Planetary nebulae

A comprehensive review of the contemporary status of the problem of planetary nebulae is presented. The characteristics of their galactic distribution, their evolution and their cosmogony are emphasised. Though the review is based on all available information on the planetary nebulae and their nuclei, the literature cited in detail covers those papers published in the years 1982–1987.     

行动研究在公共英语教师科研实践中的应用

行动研究是一种将行动和研究恰当融合在一起的范式研究,它强调研究者即行动者,可以促使研究者科学而理性地研究工作中遇到的问题,从而达到解决实际问题的根本目的。公共英语教师的科研实践能力是大学英语教学改革和教学质量提高的源泉。科学、有效地在教学中进行行动研究,必然会帮助公共英语教师在完成繁重教学任务的同时实现自身科研实践能力的提升。     

粘弹性结构振动特性分析的摄动求解技术

 本文根据粘弹性结构的特点,对其振动特性进行简化分析,构造了这类结构振动特性分析的摄动求解方法,给出了低阶摄动求解公式。还讨论了零阶摄动有重特征值时的求解。     

Comparative geology of the satellites of the giant planets

The geologic evolution of the Jovian and Saturnian satellites is reviewed with regard to the major discoveries of the Voyager 1 and 2 encounters with Jupiter and Saturn.Nearly forty satellites are now identified in the Jovian and Saturnian systems. Three of these satellites (Ganymede, Titan, and Callisto) are larger than Mercury, two (Io and Europa) have sizes similar to the Moon, and four others (Rhea, Iapetus, Dione, and Tethys) are larger than the largest asteroids.They all have experienced different geologic evolutions related to their composition, and to their location in the two systems. The emphasis is given upon the cratering record of their surfaces, and on their thermal evolution, with regard to the tidal effects produced by the giant planets. The small satellites are also presented with no attempt to review their geologic record since they are almost only known from their orbital properties.     

自发汗冷却材料的研究现状

对自发汗冷却材料的种类及特点进行了简介,综述了自发汗冷却材料的几种主要制备方法及其优缺点,详细阐述了自发汗冷却材料的研究现状、影响因素及其应用,并对其发展方向进行了讨论.     

具有弹性环的有限大弹性板应力场分析

 本文用解析与数值结合法研究在含有椭圆孔的有限大小弹性板上,有一椭圆弹性环加强时,板及环上的应力场。假设板与环间处于无初应力的紧密接触状态,弹性板和弹性环的应力函数都可按复劳伦级数展开。根据孔与环的接触边界条件以及各自的外边界条件,运用节点配置法确定板、环的级数系数,从而求出板、环上的应力场。文中分析了级数项数一配点数对计算结果的影响。     

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.     

Geomagnetic Jerks: Rapid Core Field Variations and Core Dynamics

The secular variation of the core field is generally characterized by smooth variations, sometimes interrupted by abrupt changes, named geomagnetic jerks. The origin of these events, observed and investigated for over three decades, is still not fully understood. Many fundamental features of geomagnetic jerks have been the subject of debate, including their origin internal or external to the Earth, their occurrence dates, their duration and their global or regional character. Specific tools have been developed to detect them in geomagnetic field or secular variation time series. Recently, their investigation has been advanced by the availability of a decade of high-quality satellite measurements. Moreover, advances in the modelling of the core field and its variations have brought new perspectives on the fluid motion at the top of the core, and opened new avenues in our search for the origin of geomagnetic jerks. Correlations have been proposed between geomagnetic jerks and some other geophysical observables, indicating the substantial interest in this topic in our scientific community. This paper summarizes the recent advances in our understanding and interpretation of geomagnetic jerks.     

高校音乐教学中学生乐感的培养

通过文献资料研究方法,对如何培养普通高校音乐教学中大学生的乐感进行探讨分析。在教学实践中学生乐感的培养,主要是通过提升学生的音乐欣赏能力,鉴赏水平,以及听唱练习等方法,发展学生的思维想象能力,提高学生的音乐感受能力和音乐理解水平,培养学生高尚的音乐情操以及对音乐的感知能力。音乐素养的提升是培养大学生音乐感知能力的有效途径和手段,大学生只有不断提升自己的素养,才能深刻、全面、准确的建立自己的音乐感知能力。     

流动阻力及能量损失对注射成型制件的影响

本文分析了在塑料熔体充满型腔的过程中，流动阻力及能量损失产生的形式和物理原因，进而讨论了对塑料制件成型及凝固过程中的影响。并提出降低影响的措施。     

Metal Enrichment Processes

There are many processes that can transport gas from the galaxies to their environment and enrich the environment in this way with metals. These metal enrichment processes have a large influence on the evolution of both the galaxies and their environment. Various processes can contribute to the gas transfer: ram-pressure stripping, galactic winds, AGN outflows, galaxy-galaxy interactions and others. We review their observational evidence, corresponding simulations, their efficiencies, and their time scales as far as they are known to date. It seems that all processes can contribute to the enrichment. There is not a single process that always dominates the enrichment, because the efficiencies of the processes vary strongly with galaxy and environmental properties.     

Solar magnetic fields

This paper is a review of our observational knowledge on solar magnetic fields. In Section 1 we make an attempt to summarize all observations of the general magnetic field (m.f.) of the Sun. Section 2 deals with the local m.f. at low latitudes and their connection with some features on the disk. The m.f. of sunspots and their peculiar character are considered in Section 3. The last section (4) is concerned with m.f. in sunspot groups, their changes and connections with solar activity.     

电流/频率转换类型综述

在惯性仪表输出电路中,常用的模/数转换方案是电流/频率转换方案,本文根据反馈脉冲电流的特点将电流/频率转换的几种类型进行分类,并对其中几种转换类型的工作特点、基本电路组成、工作波形做了介绍,同时进行了仿真分析比较。有助于根据惯性仪表的数字化输出系统设计要求选择合适的转换类型。     

女性的成长与困惑 --论玛格丽特·阿特伍德小说中女性成长主题

女性成长主题是贯穿阿特伍德小说的一条主线.从女性主义视角,分析了作家在其不同作品中塑造的典型的女性人物形象以及她们在各自成长过程中所经历的种种困惑与挣扎;探讨了女性为了在男性主宰的社会中寻求自我、寻求生存空间而面临的不同矛盾冲突及矛盾的解决方式.进而研究了作家是如何在其小说创作中使这一主题逐渐凸现.     

From Disks to Planets: The Making of Planets and Their Early Atmospheres. An Introduction

This paper is an introduction to volume 56 of the Space Science Series of ISSI, “From disks to planets—the making of planets and their proto-atmospheres”, a key subject in our quest for the origins and evolutionary paths of planets, and for the causes of their diversity. Indeed, as exoplanet discoveries progressively accumulated and their characterization made spectacular progress, it became evident that the diversity of observed exoplanets can in no way be reduced to the two classes of planets that we are used to identify in the solar system, namely terrestrial planets and gas or ice giants: the exoplanet reality is just much broader. This fact is no doubt the result of the exceptional diversity of the evolutionary paths linking planetary systems as a whole as well as individual exoplanets and their proto-atmospheres to their parent circumstellar disks: this diversity and its causes are exactly what this paper explores. For each of the main phases of the formation and evolution of planetary systems and of individual planets, we summarize what we believe we understand and what are the important open questions needing further in-depth examination, and offer some suggestions on ways towards solutions.We start with the formation mechanisms of circumstellar disks, with their gas and disk components in which chemical composition plays a very important role in planet formation. We summarize how dust accretion within the disk generates planet cores, while gas accretion on these cores can lead to the diversity of their fluid envelopes. The temporal evolution of the parent disk itself, and its final dissipation, put strong constraints on how and how far planetary formation can proceed. The radiation output of the central star also plays an important role in this whole story. This early phase of planet evolution, from disk formation to dissipation, is characterized by a co-evolution of the disk and its daughter planets. During this co-evolution, planets and their protoatmospheres not only grow, but they also migrate radially as a result of their interaction with the disk, thus moving progressively from their distance of formation to their final location. The formation of planetary fluid envelopes (proto-atmospheres and oceans), is an essential product of this planet formation scenario which strongly constrains their possible evolution towards habitability. We discuss the effects of the initial conditions in the disk, of the location, size and mass of the planetary core, of the disk lifetime and of the radiation output and activity of the central star, on the formation of these envelopes and on their relative extensions with respect to the planet core. Overall, a fraction of the planets retain the primary proto-atmosphere they initially accreted from the gas disk. For those which lose it in this early evolution, outgassing of volatiles from the planetary core and mantle, together with some contributions of volatiles from colliding bodies, give them a chance to form a “secondary” atmosphere, like that of our own Earth.When the disk finally dissipates, usually before 10 Million years of age, it leaves us with the combination of a planetary system and a debris disk, each with a specific radial distribution with respect to their parent star(s). Whereas the dynamics of protoplanetary disks is dominated by gas-solid dynamical coupling, debris disks are dominated by gravitational dynamics acting on diverse families of planetesimals. Solid-body collisions between them and giant impacts on young planetary surfaces generate a new population of gas and dust in those disks. Synergies between solar system and exoplanet studies are particularly fruitful and need to be stimulated even more, because they give access to different and complementary components of debris disks: whereas the different families of planetesimals can be extensively studied in the solar system, they remain unobserved in exoplanet systems. But, in those systems, long-wavelength telescopic observations of dust provide a wealth of indirect information about the unobserved population of planetesimals. Promising progress is being currently made to observe the gas component as well, using millimetre and sub-millimetre giant radio interferometers.Within planetary systems themselves, individual planets are the assembly of a solid body and a fluid envelope, including their planetary atmosphere when there is one. Their characteristics range from terrestrial planets through sub-Neptunes and Neptunes and to gas giants, each type covering most of the orbital distances probed by present-day techniques. With the continuous progress in detection and characterization techniques and the advent of major providers of new data like the Kepler mission, the architecture of these planetary systems can be studied more and more accurately in a statistically meaningful sense and compared to the one of our own solar system, which does not appear to be an exceptional case. Finally, our understanding of exoplanets atmospheres has made spectacular advances recently using the occultation spectroscopy techniques implemented on the currently operating space and ground-based observing facilities.The powerful new observing facilities planned for the near and more distant future will make it possible to address many of the most challenging current questions of the science of exoplanets and their systems. There is little doubt that, using this new generation of facilities, we will be able to reconstruct more and more accurately the complex evolutionary paths which link stellar genesis to the possible emergence of habitable worlds.     

Origins of Cometary Materials

In this introductory presentation, material is categorized according to our state of knowledge: What do we know, what do we think we know but don’t know certainly, and what do we not know but often describe it as if it were a well-established fact about comets, their nuclei, their composition, and processes within comets and their nuclei. The material is presented not with the intend to criticize laboratory work simulating condition in comet nuclei, or observers analyzing their observations, nor modelers using data from both these sources to improve our understanding and make predictions. The intent is to provoke discussion and dialog between these groups to avoid overstating the results. What is a Comet? A comet is a diffuse appearing celestial phenomenon moving in an orbit about the Sun. The central body, the nucleus, is composed of ice and dust. It is the source of all cometary activity, including comae and tails. We distinguish between molecular (including atoms and ions) and dust comae. At heliocentric distances of about 1 AU and less, the hydrogen coma typically has dimensions larger than the Sun. The tails are composed of dust, neutral atoms and molecules, and plasma.     

毛泽东、邓小平外交思想的比较研究

中华人民共和国成立以来．毛泽东、邓小平两代领导人在外交上如何走中国自己的发展道路方面，都做过可贵的探索．并取得了辉煌的成就．但由于他们所处的国际形势不同．他们的外交思想既有相同之处．又有不同之处。认识两者的联系和区别为我们应付复杂的国际形势．维护世界和平．推动现代化进程有着重要的指导意义。     

轴对称弯道流动的N—S方程数值解

利用涡量—流函数方法求解离心压气机进气弯道中的轴对称粘性流场。本文推导出了q—τ湍流模型方程在正交曲线坐标系下的表达式,并用以预测湍流流场。文中在涡量方程及q—τ方程中引进非定常项,采用时间推进法求解。通过对二维直通道及复杂边界的轴对称弯道内的层流、湍流流动的计算,获得了令人满意的结果。