The Modulation of Galactic Cosmic Rays in the Heliosphere: Theory and Models

Almost all theoretical and numerical models for the modulation of cosmic ray in the heliosphere are based on Parker's transport equation which contains all the important basic physical processes. The relative importance of the various mechanisms is however not established and may vary significantly over 22 years. The simultaneous measurements of solar wind parameters, heliospheric magnetic field properties and cosmic rays over a wide range of energies and positions in the heliosphere have brought the realization that modulation is much more complicated than what the original drift models predicted. In the process the sophistication of models based on solving Parker's equation has increased by orders of magnitude. A short review of the global modulation of cosmic rays is given from a theoretical and modelling point of view.     

梁式机翼的控制寿命设计与验证

应用“替损件”的设计思想来控制梁式机翼的疲劳寿命,并在××机翼主梁的寿命试验和全机组合疲劳试验中得到验证,得出十分满意的结果,为梁式机翼结构实现长寿命高可靠性的目标,提供一条成功的途径。     

连翼机低速气动特性实验研究

连翼机具有前、后机翼,前翼后掠上反,后翼前掠下反;后翼在前翼展60％～100％之间与前翼相连。其前视图和俯视图均构成菱形。在低速风洞中对连翼机进行了纵向及横向测力实验,其中包括前、后翼几何参数改变对气动特性的影响。实验表明,与常规飞机相比连翼机具有如下优点:诱导阻力小,升阻比大且具有较好的失速特性。改变连翼机前翼上反角和后翼下反角对纵向气动特性影响不大,对横向气动特性有明显影响。减小前翼外段的后掠角可使俯仰特性得到改善。     

典型复合材料机翼铺层设计分析

利用DASCM程序完成带整体油箱复合材料机翼铺层设计的优选方法、原理和算例。采用了灵敏度分析和导数均匀化两种方法进行复合材料铺层优选设计。优选设计后的复合材料机翼重量仅比金属机翼增重0.84kg,而颤振速度却提高22.6％,满足了设计要求,而且大大加快了设计速度。     

用三维欧拉方程计算机身与机翼绕流

本文用Jameson的三维欧拉方程有限体积法、四步Runge-Kutta时间推进格式,计算机身和大后掠细长机翼的三维可压缩绕流。对钝头机身,用C-O型网格;尖头机身与大后掠细长机翼用H-O型网格。本文介绍钝头旋成体、带座舱前机身和三角翼绕流的计算结果,显示流场等值M线分布,计算压强系数分布与实验比较,以及三角翼大迎角分离涡等。由于用了隐式残值光顺等加速收敛措施,有效地减少推进步数,节省机时。     

EXPERIMENTAL RESEARCH OF THE CONFIGURATION OF WING－TIP DRAG REDUCTION FOR LIGHT AIRCRAFT

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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.     

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.