转动帆板红外热流计算及等效方法研究

目前的空间外热流分析软件和在航天器稳态热平衡试验中模拟的外热流都不包括帆板对航天器表面的红外加热,而有时帆板的红外加热并不小,应该叠加到模拟的外热流中.文章针对一种低轨道航天器,计算了帆板红外加热的强度,给出了在热平衡试验中叠加的方法,并讨论了在固定帆板方位的同时保持其红外热流等效的可能性.结果表明,可以精确计算帆板红外加热,对任意的帆板方位均可以保持其红外加热的等效.     

反射器夹层面板精密成形原理

对高精度、大面积不可展双曲反射面的制造问题,提出了基于"离散钉模、真空负压、蜂窝夹层、应力释放、回弹补偿"的高精度反射面板成形原理;建立了四边自由面内多点约束的薄板大挠度弯曲解法及夹层板成形过程仿真模型,用于确定成形工艺参数;利用动力显式和静力隐式算法相结合的方法实现成形过程仿真;通过开缝和开槽方法释放面内压应力,确定了面板开缝和开槽方案;通过逆向修正离散模包络面,使其与成形模拟得到的夹层板型面误差最小,得到模具修正因子,补偿回弹误差.在此基础上开发了夹层板精密成形CAE系统.该方法制造的面板型面精度RMS达到25 μm以下,已成功地应用于多项大型紧缩场和毫米波天线的制造.      

Solar Variability and the Earth's Climate: Introduction and Overview

Numerous attempts have been made over the years to link various aspects of solar variability to changes in the Earth's climate. There has been growing interest in this possible connection in recent years, spurred largely by the need to understand the natural causes of climate change, against which the expected global warming due to man's activities will have to be detected. The time scale of concern here is that of decades to centuries, and excludes the longer millennial scale in which orbital variations play a dominant role. The field has long been plagued by the lack of an acceptable physical mechanism by which solar variability can affect climate, but the discovery of variability in the Sun's total irradiance (the solar ``constant' of meteorology) by spacecraft instruments has pointed to a direct mechanism. Other less direct mechanisms that have been suggested involve variations in the Sun's ultraviolet flux and in the plasma outflow of the solar wind. The purpose of this paper is to summarize the current state of the field, emphasizing the proposed mechanisms as an introduction to the more detailed papers that follow. The particular case of sea-surface temperature data will be used as an illustration.     

薄壁板结构声激励载荷作用下的响应谱估算方法

本文提出一种估算薄壁板结构在声激励载荷作用下的响应谱的方法。这一方法借助板式结构的线性振动理论, 研究薄壁板结构在声激励载荷作用下动力响应问题, 引入结合受纳函数来考虑结构模态的波长和声波长在空间的耦合程度。本文给出的估算薄壁板结构声激励响应的方法, 不仅对规则的几何结构有效, 而且也应用于复杂薄壁板结构的分析。并将估算的结果与实验值做出了比较, 较为吻合。      

月面巡视器太阳能帆板功率衰减特性研究

太阳能帆板的功率衰减特性分析,对地外天体表面探测器的功率平衡、电源系统健康管理以及长寿命在轨管理有重要意义。通过对月面巡视器在轨运行第2到11月昼的电流遥测进行研究,提出了一种基于有限遥测的太阳能帆板功率衰减特性分析方法。首先利用一种滞环的方法对大量的电流遥测进行数据处理;然后进行日月距离和太阳入射角的归一化,通过数据拟合计算,得出落月第一年太阳能帆板功率衰减约为2.5%,并利用巡视器历次月昼唤醒时刻的太阳入射角变化情况验证了该方法的有效性,对地外天体的太阳能帆板功率衰减特性计算提供一定参考。     

Observations of the local interstellar medium with the Extreme Ultraviolet Explorer

Because of the strong absorption of extreme ultraviolet radiation by hydrogen and helium, almost every observation with the Extreme Ultraviolet Explorer (EUVE) satellite is affected by the diffuse clouds of neutral gas in the local interstellar medium (LISM). This paper reviews some of the highlights of the EUVE results on the distribution and physical state of the LISM and the implications of these results with respect to the interface of the LISM and the heliosphere. The distribution of sources found with the EUVE all-sky surveys shows an enhancement in absorption toward the galactic center. Individual spectra toward nearby continuum sources provide evidence of a greater ionization of helium than hydrogen in the Local Cloud with an mean ratio of H I/He I of 14.7. The spectral distribution of the EUV stellar radiation field has been measured, which provides a lower limit to local H II and He II densities, but this radiation field alone cannot explain the local helium ionization. A combination of EUVE measurements of H I, He I, and He II columns plus the measurement of the local He I density with interplanetary probes can place constraints on the local values of the H I density outside the heliosphere to lie between 0.15 and 0.34 cm^–3 while the H II density ranges between 0.0 and 0.14 cm^–3. The thermal pressure (P/k = nT) of the Local Cloud is derived to be between 1700 and 2300 cm^–3 K, a factor of 2 to 3 above previous estimates.     

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.     

Dissipative Solitary Kinetic Alfvén Waves and Electron Acceleration in the Solar Corona

Nonthermal electrons play a major role during solar flares since not only they contain a large amount of the released energy but also they provide important information of the flaring physics through their nonthermal radiation in radio and hard X-ray bands. In a recent work Wu (Phys. Plasmas 10 (2003) 1364) proposed that dissipative solitary kinetic Alfvén wave (DSKAW) with a local shock-like structure could provide an efficient acceleration mechanism for energetic electrons in a low-β plasma. In the present paper dynamical characteristics of the DSKAW acceleration mechanism in solar coronal plasmas are studied and its application to the acceleration of flaring electrons is discussed.     

Working group 3: Coronal streamers

The working group on coronal streamers convened on the first day of the 2nd SOHO Workshop, which took place in Marciana Marina, Isola d'Elba, 27 September –1 October 1993. Recent progress in streamer observational techniques and theoretical modeling was reported. The contribution of streamers to the mass and energy supply for the solar wind was discussed. Moreover, the importance of thin electric current sheets for determining both the gross dynamical properties of streamers and the fine-scale filamentary structure within streamers, was strongly emphasized. Potential advances to our understanding of these areas of coronal physics that could be made by the contingent of instruments aboard SOHO were pointed out.     

Thermal and nonthermal flare emission observed with the Nobeyama Radio Heliograph

The early phases of three flares, observed by the Nobeyama Radio Heliograph, are studied. Nonthermal and thermal radio sources are identified by comparison with soft X-ray images taken by the Soft X-ray Telescope onboard the Yohkoh satellite. Two of the flares are mainly of nonthermal origin and their location coincides with one of the footpoints of soft X-ray loops. Another flare has both thermal and nonthermal components which start to brighten simultaneously. This suggests that particle acceleration and plasma compression develop simultaneously.