翩蝶重生——意大利S.211/M.311发展概略

<正>依靠MB 326和MB 339等成功之作跻身世界前沿,在轻型喷气式教练机领域滚打多年的意大利马基航空公司曾经创造了一个时代的辉煌,时至今日实力不减,依然有足够的资本傲视群雄。除了凭借着M 346这一"借腹生子"的后起之秀,在21世纪之初继续领跑国际高级教练机市场外,还极力打造另一款中低端喷气教练机藉以分食剩余份额,这就是本文的的两大主角——马基S.211和阿莱尼亚M.311。     

单向碳/碳复合材料高温疲劳试验研究

为了研究单向碳/碳的高温疲劳特性,从疲劳损伤力学出发,提出了考虑温度、氧化速率的碳/碳复合材料剩余刚度、剩余强度模型,并开展了碳/碳复合材料[0]16单向板试验件在室温、有涂层700℃和无涂层700℃的拉/拉疲劳试验和剩余强度试验。试验结果表明:单向碳/碳复合材料的剩余刚度曲线呈倒"S"形,材料的刚度退化存在三个阶段;单向碳/碳复合材料在室温和有抗氧化涂层700℃的疲劳加载初期和末期存在刚度突降,中期的刚度无明显退化;单向碳/碳复合材料在室温的疲劳刚度退化小于10%,而有抗氧化涂层单向碳/碳复合材料700℃的刚度退化超过30%;无抗氧化涂层单向碳/碳复合材料在疲劳中期存在明显刚度退化,末期无刚度突降。模型的拟合结果表明:复合材料高温剩余刚度、剩余强度模型能够很好地预测单向碳/碳复合材料在室温和700℃的剩余刚度、剩余强度变化。     

欠发达地区社会资本与农民政治参与研究——以苏北为例

社会资本是一种无形的资源,其强调的"信任、网络和规范"对农民政治参与具有普遍的促进作用。"信任"为政治参与提供精神支持,"网络"为政治参与提供载体支持,"规范"为政治参与提供保障。目前我国欠发达地区农村的这些社会资本存在严重缺失的现象。文章通过对苏北地区农村的实地调查,指出这种社会资本缺失对农民政治参与在选举、决策、管理、监督方面的制约,认为只有促进农村社会资本的发育,才能提高农民政治参与的愿望与行为。具体的途径包括:提高农民文化素质,增加个人可用资源,进而增强集体可用的社会资本;乡村干部在执行上级决策时还应兼顾村民意志,以此增加"信任"资本;充分发挥农村合作组织在社会资本建设中的作用,使农民的"私权"加以整合,使其面对"公权力"时获得平等话语权,同时增强农民的凝聚力;加强法制建设,通过发展"规范",引导、完善农民的政治参与,促进农民的民主决策、民主管理、民主监督。     

民用飞机APU非包容转子碎片对机体结构损伤分析

服役数据表明,民用飞机辅助动力装置在运行中发生破坏时可能产生非包容的高能转子碎片。本文总结了机体结构受非包容转子碎片损伤的评估方法。根据FAA咨询通告中的"小碎片"模型,绘制非包容转子影响区域包络图;对于处于受影响区域中的结构件,通过作图法确定结构件的平动风险角,从而确定结构受影响的严重情况;对应严重情况,建立机体剩余结构有限元模型,施加剩余载荷,计算剩余结构内力解,对剩余结构进行强度分析。     

国企改革:从搞活国有企业转向盘活国有资产

国有企业改革,特别是国有产权改革,是我国深化经济体制改革进程中的难点问题.文章认为,以往的改革主要注重于搞活国有企业,违背了市场经济中决定企业成活率的大数定理,因而注定无法获得较高的绩效.今后要以盘活国有资产为出发点,为此,必须厘清一些基本观念,不能将国有资产流失和国有资产缩水划等号;资本的社会化可以解决困扰国企的剩余索取权问题;资本的社会化可以有效解决国企的内部治理结构问题;公有制的实现形式应该是混合所有制;社会主义公有制的优越性,主要表现在政府保证社会福利提高的层面,政府对社会控制力的加强主要体现在税收领域.     

剩余浮力对系留气球静平衡特性的影响分析

在进行系留气球总体方案设计时,剩余浮力的选择直接影响到系留气球气囊和副气囊体积等参数的设计,剩余浮力选择不当将造成研制成本的增加或静平衡特性指标无法实现。因此,对同一系留气球不同剩余浮力,及两种不同体积的系留气球在相同剩余浮力时的静平衡特性进行计算与对比分析。结果表明:对同一体积的系留气球,剩余浮力对系留气球俯仰角、高度损失和水平漂移量影响较大,且剩余浮力越大,其俯仰角、高度损失和水平漂移量越小;随着系留气球体积的增大,剩余浮力对系留气球高度损失和水平漂移量的影响将逐渐减小。     

缠绕复合材料壳体低速冲击后剩余强度影响因素分析

为探索不同因素对缠绕复合材料壳体低速冲击后剩余强度的影响规律,开展了不同冲击能量、不同冲击部位下壳体的低速落锤试验和水压爆破试验,采用改进的Hashin准则和牵引分离准则模拟复合材料层内和层间损伤,建立了壳体冲击后剩余强度有限元模型,实现了冲击后剩余强度的一体化仿真分析。利用该模型计算得到的缠绕复合材料壳体低速冲击后剩余强度与试验结果一致性较好。最后研究了冲击部位、初始内压、冲头尺寸等因素对壳体冲击后剩余强度的影响规律。研究结果表明:封头赤道圆处为壳体的最薄弱冲击部位,冲击能量为25J时壳体剩余强度降低了约60%;壳体冲击后剩余强度随内压增加而增大,但当内压大于16MPa时,壳体冲击后剩余强度随内压增大而迅速降低;冲头直径在8~16mm变化时,壳体冲击后剩余强度随着冲头直径的减小而降低。     

“科曼奇“直升机研发项目被取消的综合分析

美国陆军2004年2月23日宣布,取消总预算高达390亿美元的RAH-66"科曼奇"武装侦察直升机研发项目.美陆军表示,"科曼奇"项目的剩余资金将被用于升级和扩大现有直升机战斗群,以提高陆军的快速反应和打击能力.本文介绍了"科曼奇"直升机的研制概况,分析了"科曼奇"项目取消的原因,同时阐述了"科曼奇"研发项目虽被取消但其价值还在.     

"白酒护肝",学术成果还是商业宣传?

在各种信息传播中,老百姓更相信学术研究、更相信专家学者.然而,近年来一股学术研究"商业化"的倾向在蔓延,"资本影响学术"的歪风越刮越滥.     

基于EM-KF算法的直升机主减速器剩余寿命预测方法

为解决间接状态监测数据下直升机主减速器剩余寿命预测难以估算的难题,提出了一种卡尔曼滤波和期望最大化算法相结合的剩余寿命预测方法.该方法可以根据不断更新振动信号特征值迅速且有效地估计出模型参数,进而预测不同运行时间主减速器的剩余寿命分布,最后对主减速器试验数据进行了案例分析.结果表明:该方法能够有效估计主减速器的剩余寿命分布,通过与主减速器剩余寿命准确值对比发现,剩余寿命准确值绝大多数落于剩余寿命预测值的95%置信区间内,表明该方法具有好的准确性,进而避免故障的发生.      

Anomalous Cosmic Rays and Solar Modulation

We review aspects of anomalous cosmic rays (ACRs) that bear on the solar modulation of energetic particles in the heliosphere. We show that the latitudinal and radial gradients of these particles exhibit a 22-year periodicity in concert with the reversal of the Sun's magnetic field. The power-law index of the low energy portion of the energy spectrum of ACRs at the shock in 1996 appears to be -1.3, suggesting that the strength of the solar wind termination shock at the helioequatorial plane is relatively weak, with s 2.8. The rigidity dependence of the perpendicular interplanetary mean free path in the outer heliosphere for particles with rigidities between 0.2 and 0.7 GV varies approximately as R2, where R is particle rigidity. There is evidence that ACR oxygen is primarily multiply charged above 20 MeV/nuc and primarily singly-charged below 16 MeV/nuc. The location of the termination shock was at 65 AU in 1987 and 85 AU in 1994.     

Non-BBN Constraints on the Key Cosmological Parameters

Since the baryon-to-photon ratio 10 is in some doubt at present, we ignore the constraints on 10 from big bang nucleosynthesis (BBN) and fit the three key cosmological parameters (h, M, 10) to four other observational constraints: Hubble parameter (ho), age of the universe (to), cluster gas (baryon) fraction (fo fGh3/2), and effective shape parameter (o). We consider open and flat CDM models and flat CDM models, testing goodness of fit and drawing confidence regions by the 2 method. CDM models with M = 1 (SCDM models) are accepted only because we allow a large error on ho, permitting h < 0.5. Open CDM models are accepted only for _M 0.4. CDM models give similar results. In all of these models, large 10 ( 6) is favored strongly over small 10 ( 2), supporting reports of low deuterium abundances on some QSO lines of sight, and suggesting that observational determinations of primordial 4He may be contaminated by systematic errors. Only if we drop the crucial o constraint are much lower values of M and 10 permitted.     

The Edison infrared space observatory

For five years, theEdison program has had the goal of developing new designs for infrared space observatories which will break the cost curve by permitting more capable missions at lower cost. Most notably, this has produced a series of models for purely radiative and radiative/mechanical (hybrid) cooling which do not use cryogens and optical designs which are not constrained by the coolant tanks. Purely radiatively-cooled models achieve equilibrium temperatures as low as about 20 K at a distance of 1 AU from the sun. More advancedEdison designs include mechanical cooling systems attached to the telescope assembly which lower the optical system temperature to 5 K or less. Via these designs, near-cryogenic temperatures appear achievable without the limitations of cryogenic cooling. OneEdison model has been proposed to the European Space Agency as the next generation infrared space observatory and is presently under consideration as a candidate ESA Cornerstone mission. The basic design is also the starting point for elements of future infrared space interferometers.     

Temperature Fluctuations,H II Region Abundances,and Primordial Helium

There is evidence for temperature fluctuations in Planetary Nebulae and in some Galactic H II regions. If such fluctuations occur in the low metallicity, extragalactic H II regions used to probe the primordial helium abundance, the derived 4He mass fraction, YP, could be systematically different from the true primordial value. Although this effect could be large, there are no data which allow us to estimate the size of the temperature fluctuations for the extragalactic H II regions. Therefore, we have explored this effect via Monte Carlo simulations of the data in which the abundances derived from a fiducial data set are modified by T chosen from a distribution with 0 T Tmax where Tmax is varied from 500 K to 4000 K.     

The scientific payload of the space-based Solar and Heliospheric Observatory (SOHO)

The space-based Solar and Heliospheric Observatory (SOHO) is a joint venture of ESA and NASA within the frame of the Solar Terrestrial Science Programme (STSP), the first Cornerstone of ESA's long-term programme Space Science — Horizon 2000. The principal scientific objectives of the SOHO mission are: a) a better understanding of the structure and dynamics of the solar interior using techniques of helioseismology, and b) a better insight into the physical processes that form and heat the Sun's corona, maintain it and give rise to its acceleration into the solar wind. To achieve these goals, SOHO carries a payload consisting of 12 sets of complementary instruments which are briefly described here.     

Voyager energetic particle observations at interplanetary shocks and upstream of planetary bow shocks: 1977–1990

The Voyager 1 and 2 spacecraft include instrumentation that makes comprehensive ion (E 28 keV) and electron (E 22 keV) measurements in several energy channels with good temporal, energy, and compositional resolution. Data collected over the past decade (1977–1988), including observations upstream and downstream of four planetary bow shocks (Earth, Jupiter, Saturn, Uranus) and numerous interplanetary shocks to 30 AU, are reviewed and analyzed in the context of the Fermi and shock drift acceleration (SDA) models. Principal findings upstream of planetary bow shocks include the simultaneous presence of ions and electrons, detection of tracer ions characteristic of the parent magnetosphere (O, S, O⁺), power-law energy spectra extending to 5 MeV, and large (up to 100:1) anisotropies. Results from interplanetary shocks include observation of acceleration to the highest energies ever seen in a shock ( 22 MeV for protons, 220 MeV for oxygen), the saturation in energy gain to 300 keV at quasi-parallel shocks, the observation of shock-accelerated relativistic electrons, and separation of high-energy (upstream) from low-energy (downstream) populations to within 1 particle gyroradius in a near-perpendicular shock. The overall results suggest that ions and electrons observed upstream of planetary bow shocks have their source inside the parent magnetosphere, with first order Fermi acceleration playing a secondary role at best. Further, that quasi-perpendicular interplanetary shocks accelerate ions and electrons most efficiently to high energies through the shock-drift process. These findings suggest that great care must be exercised in the application of concepts developed for heliosphere shocks to cosmic ray acceleration through shocks at supernova remnants.     

Primordial Helium and ΔY/ΔZ from H II Regions and from Fine Structure in the Main Sequence Based on Hipparcos Parallaxes

The primordial helium abundance YP is important for cosmology and the ratio Y/Z of the changes relative to primordial abundances constrains models of stellar evolution. While the most accurate estimates of YP come from emission lines in extragalactic H II regions, they involve an extrapolation to zero metallicity which itself is closely tied up with the slope Y/Z. Recently certain systematic effects have come to light in this exercise which make it useful to have an independent estimate of Y/Z from fine structure in the main sequence of nearby stars. We derive such an estimate from Hipparcos data for stars with Z Z and find values between 2 and 3, which are consistent with stellar models, but still have a large uncertainty.     

弹塑性接触有限元分析的凝缩法

 解决弹性接触问题可用一种新的弹塑性接触有限元计算方法,即有限元混合法与弹塑性有限元分析的凝缩法结合而成,能显著地节省计算时间。文中对涡轮盘榫槽与叶片榫头的接触问题进行了计算分析。     

The synthesis of helium and CNO isotopes in massive stars

We present helium and CNO isotopic yields for massive mass-losing stars in the initial mass range 15M M _i 50M . We investigate their dependence on assumptions about mass loss rates, internal mixing processes, and metallicity, and specify the contributions from stellar winds and from supernova ejecta.     

Some results of ionospheric investigations by means of coherent radiowaves emitted by satellites

In this paper we discuss theoretical expressions, determining the difference of Doppler shifts of various coherent radiowave frequencies emitted by a radiator moving in the ionosphere or interplanetary medium. The rotating Doppler effect (Faraday effect) caused by the Doppler shifts ±H of the ordinary and extraordinary waves is also considered. In a three-dimensional inhomogeneous ionosphere, stationary in time (N/t = 0), is determined in the general case, by an equation with three variables. The equation for proper depends only on the local value of the electron concentration N _c around the radiator and on integral values, determining, by means of additional calculations, the angle of refraction or its components, the horizontal gradients of electron concentration N/x and N/y, and in some cases, the integral electron concentration ₀ ^zcN dz. We describe the analysis of the measurements, made with the satellites Cosmos I, II and partially XI, assuming that N/t = N/y = 0, with a two variables equation. The expected errors are considered. The results coincide well for different points (Moscow, The Crimea, Sverdlovsk) and thus agree with the measurements of _H and with height-frequency ionospheric characteristics. The curve giving electron concentration versus height N (z) in the outer ionosphere (above the maximum of F2), shows a new maximum higher than the main maximum of the ionosphere N _MF2 at 120–140 km. At this maximum the value of N (z) is (0.9–0.95) N _MF2. The new data on the large-scale horizontal inhomogeneities of the ionosphere, exceed the previous ones by about a factor 10. By means of the irregular variations of the spectrum W() of the inhomogenous formation is determined. Three unknown constant maxima with values 16 to 18 km, 28 to 32 km and 100 to 120 km are found. The spectrum W () mainly characterizes the local properties of the ionosphere along the orbit of the satellite.