基于多格网算法的卫星图像恢复

将求解二次椭圆偏微分方程问题的多格网算法应用到卫星影像的恢复中。其基本思想是在将由总变分求极小生成的偏微分方程离散成为差分方程的过程中,采用不同大小的格网。在取得较好恢复结果的同时,提高了传统图像恢复算法的运算效率,降低了恢复运算所需要的时间。     

遥感邻近效应测量与数据分析

2004年和2005年开展了遥感邻近效应的理论研究,2次卫星、1次航空遥感同步试验测量和测量数据分析,在获取了邻近参数的基础上实现了对图像的邻近效应校正。本文介绍了2005年7月25日在官厅遥感实验场沙漠的卫星同步测量实验结果和2005年5月11日奥运场馆建设预留裸土地的ADS40航空遥感同步实验测量数据分析。改进测量方案和测量装置,并且对测量结果进行了对比分析。在两个相邻像元邻近效应分析的基础上,增加了9个点邻近像元效应分析和建立计算公式;在满足高斯条件和影像平坦性要求的前提下,直线高斯相邻点（d=2R）条件下亮度分布交叉点在（d=R）,像元分辨率相互影响约为12.5%,实际测量中亮度分布交叉点和相互影响偏向于亮度值相对低的像元。     

Crustal Electrical Structure and Deep Metallogenic Potential in Northern Wuyi Area (South China), based on Magnetotelluric Data

The northern Wuyi area, which is located in the northern Wuyi metallogenic belt, has superior mineralization conditions. The Pingxiang–Guangfeng–Jiangshan–Shaoxing fault (PSF) extends across the whole region regardless of whether or how the PSF relates to the near-surface mineralization. We carried out an MT survey in the region and obtained a reliable 2D model of the crustal electrical structure to a depth of 30 km. In the resistivity model, we inferred that a continuous high conductivity belt that ranges from the shallow to deep crust is a part of the PSF. Then, we estimated the fluid content and pressure gradient to identify the deep sources of fluid as well as its pattern of motion pattern. Finally, we proposed a model for the deep metallogenic migration processes that combines geological data, fluid content data, pressure gradient data, and the subsurface resistivity model. The model analysis showed that the Jiangnan orogenic belt and the Cathaysia block formed the PSF during the process of com. The deep fluid migrated upward through the PSF to the shallow crust. Therefore, we believe that the PSF is an ore-forming fluid migration channel and that it laid the material basis for large-scale mineralization in the shallow crust.     

斜视角度下大气交叉辐射影响分析

大气交叉辐射影响是遥感数据中存在的大气影响的重要组成部分之一。多角度遥感是通过一定的观测角获取地面遥感数据 ,因而对斜视角度下大气交叉辐射影响的分析具有重要意义 ,这也是现有大气订正模型中较少涉及的部分。大气交叉辐射影响可以用点扩散函数表示 ,在频率域则可以用调制传递函数表示 ,因而通过对上述两个函数进行分析 ,可以掌握大气交叉辐射影响的特征 ,进而加以订正。通过分析发现 ,大气交叉辐射影响不仅与大气光学厚度、遥感图象分辨率等因子有关 ,而且与传感器观测角度有关 ,该文给出其解析表达式 ,并得出其变化规律     

不受刀刃边缘倾角约束的遥感影像点扩散函数稳健计算方法

采用传统刀刃法提取PSF时,只有在刀刃边缘近似平行或垂直于采样方向情况下才能得到好的效果,这样限制了刀刃法提取PSF进行图像恢复的广泛应用。本文提出了一种稳健的基于倾斜刀刃的图像的PSF计算模型,不仅在提取理想刀刃状况下(与采样方向近似垂直或平行)与传统方法等价,而且对倾斜刀刃提取PSF进行图像恢复也能得到理想效果,所恢复的图像在峰值信噪比(PSNR),均方差测度(MSE)和信噪比(SNR)等方面,都要优于传统方法,利用任意倾角的刀刃边缘提取的PSF都可以基本达到理想刀刃所提取的PSF的效果,因而提高了刀刃法提取PSF进行图像恢复的鲁棒性和通用性。本文分别从理论和实践上论证了模型的有效性,并采用模拟实验数据和ADS40航空影像数据验证了方法的正确性。     

ROV based underwater blurred image restoration

1　Introduction　TheROV (RemoteOperatedVehicle)isakindofsystemthatcanbeusedforunderwatermeasurementanddetection (Caimi,1996 ;KevernandLeGall,1991) .Inthispaper ,theirradianceofthelightre flectedbythetargetthroughwaterbodiesindifferentconditionsissimulatedbyacomputer .Underdiffer entwaterconditions,therelationbetweentheirradi anceandthedistanceispresented .Thenthemaxi mumdetectiondistanceofthedetectorcanbeob tained .WealsorestoretheunderwaterblurryimagesusingtheWienerfilterbasedonthesimula…     

CBERS-1 PSF估计与图像复原

分析了遥感图像获取过程中导致图像退化模糊的原因。讨论了一种借助图像中的特定线状目标信息(如桥梁、堤坝等)，采用经验拟合的方式提取图像获取、传输过程中的点扩散函数，并利用该点扩散函数结合频域维纳滤波器求解去图像模糊的空域反卷积算子。将该方法应用于中巴资源卫星一号(CBERS-1)图像，图像质量得到明显的提高，收到了较好的复原效果。     

基于刃边法与正则化方法的遥感影像复原

提出了一种基于刃边法PSF估计和保边缘正则化方法的遥感影像复原方法,利用刃边法,建立正则化复原模型,以及最速下降法进行复原,实现了优于传统的维纳滤波、约束最小平方等方法的复原效果。     

一种基于CLEAN方法的小图像恢复快速算法

针对小分辨率图像恢复 ,分析了小分辨率图像中使用CLEAN技术的特殊性 ,并根据H¨ogbom的CLEAN技术核心思想 ,提出了对CLEAN技术的改进 ,并将改进后的CLEAN方法与其它图像恢复方法进行了比较 ,在小图像恢复的效果和算法执行速度方面都取得了较好效果。     

Keck AO observations of Io in and out of eclipse

We present adaptive optics (AO) observations of Io taken with the W.M. Keck II telescope on 18 December 2001 (UT) before the satellite went into eclipse, and while it was in Jupiter's shadow. Making these kind of Io-in-eclipse observations, as well as the associated data reduction and analysis are challenging; hence one focus of the paper is to explain the methods and tools used for these data sets. For the sunlit images Io itself was used as the wavefront reference source, while nearby Ganymede was used as reference ‘star’ when Io was in eclipse. Observations were obtained in K′-, L′-, and M-bands. The sunlit images have been deconvolved using MISTRAL. The Io-in-eclipse data were deconvolved with IDAC and MISTRAL. The former gives better results, both in absolute photometry and in matching the original images. We determined the flux densities of the hot spots from the original Io-in-eclipse data with StarFinder, as well as from the deconvolved images by integrating the intensity over the relevant areas. We determined the highly anisoplanatic PSF via a FFT method from the original data, and used this in StarFinder and as a starting PSF for IDAC and MISTRAL. We derived temperatures and areal coverage of all 19 spots detected in both K′- and L′-band images of Io-in-eclipse. We also determined temperatures and areal coverage of the hot spots visible on the L′- and M-band images of sunlit Io. Most volcanoes contain a compact hot ‘core’ (?10 km² at 600-800 K) within a larger area at lower temperatures (e.g., ∼10²-10⁴ km² at 300-500 K). The total heat flow contributed by these active volcanoes is 0.2 W m⁻², ∼8% of the average global heat flow measured at 5-20 μm by Veeder et al. [J. Geophys. Res. 99 (1994) 17095].