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.     

Local clouds: Distribution, density and kinematics through ground-based and HST spectroscopy

The distribution, kinematics and physical properties of the interstellar matter surrounding the Sun can be inferred from ground-based and UV spectroscopic observations. On a 200 pc scale the local interstellar matter appears inhomogeneous and asymmetric. Although it generally flows towards the lower density region, it is composed of numerous small components a few parsecs in size with slightly different velocities. On a smaller scale the extent and the nature of the Local Cloud which flows over the Sun are discussed based on HST-GHRS observations of nearby stars.     

某空间站太阳电池阵中央桁架热-结构耦合动力学分析

本文研究了大型空间结构的热振动问题。提出了全区间耦合单步内非耦合的有限元计算方法。既满足了计算精度，又提高了计算效率。通过对某型空间站太阳电池阵中央桁架热振动的数值仿真，得到了若干对工程实际有一定参考价值的结论。     

Interplanetary scintillation observations of the high-latitude solar wind

Until the ULYSSES spacecraft reached the polar regions of the solar wind, the only high-latitude measurements available were from indirect techniques. The most productive observations in regions of the solar wind between 5R and 200R have been the family of radio scattering techniques loosely referred to as Interplanetary Scintillation (IPS) (Coles, 1978). Useful observations can be obtained using a variety of radio sources, for example spacecraft beacons, planetary radar echoes and compact cosmic sources (quasars, active galactic nuclei, pulsars, galactic masers, etc.). However for measurement of the high-latitude solar wind cosmic sources provide the widest coverage and this review will be confined to such observations. IPS observations played a very important role in establishing that polar coronal holes (first observed in soft x-ray emission) were sources of fast solar wind streams which occasionally extend down to the equatorial region and are observed by spacecraft. Here I will review the IPS technique and show the variation of both the velocity and the turbulence level with latitude over the last solar cycle. I will also outline recent work and discuss comparisons that we hope to make between IPS and ULYSSES observations.     

Latitude and solar-cycle dependence of radial IMF intensity

I describe a simple procedure for extrapolating the observed solar magnetic field into the heliosphere, which averages the asymptotic fields computed using the standard source surface and current sheet models. The resultant field is characterized by strong latitudinal gradients (maintained by volume currents outside the source surface) and by abrupt reversals in direction at the current sheets. The model yields good agreement with the observed long-term variation of the radial IMF component in the ecliptic, and is used to predict the variation of |B _r | along the latitudinal trajectory of Ulysses during 1990–1994. As found in earlier studies, the magnitude ofB _r at any latitude is determined largely by the strength and relative orientation of the Sun's dipole moment.     

积分球太阳辐照模拟源的研制

文章主要从积分球、聚光系统、线性减光系统和光谱测量等方面,介绍了积分球太阳辐照模拟源的研制过程。太阳辐照模拟源采用氙灯和溴钨灯的双光源方式,滤光片对氙灯、溴钨灯的光谱进行截止和校正后,合成太阳光谱,并且通过能量计算确定了两只灯的功率大小。线性减光系统使积分球出射口的辐亮度从最大值按照10％递减,线性输出10档辐亮度值。该积分球太阳辐照模拟源用于卫星遥感器的辐射定标。     

新型航天器太阳电池阵基板的质量控制

影响新型航天器太阳电池阵基板的质量因素较多,且很复杂。文章着重介绍了基板的质量控制内容,还对一些突出的质量问题作了简述。     

KM6太阳模拟器冷却系统

太阳模拟器是在冷黑和真空环境中模拟太阳辐照的一种重要设备,其冷却系统主要用于太阳模拟器氙灯的冷却和光学组件的冷却。冷却系统主要由高压水冷却、低压水冷却、低压氮气冷却、氟里昂制冷和去离子水等5部分组成,文章分别介绍了它们的流程和特点。文章参考了ESTEC冷却系统的经验,对KM6太阳模拟器冷却系统进行了优化设计,特别采用了去离子水、密闭循环、模块化机组、PCL控制系统等多种技术,提高了系统的可靠性。此系统设计方法可以应用到其他类似太阳模拟器冷却系统和大型常温冷却系统的设计。     

日地共转扰动似稳结构及其反相和漂移规律的最新证据

日地共转扰动似稳结构及其反相现象在第２１及２２周再次显现，从而证实了上述发现是一种在长达世记的时间尺度内存在的普遍规律。包括１９９１－１９９２年内的百年地磁扰动资料还说明偶数太阳周的共转似稳结构扰动峰有逆太阳自转而线性性漂移的趋向。对即将来临的极小年前可能出现的共转扰动作了试验性的预测。