,提出了一种基于区域小波变换的序列显微图像融合算法并加以实现.用高斯插值算法得到三维显微图像的高度图,设计了一种网格轮廓线算法对高度索引图进行了三维重建显示和测量,并利用立体视觉原理生成了三维物体的左右视图和立体视图.应用此方法可以完成显微目标的表面三维参数的测量分析.     

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).     

Excitation of ion waves by charged dust beams in ionospheric aerosol release experiments

Ion waves excited by charged dust beams streaming across or along the geomagnetic field in the ionosphere may be generated by plasma instabilities during aerosol release experiments. The injection speed of the dust and gas is comparable to or larger than the ion thermal speed in the background plasma. The dust grains can get charged by plasma collection from the ambient ionosphere, and can thus act as a charged beam that excites instabilities in the background plasma. The theory is applied to relatively early time scales of the order of in the dust-gas cloud expansion, with wave frequencies that are larger than the ion gyrofrequency, and collisions with neutrals are included.     

Meteorological causes of Harmattan dust in West Africa

We investigated the temporal dynamics of dust entrainment in the Bodélé Depression, Central Sahara, to better understand the intra-annual variability of aerosol emission in the world's largest dust source. The linkages between dust entrainment and large-scale meteorological factors were examined by correlating several meteorological variables in the Mediterranean and Africa north of the equator with the aerosol concentrations in the Bodélé Depression separately for winter and summer. The methodological tools applied are NCEP/NCAR reanalysis data and the aerosol index of the Total Ozone Mapping Spectrometer (TOMS-AI), available for 15 years from 1978 to 1993. We found that dust mobilisation during the Harmattan season is highly dependent on air pressure variability in the Mediterranean area. High pressure to the north of the Bodélé intensifies the NE trade winds, leading to an increased entrainment of dust in the Bodélé Depression. In summer, dust mobilization cannot be explained by the large scale meteorological conditions. This highlights the importance of local to regional wind systems linked to the northernmost position of the intertropical convection zone (ITCZ) during this time.     

天空光遮挡法水体光谱测量便携版漂浮式光学浮标研发与应用

离水辐亮度Lw(Water-leaving radiance)是水色遥感现场观测中的关键物理量之一,由其计算获得的遥感反射率Rrs(Remote sensing reflectance)是水色遥感参数反演的最基本参数.天空光遮挡法SBA(Skylight-blocked approach)可以直接测量水体离水辐亮度,作...     

2010年民勤沙地近地面沙尘气溶胶浓度特征

为了更好地研究沙尘气溶胶起沙和输送特征,2010年4—5月,在民勤周边沙地利用EZ LIDAR ALS300&ALS450型激光雷达和 GRIMM 180型颗粒物采样器进行了大气气溶胶的外场连续观测,取得了晴天、浮尘、扬沙和沙尘暴天气条件下沙尘气溶胶总后向散射垂直剖面图和PM₁₀、PM_2.5、PM_1.0质量浓度采样资料,其中包含“0424”特强沙尘暴过程资料。结果表明：春季民勤近地层大气中沙尘气溶胶浓度较高,且随气象要素的变化很大;在整个观测期内,PM₁₀、PM_2.5、PM_1.0的平均质量浓度分别为202.3、57.4 μg/m³、16.7 μg/m³。在不同天气条件下,PM₁₀、PM_2.5、PM_1.0质量浓度的变化有很好的相关性,但变化趋势有所不同。在沙尘暴天气条件下,PM₁₀的日平均质量浓度高达2469.1μg/m³,是背景天气条件下PM10日平均质量浓度的100多倍,是浮尘天气条件下PM10日平均质量浓度的8倍,是扬沙天气条件下PM₁₀日平均质量浓度的2倍。PM_2.5在沙尘暴天气下日平均质量浓度为460.3 μg/m³,是背景天气条件下PM_2.5日平均质量浓度的45倍,是浮尘天气条件下PM_2.5日平均质量浓度的6倍,是扬沙天气条件下PM_2.5日平均质量浓度的1.4倍。PM_1.0在沙尘暴天气条件下的日平均浓度为92.7 μg/m³,是背景天气条件下PM_1.0日平均浓度的13倍,是浮尘天气条件下PM_1.0日平均浓度的7倍,是扬沙天气条件下PM_1.0日平均浓度的1.3倍。可见,风速增大时沙尘粒子浓度的增加对粒子粒径是有选择的,小粒子比重随沙尘浓度增加而相对减小,大粒子比重随沙尘浓度增加而相对增多;通过对“0424”特强沙尘暴过程的研究表明,一次沙尘暴过程往往包括沙尘暴、扬沙和浮尘天气中的两种类型;通过对激光雷达数据分析发现,在强沙尘暴发生过程当中,民勤沙地发生了非常严重的风蚀起沙现象。