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.     

液氮贮箱常压停放实验与数值仿真

为研究低温推进剂的常压停放过程,设计了可视化液氮贮箱实验系统。实验中研究充填率和环境温度对液氮汽化量的影响,并测量贮箱内流体和贮箱外壁面的温度随时间和位置的变化。实验得出贮箱常压停放过程,相变主要在壁面和气液界面产生,并且气枕区存在温度分层,距出口位置越近温度越高;而液体区温度基本一致,处于饱和状态。贮箱外壁面在轴向的温度分布显著不同,处于液体区壁面温度低。运用分子动力学推导出的Hertz-Knudsen公式作为气液相变的传热传质源项,并据实验测得温度边界条件,采用混合物模型对贮箱常压停放状态进行30 min的数值仿真。仿真得到结果显示体积汽化速率与实验数据的偏差在5%以内,液体区的温度仿真与实验的偏差在0.15 K左右。      

航天器分子污染计算方法综述

随着对航天器长寿命、高可靠、高性能要求的不断提高,污染逐渐成为影响任务成功的重要因素之一。数值模拟是评估分子污染的主要手段之一。文章对航天器分子污染计算方法进行了总结,详细介绍了污染源、污染沉积及效应、污染传输的模型以及计算方法。