广东2005年“3·22”强飑线天气过程分析

利用地面常规及自动气象站观测、NCEP/NCAR 1°×1°再分析资料和多普勒雷达探测等资料, 对2005年3月22日广东一次近年罕见的强飑线过程进行了天气动力学和中尺度的诊断分析, 对伴随飑线的强风暴区天气系统配置、空间结构特征及其演变特征等作了深入的探讨, 同时计算了强对流天气发生区域的有关物理量, 从中发现了一些有意义的事实, 以求为以后广东春季强对流天气的监测和预警提供一些有益的帮助。     

2006年1月漯河市暴雪天气过程的诊断分析

利用常规探空和地面资料以及NCEP再分析资料,对2006年1月漯河暴雪过程进行了诊断分析,结果表明:高空阶梯槽的形成和维持,为这次强降雪过程提供了有利的环流背景,中低空低涡切变线是主要影响系统;冷平流的持续使近地面层气温降至0℃以下,有利于雪的形态维持;高层辐散与低层辐合的耦合,使上升运动加强;低空急流输送了充沛的水汽,大气中水汽处于饱和状态有利于提高降水的转化率。     

论线路横断面的测设方法

论述了从直线段到曲线段(缓和曲线和圆曲线)利用全站仪自由设站法测设线路横断面的原理,介绍了利用全站仪测设线路横断面的方法及步骤,实现了线路横断面测设的快速进行,为一体化作业打下了基础.     

基于小波分析的线状要素压缩优化的综合性研究

利用小波分析理论、Douglas算法、曲率分析算法，对线状要素的压缩优化进行了深入的研究，并在建立线状要素压缩优化的自适应模型的基础上，对实际数据进行了试验。结果表明，此方法不仅能够保持高的压缩比，而且能够很好地保持原数据的特征。     

2004年9月川渝大暴雨期间西南低涡结构及其环境场的分析

采用NCEP再分析资料、常规观测资料、卫星云图资料及地面降水资料, 对2004年9月2日～8日发生在川东和重庆的大暴雨的影响系统及其环境场作了分析研究。结果表明, 此次暴雨分为三个阶段, 降水系统主要有两个:第一、三阶段的主要降水系统是低空切变线；第二阶段的主要降水系统是西南低涡, 而西南低涡影响期内的雨量最强、范围最大。西南低涡开始时为一β中尺度系统, 最后发展达α中尺度系统。其影响时间从4日00时到6日06时 (国际协调时）, 持续了54小时。本文对此次暴雨过程所做的研究表明, 川东地区的特殊地形, 500 hPa高空小槽以及700 hPa、 850 hPa低层鞍型流场均是西南低涡产生和维持的重要条件； 西南低涡上层为暖性结构； 在暴雨过程中有20个雨团接连发生, 中尺度系统是这次暴雨的直接影响系统；对水汽收支的计算表明, 水汽可能来自于低纬度热带地区。本文还对西南低涡与东北低涡的异同作了比较。     

Reprocessed emission line profiles from dense clouds in geometrically thick accretion engines

The central engines of active galactic nuclei (AGN) contain cold, dense material as well as hot X-ray-emitting gas. The standard paradigm for the engine geometry is a cold thin disc sandwiched between hot X-ray coronae. Strong support for this geometry in Seyferts comes from the study of fluorescent iron line profiles, although the evidence is not ubiquitously airtight. The thin disc model of line profiles in AGN and in X-ray binaries should still be benchmarked against other plausible possibilities. One proposed alternative is an engine consisting of dense clouds embedded in an optically thin, geometrically thick X-ray-emitting engine. This model is also motivated by studies of geometrically thick engines such as advection-dominated accretion flows (ADAFs). Here we compute the reprocessed iron line profiles from dense clouds embedded in geometrically thick, optically thin X-ray-emitting discs near a Schwarzschild black hole. We consider a range of cloud distributions and disc solutions, including ADAFs, pure radial infall and bipolar outflows. We find that such models can reproduce line profiles similar to those from geometrically thin, optically thick discs and might help alleviate some of the problems encountered from the latter. Thus, independent of thin discs, thick disc engines can also exhibit iron line profiles if embedded dense clouds can survive long enough to reprocess radiation.     

Short-period line profile variations in the Be star ε Cap

We present new high-dispersion spectroscopic data for the Be star ε Cap. The purpose of these data is to study the short-period line profile variations. By using a two-dimensional period-finding technique, we confirm that the photometric period of 0.99 d is present in the helium line profiles. We show that the variations are not easily explained by non-radial pulsation and suggest that corotating circumstellar material is responsible.     

Monitoring Changes of Ice Streams Using Time Series of Satellite-Altimetry-Based Digital Terrain Models

The Antarctic Ice Sheet plays a major role in the global system, and the large ice streams discharging into the circumpolar sea represent its gateways to the world's oceans. Satellite radar altimeter data provide an opportunity for mapping surface elevation at kilometer-resolution with meter-accuracy. Geostatistical methods have been developed for the analysis of these data. Applications to Seasat data and data from the Geosat Exact Repeat Mission indicate that the grounding line of Lambert Glacier/Amery Ice Shelf, the largest ice stream in East Antarctica, has advanced 10–12 km between 1978 and 1987–89. The objectives of this paper are to explore possibilities and limitations of satellite-altimetry-based mapping to capture changes for shorter time windows and for smaller areas, and to investigate some methodological aspects of the data analysis. We establish that one season of radar altimeter data is sufficient for constructing a map. This allows study of interannual variation and is the key for a time-series analysis approach to study changes in ice streams. Maps of the lower Lambert Glacier and the entire Amery Ice Shelf are presented for austral winters 1978, 1987, 1988, and 1989. As a first step toward understanding the dynamics of the ice-stream/ice-shelf system, elevation changes are calculated for grounded ice, the grounding zone, and floating ice. In the absence of (sufficient) surface gravity control for the Lambert Glacier/Amery Ice Shelf area, altimetry-based maps may facilitate improvement of geoid models as they provide constraints on the terrain correction in the inverse gravimetric problem.     

Carbon recombination lines from the Galactic plane at 34.5 & 328 MHz

We present the results of a search for carbon recombination lines in the Galaxy at 34.5 MHz (C575α) made using the dipole array at Gauribidanur near Bangalore. Observations made towards 32 directions resulted in detections of lines, in absorption at nine positions. Followup observations at 328 MHz (C272α) using the Ooty Radio Telescope detected these lines in emission. A VLA D-array observation of one of the positions at 330 MHz yielded no detection implying a lower limit of 10′ for the angular size of the line forming region. The longitude-velocity distribution of the observed carbon lines indicate that the line forming regions are located mainly between 4 kpc and 7 kpc from the Galactic centre. Combining our results with published carbon recombination line data near 76 MHz (Erickson, McConnell & Anantharamaiah 1995), we obtain constraintson the physical parameters of the line forming regions. We find thatif the angular size of the line forming regions is ≥ 4°, then the range of parameters that fit the data are:T _e =20–40 K,n _e ∼ 0.1–0.3 cm⁻³ and pathlengths ∼ 0.07–0.9 pc which may correspond to thin photodissociated regions around molecular clouds. On the other hand, if the line forming regions are ∼ 2° in extent, then warmer gas (T _e ∼ 60–300 K) with lower electron densities (n _e ∼ 0.03–0.05 cm⁻³) extending over several tens of parsecs along the line of sight and possibly associated with atomic HI gas can fit the data. Based on the range of derived parameters, we suggest that the carbon line regions are most likely associated with photo-dissociation regions.     

Spectrophotometric observations of a peculiar nitrogen-rich planetary nebula NGC 2440

By using the Boller and Chivens spectrograph with a moderate dispersion (59 å mm^-1) in the red spectral region, we obtained 65 spectra covering the whole surface of the planetary nebula NGC 2440. Intensities of Hα, [N II] λλ 6548–6584 and [S II] λλ 6717–6731 lines are derived using the IDS system available at the ESO in La Silva (Chile). The nebula is known to be a nitrogen-rich nebula (Peimbert 1978) surrounded by secondary structures (Minkowski 1964). The unusual high value of the [N II]/Hα in the central core (~ 30) is certainly due to the nitrogen overabundance occurring in that part of the nebula. Its variations from scale ionization structure (Capriotti, Cromwell and Williams 1971). The observations show clearly an outward increase of both [NII]/Hα andI(6717)/I(6713) ratios.