CPL蒸发器多孔芯内传热传质的非稳态数值模拟

基于多孔芯内局部热力学平衡的假设，考虑了Brinkman和Forchheimer对Darcy定律的修正模型，针对简化的物理模型中所包含的气液相区域，建立了二维分层饱和多孔介质模型，以甲醇为工质对CPL，蒸发器毛细多孔芯内的传热传质过程进行非稳态数值模拟。在不同的热负荷条件下预测气液分层界面的形状和位置、系统由初态达到稳态过程的持续时间，讨论压力和温度的分布。由两层饱和模型所得到的计算结果可知．CPL系统在启动时，为避免高热流时液体脱离多孔区而发生干涸，宜采用小负荷启动；采用预热器，改善蒸气的出口条件；增加蒸发器入口处的工质的过冷度，有利于增加CPL系统启动过程和变工况时的稳定性。文中分析结论为CPL系统的优化设计提供参考。     

飞行器伺服回路的变结构设计

本文根据变结构系统(VSS)理论对某飞行器伺服回路进行了变结构设计,给出了控制器设计的详尽步骤。设计方法几何意义直观,在IBM4341机上通过了数字仿真,给出了仿真框图,并与原伺服回路的控制性能进行了比较。仿真表明,VSS比传统普通控制系统具有以下几个突出的优点;(1)快速、无超调、无稳态误差:(2)对系统参数变化具有鲁棒性;(3)对外界干扰具有鲁棒性。     

硅谐振式压力微传感器闭环系统

硅谐振压力微传感器在自激振荡回路中采取电阻热激励、电阻拾振时得到的信号,由于有用信号本身的量级小,因而含有严重的同频干扰信号(耦合激励信号),信噪比SNR (Signal Noise Ratio)仅为10^-3数量级.为了提高信噪比,滤除同频干扰,多级放大之后的处理中将锁相环PLL(Phase-Locked Loop)工作原理和分频技术相结合,由锁相环输出作为传感器的激励和鉴相相关信号,搭建硅谐振压力微传感器闭环自激振荡回路.结果表明:采用锁相分频技术的微传感器闭环系统能可靠运行,信噪比低的问题得到了很好解决.     

圆柱状含液体介质的空间辐射器的传热效率

给出了求解典型圆柱状态含液体介质的空间辐射器传热效率的解析计算公式,降低了辐射器传热效率计算的复杂度,通过与数值计算结果的比对分析,认为用流体入口温度代替辐射器平均温度的假设在工程上是能够接受的,其引起的偏差小于5%。     

一种数字化DS/BPSK扩频接收机

介绍一种新型数字化DS/BPSK(Direct Spread/Binary Phase Shife Keying)扩频接收机的设计.该接收机采用专用数字相关器为核心的硬件设计,并结合数字处理算法完成扩频信号的解调.技术上采用串并组合的伪码捕获、科斯特环载波跟踪、延迟锁定环伪码跟踪等方式,可通过软件算法灵活实现.该接收机具有综合性能强,及软件接口灵活的特点,可有效地应用于基于码分多址的多目标测控系统中.     

Detailed magnetic structure and stochastic threshold

Non-linear evolution of reconnection is too slow to explain-by itself-fast phenomena such as internal disruptions in tokamaks or flares in the solar atmosphere. It has been proposed that the change in topology could lead to field line stochastization, and hence to highly increased transport. An important objection to this idea is that the increase of transport coefficients should smoothly follow the amplitude of the perturbation, while the observations show a catastrophic transition. We have shown 1) that the shape of the structures (and not only their size or amplitude) evolve during non-linear evolution 2) that the stochastic threshold can be strongly influenced by the detailed shape. Therefore, sharp transitions can appear during the evolution, due to the combination of these two effects. We will first consider an idealized situation, namely the two-waves problem in slab geometry, for which we will study the effect of the separatrix shape on the stochastic threshold. In the second part, we will present an application to the internal disruption in tokamaks, with anm=1 perturbation in a toroidal magnetic configuration. In the last part, we will discuss possible applications of the studies on shape effects to the behaviour of trapped particles in structures of the solar atmosphere.     

基于软件锁相环的电机速度控制系统

随着电力电子、微电子技术和控制技术的发展，一些场合对电机调速系统性能的要求越来越高，而锁相调速控制在稳速精度方面有其独特的优势。文章在改进的数字锁相环基础上，提出了软件锁相环电机速度控制系统，利用高性能微处理器实现了软件锁相环。     

On the nature of coronal loops above the quiet sun network

The structure and dynamics of a box in a stellar corona can be modeled employing a 3D MHD model for different levels of magnetic activity. Depending on the magnetic flux through the surface the nature of the resulting coronal structures can be quite different. We investigate a model of an active region for two sunspots surrounded by magnetic field patches comparable in magnetic flux to the sunspots. The model results in emission from the model corona being concentrated in loop structures. In Gudiksen and Nordlund (2005) the loops seen in EUV and X-ray emission outline the magnetic field, following the general paradigm. However, in our model, where the magnetic field is far from a force-free state, the loops seen in X-ray emission do not follow the magnetic field lines. This result is of interest especially for loops as found in areas where the magnetic field emerging from active regions interacts with the surrounding network.     

Statistical study of twist values of transequatorial loops and the relationship with flares

In this paper, the twist values of ‘S’-shape transequatorial loops (TLs) from 1991 to 2001 are calculated, GOES soft X-ray flares dataset of the active regions connected by these TLs are investigated. The result shows the twist value of the TLs has a weak relation with the flare flux. There is no clear correlation between the twist value and the distance between the footpoint of TLs and location of flare in the corresponding active regions.     

A question raised from the observation of dynamic cusp formation: When and where does particle acceleration occur?

We present observations of a C9.4 flare on 2002 June 2 in EUV (TRACE) and X-rays (RHESSI). The multiwavelength data reveal: (1) the involvement of a quadrupole magnetic configuration; (2) loop expansion and ribbon motion in the pre-impulsive phase; (3) gradual formation of a new compact loop with a long cusp at the top during the impulsive phase of the flare; (4) appearance of a large, twisted loop above the cusp expanding outward immediately after the hard X-ray peak; and (5) X-ray emission observed only from the new compact loop and the cusp. In particular, the gradual formation of an EUV cusp feature is very clear. The observations also reveal the timing of the cusp formation and particle acceleration: most of the impulsive hard X-rays (>25 keV) were emitted before the cusp was seen. This suggests that fast reconnection occurred during the restructuring of the magnetic configuration, resulting in more efficient particle acceleration, while the reconnection slowed after the cusp was completely formed and the magnetic geometry was stabilized. This observation is consistent with the observations obtained with Yohkoh/Soft X-ray Telescope (SXT) that soft X-ray cusp structures only appear after the major impulsive energy release in solar flares. These observations have important implications for the modeling of magnetic reconnection and particle acceleration.