远场涡流检测中的相速度分析

对远场的相速特性作了较详细的分析。文中首先从电磁场有限元出发对轴向和径向上的似稳态场相速度作了仿真研究，发现其在空间某些位置上具有稳定的相速，与波特点相似。同时分析了参数μ，σ，ｆ对相速的影响。结果表明，其与电磁波在良导体中传播规律的定性分析相符。最后本文还对瞬态激励下的远场涡流效应作了一定分析，结果再次证明其具有似波特性。     

异种材料的连接

异种材料之间的物理、化学及力学性能方面存在巨大差异,对连接方法要求非常苛刻。重点介绍了一些典型异种材料组合的连接问题,探讨了铝合金与其他材料、铜与其他材料、钛合金与其他材料以及异种非金属等的连接技术,为异种材料的连接提供了一定的技术指导。     

软件锁相环的设计与应用

根据虚拟无线电技术的特点和锁相环的基本原理,提出一种适于计算机软件化实现的锁相环数学模型,分析不同参数对锁相环捕获和跟踪性能的影响,得出不同情况下参数设定的基本准则。计算机仿真结果表明,软件锁相环在加性高斯白噪声信道下具有较好的捕获与跟踪性能。最后提出软件锁相环在测控系统中实现信号实时处理的优化方法。     

基于多参数特征的辐射源识别技术

针对复杂战场电磁环境下辐射源识别困难的问题,提出一种基于多参数特征的辐射源识别方法。介绍了辐射源辐射信号特征量的提取技术,给出了识别的原理和步骤。最后在小样本和大样本辐射源数据库的基础上,利用该识别技术进行了仿真,结果证明了基于多参数特征的辐射源识别方法的有效性和准确性,相比于传统的辐射源识别技术,该方法识别率更高,速度更快。     

RPC-MIP: the Mutual Impedance Probe of the Rosetta Plasma Consortium

The main objective of the Mutual Impedance Probe (MIP), part of the Rosetta Plasma Consortium (RPC), is to measure the electron density and temperature of Comet 67P/Churyumov-Gerasimenko’s coma, in particular inside the contact surface. Furthermore, MIP will determine the bulk velocity of the ionised outflowing atmosphere, define the spectral distribution of natural plasma waves, and monitor dust and gas activities around the nucleus. The MIP instrumentation consists of an electronics board for signal processing in the 7 kHz to 3.5 MHz range and a sensor unit of two receiving and two transmitting electrodes mounted on a 1-m long bar. In addition, the Langmuir probe of the RPC/LAP instrument that is at about 4 m from the MIP sensor can be used as a transmitter (in place of the MIP ones) and MIP as a receiver in order to have access to the density and temperature of plasmas at higher Debye lengths than those for which the MIP is originally designed.     

Primordial matter in the outer solar system: A study of its chemical composition from remote spectroscopic analysis

Our knowledge of the primordial matter from the objects of the outer solar system has made a considerable progress over the past years, in spite of the lack of any in situ measurements of these objects at the present time. The recent progress of ground-based instrumentation and the launch of the two Voyager fly-by missions have provided a huge amount of new informations about the origin and the evolution of the primitive Solar System objects.The most significant discoveries concerning the atmospheres of the Giant Planets can be summarized as follows: (1) there does not seem to be any differentiation in the internal structure of Jupiter during the planet's history; thus, the H₂/He ratio measured on Jupiter seems to be representative of the H/He ratio of the Primordial Nebula; (2) there is some evidence for a helium differentiation, relative to hydrogen, in Saturn's interior; (3) there seems to be a carbon enrichment on both Jupiter and Saturn by a factor about 2; this result is consistent with a model in which the planetary core is formed first, and the atmosphere accreted by this core in a second stage; (4) the D/H ratio measured on Jupiter should be representative of the D/H value in the Primordial Nebula, 4.5 billion years ago; this value is 2 to 5 times larger than the mean value measured in the local interstellar medium now; (5) Titan's atmosphere is dominated by nitrogen and contains traces of organic and prebiotic molecules (HCN, C₂N₂, HC₃N); the chemical composition of Titan's atmosphere could be favorable for the early stages of life development.The small bodies of the Solar System — asteroïds and comets — are still very poorly known. However they contain a key information about the physical and chemical properties of dust in the Primordial Nebula and the interstellar medium. With the launch of expected fly-by missions towards Comet Halley and, possibly, towards asteroïds, we may hope to know a new development of our understanding of these objects, comparable to the progress we have known on the Giant Planets over the past ten years.     

On the origin of the grooves on Phobos

L-grooves are the consequence of layered structure of Phobos, which are made up of parallel layers of different composition or hardness.     

L'avion,plateforme d'observations scientifiques

Transition between high altitude manned observatories and unmanned balloon-borne or rocket-borne experiments is achieved with high flying aircrafts, at altitudes above tropopause (>12 km), which became readily available, at reasonable cost and reliability, in the past five or ten years.This paper reviews the development of scientific uses of aircrafts, especially for astronomy and geophysics, with some emphasis placed on infrared problems, closely related to the scale height of the chief infrared absorber, i.e. telluric water vapor.Absorbers distribution vs altitude and spectral characteristics are summarized (Figures 1, 2, 3).Capabilities of various available aircrafts are compared (Table I) and the various ways to consider modifications are discussed: structural modifications or design problems to fit telescopes or light collectors on board. Tables II and III list the advantages of airborne observations, compared to other spatial carriers, and also the specific problems connected with aircrafts. Adopted solutions to these problems are exposed (Figures 4, 5, 6, 7) and costs are briefly discussed.Finally, a few examples of scientific results, gathered in the few past years from aircraft, are given, both in astronomy and in geophysics.