Composition Variations in the Solar Corona and Solar Wind

Order of magnitude variations in relative elemental abundances are observed in the solar corona and solar wind. The instruments aboard SOHO make it possible to explore these variations in detail to determine whether they arise near the solar surface or higher in the corona. A substantial enhancement of low First Ionization Potential (FIP) elements relative to high FIP elements is often seen in both the corona and the solar wind, and that must arise in the chromosphere. Several theoretical models have been put forward to account for the FIP effect, but as yet even the basic physical mechanism responsible remains an open question. Evidence for gravitational settling is also found at larger heights in quiescent streamers. The question is why the heavier elements don't settle out completely. This revised version was published online in June 2006 with corrections to the Cover Date.     

Streamer Evaporation

Streamer evaporation is the consequence of heating in ideal MHD models because plasma is weakly contained by the magnetic field. Heating causes inflation, opening of field lines, and release of solar wind. It was discovered in simulations and, due to the absence of loss mechanisms, the ultimate end point is the complete evaporation of the streamer. Of course streamers do not behave in this way because of losses by thermal conduction and radiation. Heating is also expected to depend on ambient conditions. We use a global MHD model with thermal conduction to examine the effect of changing the heating scale height. We also extend an analytic model of streamers developed by Pneuman (1968) to show that steady streamers are unable to contain plasma for temperatures near the cusp greater than ∼ 2 × 10⁶ K. This revised version was published online in June 2006 with corrections to the Cover Date.     

Dynamics of Coronal Loop Oscillations Recent Improvements and Computational Aspects

We will discuss the observed, heavily damped transversal oscillations of coronal loops. These oscillations are often modeled as transversal kink oscillations in a cylinder. Several features are added to the classical cylindrical model. In our models we include loop curvature, longitudinal density stratification, and highly inhomogeneous radial density profiles. In this paper, we will first give an overview of recently obtained results, both analytically and numerically. After that, we shed a light on the computational aspects of the modeling process. In particular, we will focus on the parallellization of the numerical codes.     

尖化前缘高导热材料防热分析

针对飞行器高超声速飞行时严重的气动加热环境,提出疏导式热防护结构( TPS),为飞行器前缘提供热防护.采用有限元法和有限体积法,分别对在特定工况下飞行的尖化前缘固体域和流体域进行计算,验证了前缘内嵌高导热材料的防热效果,其中来流马赫数为6.5时,头部壁面最高温度下降了13.6％,尾部最低温度升高了16.7％,实现了热流...     

旋转受照状态下天线温度场仿真分析

在进行星表天线地面真空热环境试验过程中,传统的红外加热设备会造成测量光路遮挡、降温速率减慢等影响。为提高试验准确性,提出了基于天线旋转受照的真空热试验方法。利用虚拟热试验平台对旋转受照状态下天线温度场进行仿真分析,得到天线温度场的分布与变化,并与试验数据对比,验证了仿真建模的准确性和试验方法的可行性。     

电机变频控制实现换热器节能的应用研究

结合寒冷地区气候特点与通信机房温控的现状,针对50%浓度乙二醇溶液为工质的换热器,试验研究了自然冷源利用率与换热器自身变频节能的关系。结合乙二醇冷剂的特性,通过建立功率与频率关系模型、温差与功率和频率关系模型,实现了换热器循环泵和风机的变频控制策略。结果表明:在室内外温差、换热功率与循环泵、风机频率同时满足的条件下,以功率模型作为参数进行换热器自身的变频节能是可行的。通过对哈尔滨地区的气候数据与散热房控温试验分析,证明了乙二醇换热器的变频节能效果。     

宽马赫数路德维希管风洞及其关键技术

随着高马赫数飞行器研制需求的增加,急需脉冲型风洞运行范围向中低马赫数段扩展,特别是需要具有跨马赫数运行能力。以路德维希管原理运行的管风洞试验设备,由于建设及使用成本较低、参数调节方便、流场品质高等优点,已在亚/跨/超声速及高超声速领域得到了发展和应用,体现出了宽马赫数的应用潜力。本文分析了宽马赫数脉冲型风洞发展现状,重点介绍了路德维希管风洞及其在宽马赫数应用中急需解决的关键技术,包括宽马赫数喷管设计技术、高温管外加热技术以及高温高压隔离技术。     

地源热泵技术在建筑节能中的应用

本文探讨如何通过地源热泵技术实现建筑节能。研究通过地源热泵来实现一机多用,使其既能用于冬季供暖,又可以用于夏季制冷。同时也讨论了如何与太阳能相配合,来实现地热平衡。文中还给出了通过插值法和曲线拟合法对测量数据进行处理获得变温带和增温带的温度-深度曲线的方法。     

暴时极光区热层大气焦耳加热与F区电离耗空的EISCAT雷达观测

利用ＥＩＳＣＡＴ雷达探测数据，分析计算了太阳活动高年夏季发生的一次强磁暴期间，极光区电离层对流电场、电导率以及焦耳加热速率等着重考察了Ｅ区热怪大气焦耳加热和Ｆ区离子摩擦增温与Ｆ区电子密度耗空的关系发现在下午东向极光电集流期间，电子密度最大耗空出现在Ｆ区３００－３２５ｋｍ高度，时间恰在积分的Ｅ区大气焦耳加热量大值和Ｆ区最大离子增温之后５－１０ｍｉｎ，耗空率达７０％。     

Spectroscopic Constraints on Models of Ion-cyclotron Resonance Heating in the Polar Solar Corona

Using empirical velocity distributions derived from UVCS and SUMER ultraviolet spectroscopy, we construct theoretical models of anisotropic ion temperatures in the polar solar corona. The primary energy deposition mechanism we investigate is the dissipation of high frequency (10-10000 Hz) ion-cyclotron resonant Alfvén waves which can heat and accelerate ions differently depending on their charge and mass. We find that it is possible to explain the observed high perpendicular temperatures and strong anisotropies with relatively small amplitudes for the resonant waves. There is suggestive evidence for steepening of the Alfvén wave spectrum between the coronal base and the largest heights observed spectroscopically. Because the ion-cyclotron wave dissipation is rapid, even for minor ions like O⁵⁺, the observed extended heating seems to demand a constantly replenished population of waves over several solar radii. This indicates that the waves are generated gradually throughout the wind rather than propagated up from the base of the corona. This revised version was published online in June 2006 with corrections to the Cover Date.