NUMERICAL EXPERIMENTS AND ANALYSIS OF DIGITAL FILTER INITIALIZATION FOR WRF MODEL     

王舒畅  黄思训  张卫民  朱小谦  曹小群  李毅 《热带气象学报(英文版)》2008,14(1):1-10

Initialization and initial imbalance problem were discussed in the context of a three-dimensional variational data assimilation system of the new generation “Weather Research and Forecasting Model”. Several options of digital filter initialization have been tested with a rain storm case. It is shown that digital filter initialization, especially diabatic digital filter initialization and twice digital filter initialization, have effectively removed spurious high frequency noise from initial data for numerical weather prediction and produced balanced initial conditions. For six consecutive intermittent data assimilation cycles covering a 3-day period, mean initialization increments and impact on forecast variables are studied. DFI has been demonstrated to provide better adjustment of the hydrometeors and vertical velocity, reduced spin-up time, and improved forecast variables quantity.  相似文献   

应用GeoStar建立数字佛像三维模型的研究     

朱宜萱  黎景良  宁晓刚  李华玮 《测绘信息与工程》2004,29(4):7-9

通过使用GeoStar系列软件进行数字三维佛像建模 ,进一步实现佛像的动态漫游 ,从而得出了一种基于等值线图建立数字表面模型并进行空间漫游的可行技术 ;通过研究卧佛的历史资料 ,对数字佛像模型进行修补 ,探讨了实现佛像表面三维可视化复原的方法  相似文献   

特征级高分辨率遥感图像快速自动配准     

何梦梦  郭擎  李安  陈俊  陈勃  冯旭祥 《遥感学报》2018,22(2):277-292

随着遥感图像分辨率的日益提高,遥感图像的尺寸和数据量也不断地增大,同时随着遥感应用的发展,对图像配准的性能也提出越来越高的要求,基于此,提出一种特征级高分辨率遥感图像快速自动配准方法。首先,对图像进行Haar小波变换,基于小波变换后的近似图像进行配准以提高配准速度;其次,根据不同的遥感图像来源使用不同的特征提取方法(光学图像使用Canny边缘提取算子,SAR图像使用Ratio Of Averages算子),并将线特征转化为点特征;然后,依据特征点间最小角与次小角的角度之比小于某一阈值来确定初始匹配点对;最后,利用改进的随机抽样一致性算法滤除错误匹配点对,并结合分块思想均匀选取匹配点对计算仿射变换参数,进一步提高配准精度。为了验证本文方法的有效性,选择高分辨率World View-2图像、Pleiades图像和Terra SAR图像进行了实验,并与典型的SIFT算法、SURF算法进行比较分析,采用匹配率、匹配效率、均方根误差和时间消耗4个定量评价指标来客观评价算法的配准性能。实验结果表明,本文方法具有较好的有效性,且在不同的情况下具有较高的配准精度。本文提出的特征级高分辨率遥感图像快速自动配准方法,多组高分辨率遥感图像数据的配准实验结果表明该方法能快速实现并具有较高的配准精度和较好的鲁棒性。  相似文献   

多特征差分核支持向量机模型的湿地变化检测   总被引：1，自引：0，他引：1  

潘琛  冯琰  林怡  陈映鹰 《测绘科学》2014,39(12):104-108,119

文章通过对不同特征空间、不同时相信息和不同类别引入多核函数组合和类别加权方式,构建了基于多特征差分核的加权支持向量机变化检测模型,能够获得平衡样本大小、综合多特征空间的变化检测结果.以上海崇明岛东端地区为例,利用4期ETM+/TM影像数据,基于构建的SVM变化检测模型,最终得到研究区湿地资源的空间变化格局,结果表明检测模型能够有效、准确地提取多种湿地变化类别的空间分布信息;并从景观水平上对检测结果进行格局分析,为湿地保护和管理提供科学参考.  相似文献   

New brown dwarf candidates in the Pleiades     

T. Eisenbeiss  M. Moualla  M. Mugrauer  T.O.B. Schmidt  St. Raetz  R. Neuhuser  Ch. Ginski  M.M. Hohle  A. Koeltzsch  C. Marka  W. Rammo  A. Reithe  T. Roell  M. Va&#x;ko 《Astronomische Nachrichten》2009,330(5):439-458

We have performed deep, wide‐field imaging on a ∼0.4 deg² field in the Pleiades (Melotte 22). The selected field was not yet target of a deep search for low mass stars and brown dwarfs. Our limiting magnitudes are R ∼ 22 mag and I ∼ 20 mag, sufficient to detect brown dwarf candidates down to 40 M_J. We found 197 objects, whose location in the (I, R – I) color magnitude diagram is consistent with the age and the distance of the Pleiades. Using CTK R and I as well as JHK photometry from our data and the 2MASS survey we were able to identify 7 new brown dwarf candidates. We present our data reduction technique, which enables us to resample, calibrate, and co‐add many images by just two steps. We estimate the interstellar extinction and the spectral type from our optical and the NIR data using a two‐dimensional χ² fitting (© 2009 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)  相似文献   

Cosmic‐ray rejection for single spectroscopic CCD images by means of template matching     

C. Wang  Z.Q. Zhu  Z.F. Ye 《Astronomische Nachrichten》2009,330(7):749-754

This article describes a novel algorithm for cosmic‐ray rejection in single spectroscopic CCD images. This algorithm is based on a variation of template matching. It focuses on identifying those pixels belong to spectra, while other conventional algorithms tried to locate the cosmic‐ray hits directly. The main principle is applying template matching to find suspicious blocks, which is followed by surface patching to locate the legitimate pixels accurately. Therefore, the rest pixels are the ones corrupted by cosmic‐ray hits. Meanwhile, almost all the parameters are automatically extracted from the images. Examples of its performance are given for both simulated and observed images. It shows an advantage of significantly low false alarm rate with relatively high detection rate (© 2009 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)  相似文献   

A novel multifrequency technique for the detection of point sources in cosmic microwave background maps     

D. Herranz  M. López-Caniego  J. L. Sanz  J. González-Nuevo 《Monthly notices of the Royal Astronomical Society》2009,394(1):510-520

In this work we address the problem of simultaneous multifrequency detection of extragalactic point sources in the maps of the cosmic microwave background. We apply a new linear filtering technique, the 'matched matrix filters', that incorporates full spatial information, including the cross-correlation among channels, without making any a priori assumption about the spectral behaviour of the sources. A substantial reduction of the background is achieved thanks to the optimal combination of filtered maps. We describe the new technique in detail and apply it to the detection of radio sources and estimation of their parameters in realistic all-sky Planck simulations at 30, 44, 70 and 100 GHz. Then, we compare the results with the single-frequency approach based on the standard matched filter, in terms of reliability, completeness and flux accuracy of the resulting point source catalogues. The new filters outperform the standard matched filters for all these indexes at 30, 44 and 70 GHz, whereas at 100 GHz both kinds of filters have a similar performance. We find a notable increment of the number of true detections for a fixed reliability level. In particular, for a 95 per cent reliability we practically double the number of detections at 30, 44 and 70 GHz.  相似文献   

Wavelet domain Bayesian denoising of string signal in the cosmic microwave background     

D. K. Hammond  Y. Wiaux  P. Vandergheynst 《Monthly notices of the Royal Astronomical Society》2009,398(3):1317-1332

An algorithm is proposed for denoising the signal induced by cosmic strings in the cosmic microwave background. A Bayesian approach is taken, based on modelling the string signal in the wavelet domain with generalized Gaussian distributions. Good performance of the algorithm is demonstrated by simulated experiments at arcminute resolution under noise conditions including primary and secondary cosmic microwave background anisotropies, as well as instrumental noise.  相似文献   

Automatic morphological classification of galaxy images     

Lior Shamir 《Monthly notices of the Royal Astronomical Society》2009,399(3):1367-1372

We describe an image analysis supervised learning algorithm that can automatically classify galaxy images. The algorithm is first trained using manually classified images of elliptical, spiral and edge-on galaxies. A large set of image features is extracted from each image, and the most informative features are selected using Fisher scores. Test images can then be classified using a simple Weighted Nearest Neighbour rule such that the Fisher scores are used as the feature weights. Experimental results show that galaxy images from Galaxy Zoo can be classified automatically to spiral, elliptical and edge-on galaxies with an accuracy of ∼90 per cent compared to classifications carried out by the author. Full compilable source code of the algorithm is available for free download, and its general-purpose nature makes it suitable for other uses that involve automatic image analysis of celestial objects.  相似文献   

Adaptive Optics Image Restoration Based on Frame Selection and Multi-frame Blind Deconvolution     

TIAN Yu  RAO Chang-hui  WEI Kai 《Chinese Astronomy and Astrophysics》2009

Restricted by the observational condition and the hardware, adaptive optics can only make a partial correction of the optical images blurred by atmospheric turbulence. A postprocessing method based on frame selection and multi-frame blind deconvolution is proposed for the restoration of high-resolution adaptive optics images. By frame selection we mean we first make a selection of the degraded (blurred) images for participation in the iterative blind deconvolution calculation, with no need of any a priori knowledge, and with only a positivity constraint. This method has been applied to the restoration of some stellar images observed by the 61-element adaptive optics system installed on the Yunnan Observatory 1.2m telescope. The experimental results indicate that this method can effectively compensate for the residual errors of the adaptive optics system on the image, and the restored image can reach the diffraction-limited quality.  相似文献