总装材料对氦气吸附性能的试验研究

文章对卫星总装中所使用的部分吸附性材料进行了氦气吸附性能试验研究。通过试验及分析证明了所采用的吸附性材料对氦气的吸附很小,在采用累积法进行卫星检漏时,吸附性材料对检漏结果的影响可以忽略。     

高精度航天器微振动力学环境分析

高精度航天器由于其指向精度和分辨率水平极高,需要考虑微振动的影响。文章给出了微振动的定义,分析了微振动特性、国外研究现状、建模特点及方法,总结归纳了高精度航天器星体内部的主要扰动源。给出了反作用轮、斯特林低温制冷器、星载敏感器以及太阳翼等典型扰动源扰动的时域或频域模型及微振动隔离模型,并进行了相应的仿真,从系统层面评估了微振动对高精度航天器性能的影响,可供高精度航天器设计时参考。     

高超声速飞行器起飞质量的解析估算

基于火箭助推的发射方式,推导出弹道式飞行器、高超声速助推-滑翔飞行器及高超声速助推-巡航飞行器的起飞质量与航程、燃料比冲和载荷之间的解析关系,为总体设计初期快速估算飞行器起飞质量提供了方法。基于此,比较了3种飞行器的起飞质量载荷比。结果表明,助推-巡航飞行器性能最优,助推-滑翔飞行器性能居中,弹道式飞行器的性能最差。     

航空发动机承力结构隔振设计方法及试验

基于先进航空发动机承力框架的结构与力学特征,通过理论分析与仿真计算验证了高隔振性承力框架结构动力学设计方法。通过对承力结构刚度/质量分布及几何构形突变的优化设计,提高转子支承结构在宽频域内的机械阻抗,实现在转子工作转速范围内的高隔振性。根据承力结构刚度/质量分布对隔振性的影响,采用折返式非连续结构,设计并搭建了转子-承力框架试验系统,通过试验进一步验证了高隔振性承力框架设计方法。试验结果表明:在承力结构中采用非连续性设计可在宽频域内对不同位置支点处激励具有良好的隔振效果。      

轴流风机的进口径向畸变研究

对轴流风机的进口速度畸变情况进行了分析,利用改进的双激盘理论通过进口速度分布的改变来分析进口畸变对于性能的影响,并且将模型的计算结果与实际的实验结果相比较,得到一种合理的速度分布.      

新型曲面压缩的高超侧压式进气道数值仿真

为进一步提高侧压式进气道性能,提出了变侧压角与变后掠角+变侧压角两种新型曲面压缩的侧压式进气道设计方案,利用数值仿真手段对其M6、M4下的流场结构及总体性能开展了研究,并与常规平面压缩的侧压式进气道进行了比较。结果表明,曲面压缩的侧压式进气道性能要明显优于常规平面压缩的进气道;采用变后掠角+变侧压角设计的曲面侧压式进气道具有前掠与后掠两种进气道的优点,能显著提高进气道高低马赫数下的性能。计算发现,马赫6设计点下,变后掠角+变侧压角的曲面侧压式进气道流量系数较常规进气道提高4.1%,总压恢复提高5.3%,二者之和为9.4%;马赫4来流条件下,流量系数提高6.3%,总压恢复提高5.4%,二者之和为11.7%。     

On the early phase of relativistic solar particle events: Are there signatures of acceleration mechanism?

Many physical processes precede and accompany the solar energetic particles (SEP) occurrence on the Earth’s orbit. Explosive energy release on the Sun gives rise to a flare and a coronal mass ejection (CME). X-ray and gamma emissions are believed to be connected with flares. Radio emission is signature of disturbances traveling through the corona and interplanetary space. Particles can gain energy both in the flare and the accompanying wave processes. The beginning of the SEP events has the advantage of being the phase most close to the time of acceleration. Influence of interplanetary transport is minimal in the case of first arriving relativistic solar protons recorded by ground based neutron monitors in so called ground-level enhancements (GLE). The early phase of the SEP events attracts attention of many scientists searching for the understanding of particle acceleration. However, they come to the opposite conclusions. While some authors find arguments for coronal mass ejections as a sole accelerator of SEPs, others prove a flare to be the SEP origin. Here, the circumstances of SEP generation for several GLEs of the 23rd solar cycle are considered. Timing of X-ray, CME, and radio emissions shows a great variety from event to event. However, the time of particle ejection from the Sun is closer to maximum of X-ray emission than to any other phenomena considered. No correlation is found between the particle fluxes and the CME characteristics.     

Large-scale waves in the solar corona: The continuing debate

Ten years after the first observation of large-scale wave-like coronal disturbances with the EIT instrument aboard SOHO, the most crucial questions concerning these “EIT waves” are still being debated controversially – what is their actual physical nature, and how are they launched? Possible explanations include MHD waves or shocks, launched by flares or driven by coronal mass ejections (CMEs), as well as models where coronal waves are not actually waves at all, but generated by successive “activation” of magnetic fieldlines in the framework of a CME. Here, we discuss recent observations that might help to discriminate between the different models. We focus on strong coronal wave events that do show chromospheric Moreton wave signatures. It is stressed that multiwavelength observations with high time cadence are particularly important, ideally when limb events with CME observations in the low corona are available. Such observations allow for a detailed comparison of the kinematics of the wave, the CME and the associated type II radio burst. For Moreton-associated coronal waves, we find strong evidence for the wave/shock scenario. Furthermore, we argue that EIT waves are actually generated by more than one physical process, which might explain some of the issues which have made the interpretation of these phenomena so controversial.     

On the relation of the Forbush decreases detected by ASEC monitors during the 23rd solar activity cycle with ICME parameters

To improve the physical understanding of the Forbush decreases (FD) and to explore the Space Weather drivers, we need to measure as much geospace parameter as possible, including the changing fluxes of secondary cosmic rays. At the Aragats Space Environmental Center (ASEC) are routinely measured the neutral and charged fluxes of secondary cosmic rays. Each of species has different most probable energy of primary “parent” proton/nuclei. Therefore, the energy range of the Galactic Cosmic Rays (GCR) affected by Interplanetary Coronal Mass Ejection (ICME) can be effectively estimated using data of the ASEC monitors. We presented relations of the magnitude of FD observed in different secondary particle fluxes to the most probable energy of the primary protons. We investigate the correlations between the magnitude of FD with the size, speed, density and magnetic field of the ICME. We demonstrate that the attenuation of the GCR flux incident on the Earth’s atmosphere due to passing of the ICME is dependent on the speed and size of the ICME and the magnetic field strength.