细缝裁减和非均匀映射结合的图像自适应方法

采用将细缝裁减和非均匀映射相结合的图像尺寸自适应框架,提出了一种基于内容的图像重要信息变形的度量方法.首先提取原始图像的重要性像素点,利用细缝裁减去掉一条像素细缝后,相应的重要性像素点会被更新.对于图像中保留的重要性像素点,计算它们的子图像平均偏差(ADSI,Average Difference of Sub Images);对于被移除的重要性像素点,计算它们的平均丢失能量(ALE,Average Lost Energy).通过ADSI和ALE可计算出重要信息变形的度量函数(IIDF,Important Information Deformation Function)的值,通过分析IIDF的趋势得到细缝裁减的终止条件,然后改用非均匀映射方法(non-homogeneous warping)将图像自适应到目标尺寸.实验结果证明,新方法处理的结果图像重要区域变形较小,并且计算效率比较高.     

直升机红外辐射的理论计算

选取了适当的理论计算方法,给出了计算公式和计算步骤,进而在所假设的飞行状态下计算了直升机的红外辐射,包括直升机发动机的排气管辐射和直升机蒙皮辐射的全辐射量和红外波段辐射量,最后对计算结果进行了分析。从分析来看,计算结果是可信的。     

气动热试验中稳态热流测量技术研究

高超声速飞行器热防护系统防热结构、防热材料的地面防热试验研究中,模型表面热流大小是关键参数之一。介绍了防热试验研究中瞬态热流测量技术,详细分析和论述了将红外热图测试技术和水卡量热计测试技术相结合,利用动态换热平衡和能量守恒原理实现防热试验中稳态热流测量的基本理论和测试方法,并给出初步试验结果。该技术的建立,为地面防热材料筛选和材料防热机理研究提供了有效、可行的测试手段。     

New method of enhancement using wavelet transforms applied to SODISM telescope

PICARD is a space-based observatory hosting the Solar Diameter Imager and Surface Mapper (SODISM) telescope, which has continuously observed the Sun from July 2010 and up to March 2014. In order to study the fine structure of the solar surface, it is helpful to apply techniques that enhance the images so as to improve the visibility of solar features such as sunspots or faculae. The objective of this work is to develop an innovative technique to enhance the quality of the SODISM images in the five wavelengths monitored by the telescope at 215.0?nm, 393.37?nm, 535.7?nm, 607.1?nm and 782.2?nm. An enhancement technique using interpolation of the high-frequency sub-bands obtained by Discrete Wavelet Transforms (DWT) and the input image is applied to the SODISM images. The input images are decomposed by the DWT as well as Stationary Wavelet Transform (SWT) into four separate sub-bands in horizontal and vertical directions namely, low-low (LL), low–high (LH), high-low (HL) and high–high (HH) frequencies. The DWT high frequency sub-bands are interpolated by a factor 2. The estimated high frequency sub-bands (edges) are enhanced by introducing an intermediate stage using a Stationary Wavelet Transform (SWT), and then all these sub-bands and input image are combined and interpolated with half of the interpolation factor α/2, used to interpolate the high-frequency sub-bands, in order to reach the required size for IDWT processing. Quantitative and visual results show the superiority of the proposed technique over a bicubic image resolution enhancement technique. In addition, filling factors for sunspots are calculated from SODISM images and results are presented in this work.     

Impacts of the PAH size and the radiation intensity on the IR features of illuminated dust within the reflection nebulae

Interstellar dust grains are illuminated in the reflection nebulae. Under conditions of the PAH size and the intensity of the interstellar radiation field, we follow their impact on the PAH aromatic infrared bands using the numerical DustEM code. For a dust model consisting of PAH, amorphous C and amorphous silicate, the PAH size varies in a range from 0.31 to 4.9 nm while the radiation intensity varies by a scale factor from 0.1 to 10⁴. Various trends of the results show the effect of varying both the PAH size and the radiation intensity on the strength of the aromatic mid-IR bands. Through small PAH sizes less than 0.7 nm, the grain temperature distribution of PAHs shows a small variation within 2–3 K at low radiation intensity while it increases to 15 and 8 K for PAH⁰ and PAH⁺, respectively, at higher radiation intensity. In final the variability in these results reveals the evolution of the dust grains under the physical space conditions of the reflection nebulae. In the mid-IR region, the contributions of PAH⁰ and PAH⁺ in the total SED intensity agree with the proportions of these PAHs observed in some reflection nebulae having higher radiation intensities.     

Discriminating satellite IR anomalies associated with the MS 7.1 Yushu earthquake in China

In the process of exploring pre-earthquake thermal anomalies using satellite infrared data, Blackett et al. (2011) found that the previously reported anomalies before the 2001 Mw 7.7 Gujarat earthquake, in India, were related to positive biases caused by data gaps due to cloud cover and mosaicing of neighboring orbits of MODIS satellite data. They supposed that such effects could also be responsible for other cases. We noted a strip-shaped TIR anomaly on March 17th, 2010, 28?days before the Ms. 7.1 Yushu earthquake (Qin et al., 2011). Here we again investigate multi-year infrared satellite data in different bands to discriminate whether the anomaly is associated with the earthquake, or is only bias caused by the data gaps. From the water vapor images, we find lots of clouds that have TIR anomalies. However, on the cloudiness background, there is an obvious strip-shaped gap matching the tectonic faults almost perfectly. In particular, the animation loops of hourly water vapor images show that the cloud kept moving from west to east, while they never covered the strip-shaped gap. We consider that the cloud with this special spatial pattern should have implied the abnormal signals associated with the seismogenic process. Based on current physical models, the satellite IR anomalies both on TIR and water vapor bands can qualitatively be explained using synthetic mechanisms.     

像片数目对工业摄影测量精度影响研究

高精度工业摄影测量技术是现代工业制造的一种测量方法，在航空航天、机械制造、军事工业等领域得到了广泛的应用。提高工业摄影测量的精度则是该技术发展的重点之一，本文针对像片数目对工业摄影测量精度的影响做了研究，在控制如光照、反光标志材料、像中心点坐标精度等条件因素不变的情况下，采用固定网型一次性采集共计1200张像片，并等差随机分为17×3组不同像片数目组合，处理得出各组点三维坐标。以重复性作为精度评定标准，通过综合分析得出像片数目对工业摄影测量精度无实质性影响，为进一步研究如何提高摄影测量精度提供参考。     

一种氧杂蒽酮类海洋抗污损天然产物振动光谱的理论研究

基于 Gaussian 09W软件包,采用 DFT-B3LYP方法,研究了 1种来源于红树林未知真菌的海洋抗污损天然产物——6,8-di-O-methyl versiconol。先用 3-21G基组,再用 6-311G基组计算了分子的最稳定构型及其前线分子轨道分布。分析稳定构型发现,以蒽二酮为主体的分子是 1个三维非平面的结构,并且分子内部形成了 1个大的 π共轭体系。在最稳定构型的基础上,用同样的理论方法和 6-311G基组计算了该分子的红外振动频率及拉曼光谱频率,根据红外和拉曼光谱的振动频率特点,将红外光谱和拉曼光谱分成 3个区域,讨论了 2种光谱在各区域的特征峰的位置、振动特点、振动模式等,为氧杂蒽酮类海洋抗污损天然产物分子的振动光谱检测和分子结构的鉴定,提供了光谱解析方面的理论依据。     

高光谱图像融合最佳波段选择方法

针对高光谱图像高数据维给图像处理带来的困难和影响,本文构造了高光谱图像融合的最佳波段选择新模型-联合偏度-峰度指数(Joint Skewness-Kurtosis figure,JSKF)模型,利用JSKF指数进行自适应子空间的分解和波段选择,降低高光谱数据维数;并将选择出的最佳波段组合进行了融合,实验结果表明,该方法所选择的波段信息差异较大、互补特征明显,融合后图像包含的信息量丰富,效果优于传统的自适应波段选择方法和主成分分析累计贡献率方法.     

REM/ROSS: a powerful tool for monitoring the prompt afterglow of γ-ray bursts

Observations of the prompt afterglow of γ-ray burst events are unanimously considered of paramount importance for GRB science and cosmology. Such observations at NIR wavelengths are even more promising allowing the monitoring of high-z Ly- absorbed bursts as well as events occurring in dusty star-forming regions. In these pages we present rapid eye mount (REM), a fully robotized fast slewing telescope equipped with a high throughput NIR (Z, J, H, K) camera dedicated to detecting the prompt IR afterglow. REM can discover objects at extremely high redshift and trigger large telescopes to observe them. The REM telescope will simultaneously feed REM optical slitless spectrograph (ROSS) via a dichroic. ROSS will intensively monitor the prompt optical continuum of GRB afterglows. The synergy between the REM-IR camera and the ROSS spectrograph makes REM a powerful observing tool for any kind of fast transient phenomena. Beside its ambitious scientific goals, REM is also technically challenging since it represent the first attempt to locate a NIR camera on a small telescope providing, with ROSS, unprecedented simultaneous wavelength coverage on a telescope of this size.