1+1/2级超跨声对转涡轮气动性能试验及分析

对转涡轮是高性能航空发动机的关键技术之一。采用试验方法对某1+1/2级超跨声对转涡轮气动性能进行了研究与分析。针对试验中涡轮级间难以布置测点的问题,提出了基于特性反推的分步试验方法,然后对超跨声对转涡轮运行特性进行了详细分析。研究结果表明,该超跨声高压涡轮流量特性几乎不随膨胀比变化,而效率特性变化较大;高、低压涡轮喉道面积比在涡轮膨胀比分配中起到重要作用,该值低于设计状态时,总膨胀比满足设计要求下,高压涡轮膨胀比增大,低压涡轮膨胀比减小;高压涡轮出口气流角对低压涡轮运行特性影响显著。     

半球谐振陀螺精密集成组装技术探讨

半球谐振陀螺零件制造的高精度和对称性是保障产品性能指标的关键,当前制造技术的短板是制约半球谐振陀螺性能指标提升、高合格率和低成本制造,以及批量生产的主要原因之一,集成组装是半球谐振陀螺制造过程的关键环节。因此提出了面向半球谐振陀螺装配的"六心一线"目标,即半球谐振子几何球心、质量中心、谐振中心、激励罩的激励电极中心、读出基座输出检测中心以及形成的静电场中心必须做到同心、同轴,探讨了保证"六心一线"的集成装调技术,为保障半球谐振陀螺的装配精度、性能和装配合格率提供技术支持。     

试论民用飞机选型程序

飞机选型的最终目的是为航空公司选择一个最满意的机群。它从每个城市对子之间的航班对飞机的优选开始,综合公司全部航班选型结果,从中挑选不同的若干机型组合,形成不同的机群方案;再评估这些方案,选取其中最为满意的一个。本文就如何进行民用飞机和机群的优选进行了探讨,并提出了一个“飞机选型程序框图”。     

来流扰动对圆盘绕流结构影响的实验研究

主要讨论由水槽流动显示实验得到的圆盘绕流结构在上游小圆柱尾迹干扰下的变化,对圆盘前驻点附近逆压区的流动通过氢气泡显示技术进行观察.由实验结果处理得到圆盘前大涡的结构特征(如周期、最大宽度、在周期内结构随时间的变化等)受扰动几何参数的影响.发现无量纲参数L/d(L为小圆柱中心与圆盘迎风面之间的间距,d为小圆柱直径)对圆盘前驻点区域中大涡的形成和发展有重要的影响.圆柱尾迹中涡通量的增加会在圆盘前产生大尺度的涡对,其周期性演化的频率随L/d增加而增加.     

不可压缩平板边界层转捩中突变过程的数值模拟

采用时间模式对不可压平板边界层从层流到湍流的转捩过程进行了直接数值模拟.分析结果表明:在层流-湍流转捩的突变过程开始之前,已经产生非线性作用;二维波与三维波的幅值实际增长率也偏离线性状态,而且在二者之间存在能量转移的迹象.在突变过程中,速度变形率对总应力的影响较大,在转捩结束后雷诺应力对总应力的影响比较显著.研究表明:正是由于大量谐波被快速激发并增大,导致了雷诺应力及其法向梯度也快速增大.这使得平均流剖面快速被修正,流动快速转为湍流.      

The Composition of the Solar Wind in Polar Coronal Holes

The solar wind charge state and elemental compositions have been measured with the Solar Wind Ion Composition Spectrometers (SWICS) on Ulysses and ACE for a combined period of about 25 years. This most extensive data set includes all varieties of solar wind flows and extends over more than one solar cycle. With SWICS the abundances of all charge states of He, C, N, O, Ne, Mg, Si, S, Ar and Fe can be reliably determined (when averaged over sufficiently long time periods) under any solar wind flow conditions. Here we report on results of our detailed analysis of the elemental composition and ionization states of the most unbiased solar wind from the polar coronal holes during solar minimum in 1994–1996, which includes new values for the abundance S, Ca and Ar and a more accurate determination of the ²⁰Ne abundance. We find that in the solar minimum polar coronal hole solar wind the average freezing-in temperature is ∼1.1×10⁶ K, increasing slightly with the mass of the ion. Using an extrapolation method we derive photospheric abundances from solar wind composition measurements. We suggest that our solar-wind-derived values should be used for the photospheric ratios of Ne/Fe=1.26±0.28 and Ar/Fe=0.030±0.007.     

Johannes Geiss’ Investigations of Solar, Heliospheric and Interstellar Matter

Johannes Geiss is a world leader and foremost expert on measurements and interpretation of the composition of matter that reveals the history, present state, and future of astronomical objects. With his Swiss team he was first to measure the composition of the noble gases in the solar wind when in the late 1960s he flew the brilliant solar wind collecting foil experiments on the five Apollo missions to the moon. Always at the forefront of the art of composition measurements, he with his colleagues determined the isotopic and elemental composition of the solar wind using instruments characterized by innovative design that have provided the most comprehensive record of the solar wind composition under all solar wind conditions at all helio-latitudes. He discovered heavy interstellar pickup ions, from which the composition of the neutral gas of the Local Interstellar Cloud is determined, and the “Inner Source” of pickup ions. Johannes Geiss played a key role both in the in-situ measurements and modeling of molecular ions in comets, and the interpretation of these data. He and co-workers measured the composition of plasmas in the magnetospheres of Earth and Jupiter. Here we highlight Johannes Geiss’ many discoveries and seminal contributions to our knowledge of the composition of matter of the Sun, solar wind, interstellar gas, early universe, comets and magnetospheres.     

An Update on Ultra-Heavy Elements in Solar Energetic Particles above 10 MeV/Nucleon

Measurements below several MeV/nucleon from Wind/LEMT and ACE/ULEIS show that elements heavier than Zn (Z=30) can be enhanced by factors of ∼100 to 1000, depending on species, in ³He-rich solar energetic particle (SEP) events. Using the Solar Isotope Spectrometer (SIS) on ACE we find that even large SEP (LSEP) shock-accelerated events at energies from ∼10 to >100 MeV/nucleon are often very iron rich and might contain admixtures of flare seed material. Studies of ultra-heavy (UH) SEPs (with Z>30) above 10 MeV/nucleon can be used to test models of acceleration and abundance enhancements in both LSEP and ³He-rich events. We find that the long-term average composition for elements from Z=30 to 40 is similar to standard solar system values, but there is considerable event-to-event variability. Although most of the UH fluence arrives during LSEP events, UH abundances are relatively more enhanced in ³He-rich events, with the (34<Z<40)/O ratio on average more than 50 times higher in ³He-rich events than in LSEP events. At energies >10 MeV/nucleon, the most extreme event in terms of UH composition detected so far took place on 23 July 2004 and had a (34<Z<40)/O enhancement of ∼250–300 times the standard solar value.     

Long-Term Fluences of Solar Energetic Particles from H to Fe

Data from ACE and GOES have been used to measure Solar Energetic Particle (SEP) fluence spectra for H, He, O, and Fe, over the period from October 1997 to December 2005. The measurements were made by four instruments on ACE and the EPS sensor on three GOES satellites and extend in energy from ∼0.1 MeV/nuc to ∼100 MeV/nuc. Fluence spectra for each species were fit by conventional forms and used to investigate how the intensities, composition, and spectral shapes vary from year to year.     

基于视线矢量的深空自主导航算法研究

针对深空探测器在行星际飞行的轨道确定问题, 研究了一种基于视线矢量的自主导航算法. 结合深空探测任务的特点, 以太阳视线矢量和地球视线矢量作为导航系统的观测量, 在详细分析太阳敏感器测量原理的基础上, 给出了太阳视线矢量的观测模型及其观测误差表达式. 通过分析导航相机观测原理, 给出像元像线观测模型, 并推导了地球视线矢量的观测误差. 根据惯性空间内视线矢量间的几何关系, 详细推导了探测器的位置矢量及其误差表达式, 结合非线性扩展卡尔曼滤波建立自主导航算法. 利用深度撞击任务的实际飞行数据对本文提出的深空自主导航算法进行了仿真验证.