用1：5万磁异常特征圈定贵州水城-艾家坪地区成矿靶区

对1：5万高精度磁异常原始资料数据处理,进行化极、延拓计算7个不同上延高度异常,分析对比所有资料,结合地物化资料,对磁异常平面进行特征分区。又根据已知的白马洞（区内）-杉树林（区外）铅锌矿床成矿带及区内异处的铅锌、铜、锰等矿床（点）的成矿规律和分布特点,圈定了8个异常成矿靶区,19个大型的浅层局部负磁异常,均为有一定找矿意义的磁异常,并推测它们可能为岩体与矿致磁异常（铅锌、铜、锰、铁）等综合引起,在岩体（浅表隐伏的花岗岩珠或岩枝）与围岩接触带、层间破碎带上,应是赋矿的有利部位。     

地面高精度磁测数据在区域地质填图中应用研究

在前人工作的基础上提出了“多频段的磁异常”的概念.并通过对目前流行的一些滤波方法进行比较,提出使用小波滤波和插值切割法滤波分频的工作思路.探讨了分频段磁异常与地质岩性的关系.认为：①分频以后信息量成倍地增加,读到了许多原始数据（包括常规数据处理）无法读到的信息;②分频提出的信息,不同频率有着不同宏观特征;③不是一种岩性只相关一种频率段异常;④原始数据的结构特点对分频结果起决定性作用;⑤分频有4~5个频段就可以得到许多新的信息;⑥同常规磁异常解释一样,信息提取以后的人工分析是异常解释中非常值得关注的一环;⑦利用插值切割分频的原则是,切割次数是起圆滑作用的因子,因子的大小取决于原始数据的干扰水平（圆滑水平）;⑧分频磁异常可以区分不同的岩性.     

太行山红层磁学性质及古环境意义初探

环境磁学研究磁性矿物特征（磁性矿物类型、含量和颗粒大小）及其转化与环境关系,在不同地质时期古气候和古环境重建中得到广泛应用。本文将磁学方法应用于太行山中元古界红层研究,并从其磁学性质角度初步探讨太行山红层的古环境。对太行山红色石英砂岩和紫红色砂质泥岩样品进行了高温磁学和常温磁学系统测试。结果显示,太行山红层主要以硬磁性的赤铁矿为主,包含少量磁铁矿,部分样品赤铁矿是唯一磁性矿物;磁性颗粒大小以单畴为主;红色石英砂岩不同样品间磁性差别显著,反映沉积环境的不稳定性。紫红色砂质泥岩中的青灰色层表现为顺磁性特征,原因可能是紫红色砂质泥岩中的赤铁矿在后期还原环境下溶解或转化为弱磁性矿物所致,说明紫红色层并非形成于长期的水下还原环境。太行山红层中普遍存在的红色波痕和泥裂说明水环境对其有短暂影响,但是红层及赤铁矿的富集说明其长时间处于氧化环境,推断太行山红层可能形成于高度氧化的陆地环境。     

关于"太阳线性无力场评注和快速傅氏分析法的应用"的评论

“太阳线性无力场评注和快速傅氏分析法的应用”一文对太阳线性无力场的工作做了一些评注,在此基础上对快速傅立叶方法的应用提出了改进的计算方法．该文的某些观点值得商榷,有必要对其中存在的问题予以澄清．另外,对该文关于快速傅氏分析法的工作从理论的角度提出看法．     

3. Solar System Formation and Early Evolution: the First 100 Million Years

The solar system, as we know it today, is about 4.5 billion years old. It is widely believed that it was essentially completed 100 million years after the formation of the Sun, which itself took less than 1 million years, although the exact chronology remains highly uncertain. For instance: which, of the giant planets or the terrestrial planets, formed first, and how? How did they acquire their mass? What was the early evolution of the “primitive solar nebula” (solar nebula for short)? What is its relation with the circumstellar disks that are ubiquitous around young low-mass stars today? Is it possible to define a “time zero” (t ₀), the epoch of the formation of the solar system? Is the solar system exceptional or common? This astronomical chapter focuses on the early stages, which determine in large part the subsequent evolution of the proto-solar system. This evolution is logarithmic, being very fast initially, then gradually slowing down. The chapter is thus divided in three parts: (1) The first million years: the stellar era. The dominant phase is the formation of the Sun in a stellar cluster, via accretion of material from a circumstellar disk, itself fed by a progressively vanishing circumstellar envelope. (2) The first 10 million years: the disk era. The dominant phase is the evolution and progressive disappearance of circumstellar disks around evolved young stars; planets will start to form at this stage. Important constraints on the solar nebula and on planet formation are drawn from the most primitive objects in the solar system, i.e., meteorites. (3) The first 100 million years: the “telluric” era. This phase is dominated by terrestrial (rocky) planet formation and differentiation, and the appearance of oceans and atmospheres.     

解决太阳横向磁场方向测定中180°不确定性的一个方法

本文提出了一种解决太阳横向磁场方向测定中１８０°不确定性的方法。该方法首先将Ｇａｒｙ等提出的方法定量化，客观地确定每一点的横场方向；然后由独立的Ｈ＿α观测或磁场演化历史，分析和确定磁力线的拓扑联接性，对客观确定的横场方向做经验修正。对活动区的应用表明，该方法是一个可供选择的解决横场方向不确定性的有效方法。     

An interpretation of the variations of the magnetic core-mantle coupling torques and the core drift rate

The influence of recently computed axial magnetic core-mantle coupling torques on the Earth's rotation was investigated. These torques derived from poloidal geomagnetic field within the mantle and at the core-mantle boundary are retarding torques. An accelerating torque due to the action of unknown parts of the core field was estimated by inverse solution of the equation of the mantle rotation for the periodic variations of the quantities of the magnetic field and the length of day. The variations of the drift rate of the Earth's core were compared with those of the mantle rotation velocity for a force-free Earth. The time constants of the coupling process were estimated and discussed in connection with the magnetic coupling of the mantle with an upper core layer. Der Einfluß kürzlich berechneter axialer Kern-Mantel-Kopplungsmomente auf die Erdrotation wurde untersucht. Diese Lorentz-Drehmomente, abgeleitet vom poloidalen geomagnetischen Feld im Mantel und an der Kern-Mantel-Grenze, sind retardierende Momente. Ein beschleunigendes Drehmoment, das der Wirkung unbekannter Feldanteile zugeordnet wird, wurde durch inverse Lösung der Mantelrotationsgleichung für die periodischen Variationen der Magnetfeldgrößen und der Tageslänge abgeschätzt. Die Variationen der Kerndriftgeschwindigkeit wurden mit denen der Mantelrotationsgeschwindigkeit für eine kräftefreie Erde verglichen. Die Zeitkonstanten des Kopplungsprozesses wurden ermittelt und im Zusammenhang mit der magnetischen Kopplung des Mantels mit einer oberen Kernschicht diskutiert.     

Determination of dust properties and magnetic fields from polarimetric and photometric observations of stars (Review)

Verschiedene Modelle zur Darstellung der interstellaren Extinktion und Polarisation werden betrachtet. Dabei wird den Ausrichtungsmechanismen, wie dem Davies-Greenstein-Mechanismus und der Ausrichtung durch suprathermische Rotation, und ihren Näherungen besondere Aufmerksamkeit zu teil. Es wird geschlußfolgert, daß die Größe der Staubteilchen sowie die Starke und Richtung des interstellaren Magnetfeldes aus den Extinktions- und Polarisationsdaten abgeschätzt werden können. Die Anwendung der theoretischen Ergebnisse auf Sterne in der galaktischen Ebene wird erörtert.     

Geo-effectiveness of solar wind extremes

Examples of extreme events of solar wind and their effect on geomagnetic conditions are discussed here. It is found that there are two regimes of high speed solar wind streams with a threshold of ∼ 850 km s^-1. Geomagnetic activity enhancement rate (GAER) is defined as an average increase in Ap value per unit average increase in the peak solar wind velocity (Vp) during the stream. GAER was found to be different in the two regimes of high speed streams with +ve and-ve IMF. GAER is 0.73 and 0.53 for solar wind streams with +ve and -ve IMF respectively for the extremely high speed streams (< 850 km s^-1). This indicates that streams above the threshold speed with +ve IMF are 1.4 times more effective in enhancing geomagnetic activity than those with -ve IMF. However, the high speed streams below the threshold with -ve IMF are 1.1 times more effective in enhancing geomagnetic activity than those with +ve IMF. The violent solar activity period (October–November 2003) of cycle 23 presents a very special case during which many severe and strong effects were seen in the environment of the Earth and other planets; however, the z-component of IMF (Bz) is mostly positive during this period. The most severe geomagnetic storm of this cycle occurred when Bz was positive.