ATM: general description of the processes and influencing factors

The purpose of this article is to provide the reader with a broad understanding of the Air Traffic Management system and of the various interconnecting issues involved. Such understanding of what is the ATM system, its purpose, processes and influencing factors is, indeed, essential if we want to analyse the problems of today and the type of solutions that will need to be developed and implemented today and in the future to meet the challenges of a safe and efficient handling of air traffic in the European sky.     

Large Scale Flows in the Solar Convection Zone

We discuss the current theoretical understanding of the large scale flows observed in the solar convection zone, namely the differential rotation and meridional circulation. Based on multi-D numerical simulations we describe which physical processes are at the origin of these large scale flows, how they are maintained and what sets their unique profiles. We also discuss how dynamo generated magnetic field may influence such a delicate dynamical balance and lead to a temporal modulation of the amplitude and profiles of the solar large scale flows.     

Observational Signatures of Particle Acceleration in Supernova Remnants

We evaluate the current status of supernova remnants as the sources of Galactic cosmic rays. We summarize observations of supernova remnants, covering the whole electromagnetic spectrum and describe what these observations tell us about the acceleration processes by high Mach number shock fronts. We discuss the shock modification by cosmic rays, the shape and maximum energy of the cosmic-ray spectrum and the total energy budget of cosmic rays in and surrounding supernova remnants. Additionally, we discuss problems with supernova remnants as main sources of Galactic cosmic rays, as well as alternative sources.     

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.     

Ion Acceleration and Outflow from Mars and Venus: An Overview

Solar wind forcing of Mars and Venus results in outflow and escape of ionospheric ions. Observations show that the replenishment of ionospheric ions starts in the dayside at low altitudes (??300?C800 km), ions moving at a low velocity (5?C10 km/s) in the direction of the external/ magnetosheath flow. At high altitudes, in the inner magnetosheath and in the central tail, ions may be accelerated up to keV energies. However, the dominating energization and outflow process, applicable for the inner magnetosphere of Mars and Venus, leads to outflow at energies ??5?C20 eV. The aim of this overview is to analyze ion acceleration processes associated with the outflow and escape of ionospheric ions from Mars and Venus. Qualitatively, ion acceleration may be divided in two categories:

1. Modest ion acceleration, leading to bulk outflow and/or return flow (circulation).
2. Acceleration to well over escape velocity, up into the keV range.

In the first category we find a processes denoted ??planetary wind??, the result of e.g. ambipolar diffusion, wave enhanced planetary wind, and mass-loaded ion pickup. In the second category we find ion pickup, current sheet acceleration, wave acceleration, and parallel electric fields, the latter above Martian crustal magnetic field regions. Both categories involve mass loading. Highly mass-loaded ion energization may lead to a low-velocity bulk flow??A consequence of energy and momentum conservation. It is therefore not self-evident what group, or what processes are connected with the low-energy outflow of ionospheric ions from Mars. Experimental and theoretical findings on ionospheric ion acceleration and outflow from Mars and Venus are discussed in this report.     

Exo-Astrobiological Aspects of Europa and Titan: From Observations to Speculations

By extrapolating what we know on the origins of life on Earth, and in particular on the chemical processes which gave rise to the first living system, Europa and Titan appear as two major targets for studies of exo/astrobiology in the outer solar system. With the likely presence of water oceans relatively close to its surface, coupled to possible sources of organics, the emergence and sustaining of life on Europa seems possible. On Titan, it cannot be ruled out. But the main exobiological interest of the largest satellite of Saturn is the presence of a complex organic chemistry which shows many similarities with the prebiotic chemistry which allowed the emergence of life on Earth.     

The Charging of Planetary Rings

This chapter will review what is known about the charging of planetary rings, in particular the sum of the individual currents from the time-varying charge dQ/dt, of the planetary ring particle. For the smallest ring particles, in addition to checking the plasma conditions for the charging currents, one must consider if collective effects in the ring environment are relevant. Two planetary ring environments that have held a strong interest for ring scientists in the last two decades are Saturn’s spokes in the B Ring and the environment of Saturn’s E ring. Two sections of this chapter will describe these planetary ring charging environments in detail. Finally, we describe two charging effects that demonstrate areas of future studies while providing fresh examples of the intriguing effects from planetary ring charging processes.     

Energetic particles in the inner Van Allen belt

A survey is given of the high energy particle populations in the inner radiation belt. The experiments which have given information about particles are discussed and the best experimental information about particle fluxes and spectra presented. Calculations are given which deal with the particles and indicate what particle sources and loss processes are most important. The role of neutrons in making the inner belt is considered in detail and the need for particle acceleration and/or other sources is shown.     

发动机起动过程的振动谱分析

在开展某型涡桨发动机振动监控课题研究工作时,曾迂到该型发动机在台架试车过程中出现压气机转子前部叶片严重偏磨和轴承损坏等故障,且每次都发生在起动过程,故障后均伴有严重的振动损坏现象。为此,我们决定从测量分析发动机起动过程的振动特性着手,寻找规律,为排故提供重要依据。因其问题属于瞬态振动分析,以运用实时振动分析技术进行数据处理为宜。      

The meteorite flux

Meteorites are being retrieved from the surface of our planet all the time, the number of located falls being at maximum in the range 0.3 to 1.0 yr^-1 (10⁶ km²)^-1. Using the known flux of meteorite parent bodies to the top of the atmosphere this paper reviews suggested ablation processes and predicts the actual flux of meteorites to the Earth. It is found that this is some 70 to 300 times what is observed.     

英语精读课教学方式探索

在信息时代如何提高课堂教学的信息量？如何满足学生的求知欲？本结合作的教学经验，从词汇、听力及阅读三个方面提出了有关英语教学的几点实践性见解。     

Real-Time Specifications of the Geospace Environment

We report the recent progress in our joint program of real-time mapping of ionospheric electric fields and currents and field-aligned currents through the Geospace Environment Data Analysis System (GEDAS) at the Solar-Terrestrial Environment Laboratory and similar computer systems in the world. Data from individual ground magnetometers as well as from the solar wind are collected by these systems and are used as input for the KRM and AMIE magnetogram-inversion algorithms, which calculate the two-dimensional distribution of the ionospheric parameters. One of the goals of this program is to specify the solar-terrestrial environment in terms of ionospheric processes, providing the scientific community with more than what geomagnetic activity indices and statistical models provide. This revised version was published online in August 2006 with corrections to the Cover Date.     

The Modulation of Galactic Cosmic Rays in the Heliosphere: Theory and Models

Almost all theoretical and numerical models for the modulation of cosmic ray in the heliosphere are based on Parker's transport equation which contains all the important basic physical processes. The relative importance of the various mechanisms is however not established and may vary significantly over 22 years. The simultaneous measurements of solar wind parameters, heliospheric magnetic field properties and cosmic rays over a wide range of energies and positions in the heliosphere have brought the realization that modulation is much more complicated than what the original drift models predicted. In the process the sophistication of models based on solving Parker's equation has increased by orders of magnitude. A short review of the global modulation of cosmic rays is given from a theoretical and modelling point of view.     

Concepts of turbulence and C.F.D. applications

The article's main theme is the ‘turbulence modelling’ used in present days' computational schemes. This modelling is an effort to account for the influence of turbulent motion on diffusion processes, and reflects our efforts to bridge what is generally recognized as the ‘closure gap’, i.e. to replace a needed phenomenological relation(s) with hypotheses of some kind. In this way one tries to remedy our lack of knowledge of turbulent motion. For that purpose a number of ideas and concepts over the past 60 years is mentioned and their incorporation in numerical analysis is discussed. The main emphasis is placed on the physical concepts and their consequences.     

Working Group 1 Report: Solar Wind Models from the Sun to 1 AU: Constraints by "in situ" and Remote Sensing Measurements

The goal of Working Group 1 was to discuss constraints on solar wind models. The topics for discussion, outlined by Eckart Marsch in his introduction, were: (1) what heats the corona, (2) what is the role of waves, (3) what determines the solar wind mass flux, (4) can stationary, multi-fluid models describe the fast and slow solar wind, or (5) do we need time dependent fluid models, kinetic models, and/or MHD models to describe solar wind acceleration. The discussion in the working group focused on observations of "temperatures" in the corona, mainly in coronal holes, and whether the observations of line broadening should be interpreted as thermal broadening or wave broadening. Observations of the coronal electron density and the flow speed in coronal holes were also discussed. There was only one contribution on observations of the distant solar wind, but we can place firm constraints on the solar wind particle fluxes and asymptotic flow speeds from observations with Ulysses and other spacecraft. Theoretical work on multi-fluid models, higher-order moment fluid models, and MHD models of the solar wind were also presented. This revised version was published online in June 2006 with corrections to the Cover Date.     

3-连通无爪图的最长圈

Hamilton问题是图论中重要的问题之一,已经得到了很多很好的结果,但一个图是Hamilton图的充分必要条件到现在还没有得出,于是开始研究无向图的最长圈,文章应用幅度的概念,使用反证法,通过构造最长圈并得出矛盾的方法,给出了3-连通无爪图最长圈的下限 .     

The Solar Wind and the Sun in the Past

Exposure to the solar wind can have significant long term consequences for planetary atmospheres, especially for planets such as Mars that are not protected by global magnetospheres. Estimating the effects of solar wind exposure requires knowledge of the history of the solar wind. Much of what we know about the Sun’s past behavior is based on inferences from observations of young solar-like stars. Stellar analogs of the weak solar wind cannot be detected directly, but the interaction regions between these winds and the interstellar medium have been detected and used to estimate wind properties. I here review these observations, with emphasis on what they suggest about the history of the solar wind.     

The Challenges of Plasma Modeling: Current Status and Future Plans

Successfully modeling X-ray emission from astrophysical plasmas requires a wide range of atomic data to be rapidly accessible by modeling codes, enabling calculation of synthetic spectra for fitting with observations. Over many years the astrophysical databases have roughly kept pace with the advances in detector and spectrometer technology. We outline here the basic atomic processes contributing to the emission from different types of plasmas and briefly touch on the difference between the methods used to calculate this data. We then discuss in more detail the different issues addressed by atomic databases in regards to what data to store and how to make it accessible. Finally, the question of the effect of uncertainties in atomic data is explored, as a reminder to observers that atomic data is not known to infinite precision, and should not be treated as such.     

二元推力矢量喷管导流管的设计研究

针对某型飞机进行二元推力矢量改装时对发动机出口的气流进行过渡转换的问题，设计了喷管导流管，将导流管气流截面由圆形过渡到长方形。本文利用有限元软件PATRAN对导流管进行了应力强度分析和变形分析，得出导流管的应力分布场和变形位移场，通过对不同厚度的导流管的分析计算得出导流管最大应力和最大位移随管壁厚度变化曲线，从而确定最佳的管壁厚度。研究了导流管最大应力和最大位移沿轴向的变化曲线，并对导流管的结构进行了优化设计，给出两种优化设计方案，得到较为理想的结构。     

What Can Be Learned from X-ray Spectroscopy Concerning Hot Gas in the Local Bubble and Charge Exchange Processes?

Both solar wind charge exchange emission and diffuse thermal emission from the Local Bubble are strongly dominated in the soft X-ray band by lines from highly ionized elements. While both processes share many of the same lines, the spectra should differ significantly due to the different production mechanisms, abundances, and ionization states. Despite their distinct spectral signatures, current and past observatories have lacked the spectral resolution to adequately distinguish between the two sources. High-resolution X-ray spectroscopy instrumentation proposed for future missions has the potential to answer fundamental questions such as whether there is any hot plasma in the Local Hot Bubble, and if so what are the abundances of the emitting plasma and whether the plasma is in equilibrium. Such instrumentation will provide dynamic information about the solar wind including data on ion species which are currently difficult to track. It will also make possible remote sensing of the solar wind.