PSD用于零位跟踪的研究及应用

介绍了一维PSD的工作原理及特性,提出了一种利用PSD为位置传感器进行零位跟踪的方法,详细阐述了根据该方法设计的高速、高准确度的PSD信号处理电路、软件算法及其中的关键技术,有效地解决了方位角测量系统中远距离垂直传递的难题,并取得了综合角度传递误差小于±10″的测量结果。     

一种基于小波变换的SAR图像边缘检测器(英文)

边缘提取是图像处理与图像分析的基础。本文基于小波变换 ,研究了 SAR图像边缘提取的方法 ,从而为合成孔径雷达 (SAR)图像辅助导航系统奠定基础。由于 SAR图像受固有斑点噪声的影响 ,采用小波变换与固定阈值提取 SAR图像边缘特征时 ,将有大量虚假边缘产生 ,特别是在图像的亮区。为此 ,本文提出了采用具有恒定误警率的阈值 ,以消除斑点噪声的影响。同时 ,分别对两幅不同的图进行仿真 ,仿真结果表明 ,斑点噪声的影响被大大抑制 ,且由于阈值是由小波变换系数直接构成 ,能保证辅助导航对实时性的要求。     

深空探测器定位在太阳系中特殊点上的有关问题

由于某些探测任务的需要,要将空间探测器定位在日-地空间的适当 位置上,日-地系统中的5个平动点就是首选的位置。因其平动点是否稳定关 系到探测任务能否完成,如果不稳定又如何采取轨控策略是任务的关键。鉴于 这一点,本文将阐明5个平动点的动力学特征,特别是对3个不稳定的共线平动 点Li(i=1,2,3),给出相应的轨控条件,并以仿真计算结果表明,采用一定的轨 控方式,可以使探测器保持在Li附近而不远离。     

Study of a Coronal Mass Ejection with SOHO/UVCS and STEREO data

We study the 3-D kinematics of a Coronal Mass Ejection (CME) using data acquired by the LASCO C2 and UVCS instruments on board SOHO, and the COR1 coronagraphs and EUVI telescopes on board STEREO. The event, which occurred on May 20, 2007, was a partial-halo CME associated with a prominence eruption. This is the first CME studied with UVCS data that occurred in the STEREO era. The longitudinal angle between the STEREO spacecrafts was ∼7.7° at that time, and this allowed us to reconstruct via triangulation technique the 3-D trajectory of the erupting prominence observed by STEREO/EUVI. Information on the 3-D expansion of the CME provided by STEREO/COR1 data have been combined with spectroscopic observations by SOHO/UVCS. First results presented here show that line-of-sight velocities derived from spectroscopic data are not fully in agreement with those previously derived via triangulation technique, thus pointing out possible limitations of this technique.     

人工免疫木马检测中动态克隆选择算法的改进

针对人工免疫木马检测中检测器的冗余,检测过程中成熟检测器和记忆检测器在检测到自我抗原或年龄过大时,被直接删除造成的非我信息资源丢弃等问题,引入限次变异对检测器的生成进行改进,提出将随机生成的检测器在自我耐受后,再与已有合格检测器匹配,对与已有合格检测器匹配的检测器进行限次变异;而检测到自我抗原或年龄过大的检测器同样进行限次变异的方法。实验结果表明,这种方法能准确而快速地检测已知和未知木马。     

Optimum detection and location estimation of target lines in the range-time space of a search radar

The average likelihood ratio detector is derived as the optimum detector for detecting a target line with unknown normal parameters in the range-time data space of a search radar, which is corrupted by Gaussian noise. The receiver operation characteristics of this optimum detector is derived to evaluate its performance improvement in comparison with the Hough detector, which uses the return signal of several successive scans to achieve a non-coherent integration improvement and get a better performance than the conventional detector. This comparison, which is done through analytic derivations and also through simulation results, shows that the average likelihood ratio detector has a better performance for different SNR values. This result is justified by showing the disadvantages of the Hough method, which are eliminated by the optimum detector. To have an estimate for the location of the detected target line in the optimum detection method as the Hough method, which detects and localizes the target lines simultaneously, we present the maximum a posteriori probability estimator. The estimation performance of the two methods is then compared and it is shown that the maximum a posteriori probability estimator localizes the detected target lines with a better performance in comparison with the Hough method.     

Photo-alteration of hydantoins against UV light and its relevance to prebiotic chemistry

Aqueous solutions of 5-substituted hydantoins were irradiated with ultraviolet (UV) light, to investigate their structural stability against UV radiation as well as the possible photolysis products. The photolysis products were identified and the degree of photolysis was measured using reversed-phase and ion-exchange high-performance liquid chromatography. Hydantoin (2,4-imidazolidinedione) was dominantly detected as a photolysis product of 5-substituted hydantoins. With hydrolysis of UV-irradiated 5-substituted hydantoins, glycine and alanine were dominantly detected. These experimental results are important for the prebiotic photochemistry of 5-substituted hydantoins in the formation of hydantoin since they have been detected in Solar System materials.     

UV disinfection system for cabin air

The air of indoor cabin environments is susceptible to contamination by airborne microbial pathogens. A number of air treatment processes are available for inactivation or removal of airborne pathogens; included among these processes is ultraviolet (UV) irradiation. The effectiveness of UV-based processes is known to be determined by the combined effects of UV dose delivery by the reactor and the UV dose–response behavior of the target microbe(s). To date, most UV system designs for air treatment have been based on empirical approaches, often involving crude representations of dose delivery and dose–response behavior. The objective of this research was to illustrate the development of a UV system for disinfection of cabin air based on well-defined methods of reactor and reaction characterization.     

Observed redshifts of transition region/corona lines

Solar UV observations reveal a redshifted emission at transition region temperatures, commonly interpreted as a net downflow of plasma. In earlier investigations the magnitude of the redshift has been found to increase with temperature, reaching a maximum at T=10⁵ K, and then to decrease towards higher temperatures. These observations, mostly from Skylab, suggested no significant shift of the O V line at 1218 Å formed at 2.4×10⁵ K. The variation of the downflow velocity with temperature is, however, uncertain since there are few reliable observations of lines formed at higher temperatures.Using spectrograms from the High Resolution Telescope and Spectrograph — HRTS we find an average net redshift of the O V lines at 1218 Å and 1371 Å at all locations extending from disk center to solar limb. A discrepancy between the observed flow velocity in the two lines is probably caused by uncertainty in the available laboratory wavelength of the intercombination line at 1218 Å (2s^{2 1}S₀-2s2p³P₁).The observed shift in O V is compared with corresponding measurements of lines formed at other temperatures (Si IV, C IV, N IV, O IV, and Fe XII). Large variations in the shift are found along the instrument slit. Thus, blueshifts are also observed with the sites of the largest upflow located in the sunspot umbrae and in a quiet region close to an active region.     

Understanding solar streamers: The role of SOHO

Streamers have been observed since far back in time, but our knowledge of their morphology and of their physical characteristics is still very limited. As a consequence, the present streamer picture is largely incomplete: because individual features are poorly known, their role in more general phenomena (like the evolution of the global corona or the solar wind mass and flow pattern) is also poorly known. In this presentation, the more relevant open problems in the understanding of streamers will be illustrated and it will be shown how new data acquired by SOHO may help us to reach a better understanding of these structures.