Gaseous Jets in Comet Hale-Bopp (1995 O1)

We report the identification of gas jets in comet Hale-Bopp in OH, NH, CN, C₂ and C₃. This is the first time OH and NH jets without an obvious optical dust jet counterpart have been identified in narrowband comet images. We also confirm the existence of CN jets as reported by Larson et al. (1997) and Mueller et al. (1998). Jet features can be seen in the March and April 1997 datasets, approximately a month before and after perihelion. Our results contribute to the understanding of both the chemical properties of the comet as well as the physical mechanisms necessary to produce these features. This revised version was published online in July 2006 with corrections to the Cover Date.     

PRIMA for the VLTI – Science

The four main scientific objectives of PRIMA – the Phase-Referenced Imaging and Micro-arc second Astrometry facility for the VLTI – will be described:– extra-solar system characterization with astrometry, to detect planets and evaluate their mass, and imaging of the dust accretion disk,– galactic center study with astrometry(dynamics of the bulge stars) and imaging at 10μm (piercing the gas and dust clouds surrounding the galactic center),– observations of AGNs and other extra-galactic objects, too faint to be observed without PRIMA, for which partial imaging is needed to constrain their structuremodels,– micro-gravitational lensing event resolution (imaging and astrometry of their photo-center) in the Galactic Bulge and Magellanic Clouds, helping to determine directly the lens mass and distance. This revised version was published online in July 2006 with corrections to the Cover Date.     

Generalized Born inversion of seismic reflection data

Summary . Born inverse methods give accurate and stable results when the source wavelet is impulsive. However, in many practical applications (reflection seismology) an impulsive source cannot be realized and the inversion needs to be generalized to include an arbitrary source function. In this paper, we present a Born solution to the seismic inverse problem which can accommodate an arbitrary source function and give accurate and stable results. It is shown that the form of the generalized inversion algorithm reduces to a Wiener shaping ***filter, which is solved efficiently using a Levinson recursion algorithm. Numerical examples of synthetic and real field data illustrate the validity of our method.     

用卫星高光谱数据提取德兴铜矿区植被污染信息

在深入分析研究德兴铜矿矿区植被光谱特征的基础上,利用美国EO-1卫星Hyperion高光谱数据,通过反演表征植物生理状态的光谱特征参数(红边位置和最大吸收深度)变异,提取与污染相关的信息,获取了矿山植被污染生态效应概况,为矿山污染的诊断和监测提供新技术和知识支撑。     

镇江圌山绍隆禅寺“活地”成因

"活地"是宗教的传奇,而由于以往知识与技术的限制以及宗教圣地的"不可侵犯性","活地"也成了大自然的千年未解之谜。通过现场考察和资料调研,明晰了"活地"所在地区的地质构造特征。采用高频率表面波监测、分析技术,通过现场试验,研究了"活地"附近地表浅层岩土体分布情况。采用图像分析技术,经室内试验研究得出了"活地"及周围地区出露岩石的矿物组成。最终,对于"活地"的成因提出以下看法:1.否定了地下深层生长性岩脉诱发"活地"现象的观点;2.膨胀岩及膨胀土吸水膨胀对"活地"的隆升有一定作用,但这不是"活地"的主要诱因;3.提出"活地"是岩石风化作用及特殊地理环境综合作用结果的观点:风化作用使岩体疏松、体积增大,地面隆起;两侧山体运动对其交界处岩石产生挤压作用,为"活地"的持续隆升提供动力源。     

基于星座图改进的QAM盲均衡算法

针对多模辅助算法均方误差高的缺点,提出了两种基于星座图改进的盲均衡算法.首先利用16QAM星座图信息,增加多模辅助算法代价函数中信号点的均衡数目,得到改进的多模辅助算法,与多模辅助算法相比,改进后的算法稳态均方误差更低,而且收敛速度略有提高;其次将改进的多模辅助算法和判决引导算法相结合,根据均方误差调整两种算法的比例,得到的混合算法进一步降低了稳态均方误差.水声信道仿真结果表明:提出的两种算法都可以有效地降低均方误差,适用于对精度要求较高的场合.     

基于地闪数据的雷电流幅值累积频率公式探讨

利用2007年和2008年浙江省气象部门闪电定位系统的地闪监测数据,应用Matlab数学软件中的曲线拟合工具箱,以最小二乘法原理对IEEE推荐公式和我国规程推荐公式进行最优化拟合,得出前者拟合效果优于后者的结论。通过分析IEEE推荐公式计算结果与实际值之间的相对误差,发现正闪雷电流幅值累积频率在(1kA,270kA)范围内相对误差绝对值较小,最大不超过10%;而负闪雷电流幅值累积频率在(-1kA,-300kA)范围内相对误差绝对值较大,最大值约为38%。针对上述情况,利用数学软件拟合出负闪(-1kA,-300kA)相对误差曲线的近似函数,修正了原累积频率公式,大幅度减小了其相对误差。其适用范围也从原来的(2kA,200kA)放宽至正闪(1kA,270kA)、负闪(-1kA,-300kA)。     

基于ADTD系统的雷电流波头陡度频率分布特征

通过对ADTD闪电定位系统2006 2008年在重庆地区监测的729598次闪电进行统计,重点分析雷电流陡度的频率分布特征。结果表明:雷电流波头陡度及其频率随极性不同而差异较大,正闪陡度明显大于负闪陡度,而同陡度负闪频率却显著大于正闪;雷电流幅值与陡度相关系数为+0.613;采用电力行业标准DL/T620推荐波头时间反推得到的雷电流陡度和采用Ciger推荐公式计算得到的雷电流陡度的概率分布特征与统计特征差异较大。在此基础上分析了ADTD系统获取雷电流陡度资料的局限性,为合理选取雷电流陡度参数提供理论依据。     

Detection of non-radial pulsation and faint companion in the symbiotic star CH Cyg

We have detected asymmetry in the symbiotic star CH Cyg through the measurement of precision closure phase with the Integrated Optics Near-Infrared Camera (IONIC) beam combiner, at the infrared optical telescope array interferometer. The position of the asymmetry changes with time and is correlated with the phase of the 2.1-year period found in the radial velocity measurements for this star. We can model the time-dependent asymmetry either as the orbit of a low-mass companion around the M giant or as an asymmetric, 20 per cent change in brightness across the M giant. We do not detect a change in the size of the star during a 3-year monitoring period neither with respect to time nor with respect to wavelength. We find a spherical dust shell with an emission size of 2.2 ± 0.1 D _* full width at half-maximum around the M giant star. The star to dust flux ratio is estimated to be 11.63 ± 0.3. While the most likely explanation for the 20 per cent change in brightness is non-radial pulsation, we argue that a low-mass companion in close orbit could be the physical cause of the pulsation. The combined effect of pulsation and low-mass companion could explain the behaviour revealed by the radial velocity curves and the time-dependent asymmetry detected in the closure-phase data. If CH Cyg is a typical long secondary period variable then these variations could be explained by the effect of an orbiting low-mass companion on the primary star.