Formation of the CME Leading Edge Observed in the 2003 February 18 Event

This work investigates a typical coronal mass ejection (CME) observed on 2003 February 18, by various space and ground instruments, in white light, Ha, EUV and X-ray. The Ha and EUV images indicate that the CME started with the eruption of a long filament located near the solar northwest limb. The white light coronal images show that the CME initiated with the rarefaction of a region above the solar limb and followed by the formation of a bright arcade at the boundary of the rarefying region at height 0.46 R(?) above the solar surface. The rarefying process synchronized with the slow rising phase of the eruptive filament, and the CME leading edge was observed to form as the latter started to accelerate. The lower part of the filament brightened in Ha as the filament rose to a certain height and parts of the filament was visible in the GOES X-ray images during the rise. These brightenings imply that the filament may be heated by the magnetic reconnection below the filament in the early stage of the eruption. We suggest that a possible mechanism which leads to the formation of the CME leading edge and cavity is the magnetic reconnection which takes place below the filament after the filament has reached a certain height.     

The Magnetic Field Effect on Planetary Nebulae

In our previous work on the 3-dimensional dynamical structure of planetary nebulae the effect of magnetic field was not considered. Recently Jordan et al. have directly detected magnetic fields in the central stars of some planetary nebulae. This discovery supports the hypothesis that the non-spherical shape of most planetary nebulae is caused by magnetic fields in AGB stars. In this study we focus on the role of initially weak toroidal magnetic fields embedded in a stellar wind in altering the shape of the PN. We found that magnetic pressure is probably influential on the observed shape of most PNe.     

Monitoring Secular Orbital Period Variations of Some Eclipsing Binaries at the Ankara University Observatory

This study concerns the long-term monitoring of the secular variation character in the orbital period of some short-period eclipsing binaries observed at the Ankara University Observatory. Among the systems of our observing list are CK Boo, V502 Oph and V836 Cyg that show long-term secular variations in their orbital periods. We use classical O-C diagram analysis technique as a tool to reveal the character of the period variations of these binary systems.     

SLR新星历及其在卫星预报中的应用

目前卫星激光测距(SLR)中所采用的IRV星历已经使用了近20年,近几年来随着对高轨卫星的测距和卫星白天测距的开展以及考虑到今后激光测距技术的发展,需要对SLR所采用的星历进行改进,以适应SLR发展的需求。从2006年8月起国际激光测距网(ILRS)将使用一种新的可用于多种目标测距的星历——CPF星历,该星历不仅可用于人造卫星的激光测距,而且还可用于月球及其转发器等目标的激光测距。该文介绍了这种SLR新星历和应用它进行卫星位置台站预报的情况,分析了其预报精度。     

白噪声中f~(-2)随机过程的最优估计

从功率谱的角度分析了白噪声中f-2随机过程的最优估计问题，推导了线性估计方法的精度极限，并通过对若干线性估计方法的精度进行分析和比较，得到了一些有意义的结论。     

A Study on the Recovery and Classification of Meteorites from the Mt. Grove Region of Antarctica

The Antarctic Continent has become the largest natural preservatory of meteorites in the world because of its unique geographical position and climatic conditions. Mt. Grove is located in the inland area of the Antarctic Continent where the conditions are favorable for the preservation of meteorites. During China's 15th, 16th and 19th Antarctic Scientific Explorations a large number of meteorites were recovered in the Mt. Grove region. Especially during the 19th Exploration in 2002/03 a total of 4448 meteorites were recovered, which at one stroke put China among countries that have recovered most numbers of meteorites. Here, we report mainly the results of microscope and electron microprobe studies of 28 meteorites recovered during the 16th Exploration. The meteorites are chemically classified based on their mean Fa contents of olivine, mean Fs contents of low-Ca pyroxene and abundances of Fe-Ni metal. We also give a brief account of the meteorite recovery during the three Explorations and of some preli     

Global Axisymmetric Stability Analysis for a Composite System of Two Gravitationally Coupled Scale-Free Discs

For a composite system of gravitationally coupled stellar and gaseous discs, we have carried out a linear stability analysis for axisymmetric coplanar perturbations using the two-fluid formalism. The background stellar and gaseous discs are taken to be scale-free with all physical variables varying as powers of the cylindrical radius r with compatible exponents. The unstable modes set in as neutral modes or stationary perturbation configurations with angular frequency ω=0. The axisymmetric stable range is bounded by two marginal stability curves derived from stationary perturbation configurations. Because of the gravitational coupling between the stellar and the gaseous discs, one only needs to consider the parameter regime of the stellar disc. There exist two unstable regimes in general: a collapse regime corresponding to large-scale perturbations and a ring-fragmentation regime corresponding to short-wavelength perturbations. The composite system will collapse if it rotates too slowly and will succumb to ring-fragmentation instabilities if it rotates sufficiently fast. The overall stable range against axisymmetric perturbations is determined by a necossary D-criterion involving the effective Mach number squared Ds^2 (the squared ratio of the stellar disc rotation speed to the stellar velocity dispersion up to a numerical factor). Different mass ratio δ and sound speed ratio of the gaseous and stellar disc components will alter the overall stability. For spiral galaxies or circumnuclear discs, we further include the dynamical effect of a massive dark matter halo. Astrophysical applications to disc galaxies, proto-stellar discs and circumnuclear discs are given as examples.     

巴基斯坦胡兹达尔- 拉斯贝拉铅锌成矿带遥感地质特征与找矿模型

巴基斯坦胡兹达尔- 拉斯贝拉铅锌成矿带是特提斯成矿域铅锌成矿带的重要组成部分,该成矿带的矿床类型主要为喷流- 沉积型(SEDEX)和密西西比河谷型(MVT)。目前针对胡兹达尔- 拉斯贝拉铅锌成矿带及典型矿床的研究程度较低,制约了对该成矿带的认识及找矿勘查研究。本研究以胡兹达尔- 拉斯贝拉成矿带为研究区,通过合理选择遥感数据源和图像处理方法,对典型矿床(杜达、贡尕铅锌矿床)及部分矿点的样品光谱特征、影像特征综合分析,结合关键控矿要素研究,建立了胡兹达尔- 拉斯贝拉地区与沉积岩有关铅锌矿遥感找矿标志并开展成矿预测,为该成矿带找矿提供可行性方法。基于本研究建立的找矿标志,利用增强型专题制图仪(Enhanced thematic mapper, ETM)和先进星载热辐射与反射辐射计(Advanced spaceborne thermal emission and reflection radiometer, ASTER)影像圈定主要预测含矿地层分布区30处,结果与已知矿床、矿点吻合较好,圈定的含矿地层分布区主要集中在研究区中部和北部,均位于侏罗纪地层内且矿化带与地层走向一致,矿化主要位于安吉拉组、劳瑞莱组地层内部;根据含矿地层像元光谱,利用资源一号02D高光谱影像提取了中部地区含矿地层的空间分布,提取结果与找矿标志分析结果吻合较好,证实了在该区利用国产高光谱影像开展含铅锌矿地层自动提取与找矿的可行性。     

浅析过钻头测井面临的挑战及应对策略

本文研究了时下热门的过钻头测井技术。过钻头测井技术是21世纪以来新兴的测井方式,不同于以往的电缆测井和随钻测井。过钻头测井主要是在水平井、大斜度井段实施测量,自该技术开发以来,解决了多种技术难题。同时,过钻头测井技术也暴露出各种问题,主要就体现在(1)抗温抗压性能;(2)垂向分辨率和测量精度;(3)测量项目。本文着重介绍了这三个方面的认识与看法,提出了一些解决方案,并简要叙述了过钻头测井技术的发展方向。     

ICP-AES法快速测定卤水中的硫酸根

本文建立了电感耦合等离子体发射光谱(ICP-AES)法测定卤水中硫酸根含量的方法。该方法在S 182.034 nm处的检出限为0.0324 mg/L,线性范围为0.0324 -1000 mg/L。实验研究了卤水中常见共存离子对硫酸根测定的影响情况。经国家标准物质验证,结果与标准值相符。将该方法应用于实际卤水中硫酸根的测定,方法的相对标准偏差(RSD,n=11)小于2.2 %,加标回收率为98.1 %—104.4 %。将该方法的测定值与重量法的结果进行了对比,无明显系统偏差。