Broadening of Fe X (6374 Å) profiles above the limb in a coronal hole

Profiles of the visible Fe X (6374 Å) coronal emission line as a function of height above the limb were obtained out to 1.16 solar radii in a coronal hole using the NSO/Sacramento Peak Observatory Coronagraph, Universal Spectrograph and a CCD camera. These are the first coronal line profiles obtained as a function of height in a coronal hole from the ground. Analysis of the line widths suggests a large component of nonthermal broadening which increases with height ranging from 40 to 60 km/s, depending upon the assumed temperature or thermal component of the profile.     

低RCS飞行器外形设计实践

 在鸭式布局的基础上 ,对飞行器各部件及部件间的连接方式进行了外形隐身设计。对初步形成的鸭翼 -翼身融合体改变机身头部形状和立尾配置等进行 RCS优化。给出了飞行器各种状态下的 RCS平均值和迎头± 45°区内的 RCS值。测试结果表明 ,尖头机身、 30°双立尾 (立尾与垂直平面成± 30°角 )的鸭翼 -翼身融合体的 RCS值最小。对 RCS优化后的外形 ,风洞测力试验表明其气动性能也较好 (最大升阻比达到 8,失速迎角超过 2 6°)     

Energetic particles at high latitudes

We review work on diffusion coefficients of energetic particles with an attempt to extract implications on their behaviour at high latitudes. In the ecliptic plane results from solar energetic particle propagation between the Sun and about 5 AU can be described by an effective radial mean free path _r which is approximately constant as a function of distancer. When particle propagation in three dimensions in the heliosphere is considered it is not sufficient to consider _r only. Jovian electrons can be used as probes to determine the parameters of three-dimensional diffusion. In the polar regions diffusion is dominated by its parallel component. Some predictions how should vary with latitude are discussed. For different choices of this variation we present expectations for intensity-time profiles of solar particle events during the Ulysses polar passages.     

SDM 标模大攻角动导数试验

介绍了ＣＡＲＤＣ高速所１．２ｍ风洞大攻角的动导数试验装置与测量系统以及在１．２ｍ风洞中对标准动态模型（ＳＤＭ标模）所作的一系列风洞试验结果。试验结果与国外文献数据具有较好的一致性。试验结果随马赫数和攻角的变化表现出明显的非线性,而减缩频率的影响并不显著。天平与测试系统的重复性精度较高。     

PVM平台下通量守恒的嵌入自适应网格解激波和底部流

运用嵌入式自适应网格技术来提高结构网格求解复杂流场的分辨率。该方法根据流场的形成,将密集网格嵌入到物理量剧烈变化的区域,使求解精度得以提高的同时,避免较大的计算开销,从而达到求解效率和求解精度之间的平衡。 Ｐ Ｖ Ｍ 平台使得被嵌入的网格可以在网络中不同的机器上完成,大幅度降低了墙上时间。原始网格与被嵌入网格之间数值通量守恒的实现增强了该方法在捕捉间断时的有效性和可靠性。     

Solar Irradiance Variability Since 1978

Since November 1978 a set of total solar irradiance (TSI) measurements from space is available, yielding a time series of more than 25 years. Presently, there are three TSI composites available, called PMOD, ACRIM and IRMB, which are all constructed from the same original data, but use different procedures to correct for sensitivity changes. The PMOD composite is the only one which also corrects the early HF data for degradation. The results from the detailed analysis of the VIRGO radiometry allow a good understanding of the effects influencing the long-term behaviour of classical radiometers in space. Thus, a re-analysis of the behaviour of HF/NIMBUS-7 and ACRIM-I/SMM was indicated. For the former the situation is complicated by the fact that there are no in-flight means to determine changes due to exposure to solar radiation by comparison with a less exposed radiometer on the same spacecraft. The geometry and optical property of the cavity of HF is, however, very similar to the PMO6-type radiometers, so the behaviour of the PMO6V radiometers on VIRGO can be used as a model. ACRIM-I had to be revised mainly due to a henceforth undetected early increase and a more detailed analysis of its degradation. The results are not only important for solar radiometry from space, but they also provide a more reliable TSI during cycle 21. The differences between the revised PMOD composite and the ACRIM and IRMB are discussed by comparison with a TSI reconstruction from Kitt-Peak magnetograms. As the PMOD composite is the only one which has reliable data for cycle 21, the behaviour of the three solar cycles can now be compared and the similarities and differences discussed.     

Global Response of Martian Plasma Environment to an Interplanetary Structure: From Ena and Plasma Observations at Mars

As a part of the global plasma environment study of Mars and its response to the solar wind, we have analyzed a peculiar case of the subsolar energetic neutral atom (ENA) jet observed on June 7, 2004 by the Neutral Particle Detector (NPD) on board the Mars Express satellite. The “subsolar ENA jet” is generated by the interaction between the solar wind and the Martian exosphere, and is one of the most intense sources of ENA flux observed in the vicinity of Mars. On June 7, 2004 (orbit 485 of Mars Express), the NPD observed a very intense subsolar ENA jet, which then abruptly decreased within ∼10 sec followed by quasi-periodic (∼1 min) flux variations. Simultaneously, the plasma sensors detected a solar wind structure, which was most likely an interplanetary shock surface. The abrupt decrease of the ENA flux and the quasi-periodic flux variations can be understood in the framework of the global response of the Martian plasma obstacle to the interplanetary shock. The generation region of the subsolar ENA jet was pushed towards the planet by the interplanetary shock; and therefore, Mars Express went out of the ENA jet region. Associated global vibrations of the Martian plasma obstacle may have been the cause of the quasi-periodic flux variations of the ENA flux at the spacecraft location.     

三维舵面绕流的N-S方程计算研究

基于粘性非结构混合网格,采用格心格式的有限体积法,应用Spalart-Allmaras湍流模型进行绕三维舵面流动的N-S方程数值模拟。操纵面铰链力矩的计算结果与风洞试验结果的对比分析表明,计算方法对粘性流动具有良好的适应性。对舵面铰链力矩随迎角、马赫数、雷诺数变化的规律也进行了分析研究。     

平流层长航时气球轨迹控制系统研究

首先介绍了平流层气球的应用意义及进行轨迹控制的必要性,然后描述了一种基于不同海拔风速差的轨迹控制方法,简要说明了平流层风速随海拔的变化规律,在此基础上研究了包括超压气球和轨迹控制系统在内的气球飞行系统各部分特点,最后简单分析了整个飞行系统的建模与仿真中的要点问题。结果表明,这种轨迹控制方法是一种几乎不需要消耗能源的有效轨迹控制方法,具有较高的应用价值和推广价值。