有理分式正交多项式频响函数模态参数识别

 讨论一种多输入的频域模态参数识别方法。该方法将频响函数表示为具有矩阵系数的有理分式,利用Forsythe 正交多项式减少方程的病态并解耦系统矩阵,随后运用特征值与奇异值分解求解系统的极点与留数。使用欧洲国家航空界广泛使用的GARTEUR 飞机模型进行仿真计算。结果表明:该方法在30 %噪声下仍具有对严重耦合模态的识别能力;振型识别较为准确;适当提高分母阶次能取得更好的识别结果。     

GARTEUR有限元模型修正与确认研究

待修正参数的选择以及修正后模型的质量评估是有限元模型修正的两个重要问题。以欧洲学术界广泛采用的GARTEUR飞机模型为例,利用基于灵敏度分析的模型修正方法,通过仿真算例研究参数选择对模型修正质量的影响,并以试验数据为目标值对有限元模型进行修正与确认。为全面评估模型的修正质量,引入三级标准对修正后有限元模型进行确认。     

结构动力学模型修正的三步策略及其实践

首先构建了由模型结构调整、模型参数修正以及模型确认组成的三步模型修正策略。该方法优于传统模型修正方法的是:在模型修正之初基于误差定位、灵敏度分析以及工程经验进行的模型结构调整可以给出一个适于参数修正的初始有限元模型,从而保证了模型修正的成功。然后,采用三步法针对国际上模型修正的标准考题——GARTEUR19结构动力学模型进行修正,详尽论述了模型结构调整、参数修正以及模型确认的过程,并将修正结果与国外同行的研究结果进行了对比,综合精度与国际先进水平相当,从而验证了三步模型修正策略的有效性。     

计及随机噪声的频域多输入多输出模态参数识别

提出了一种计及随机噪声的多输入多输出频域模态参数识别方法。该方法基于连续时间域的频率响应函数有理分式模型,利用Forsythe正交多项式改善求解性态,属频域的极大似然类估计方法。在最小二乘估计的基础上,利用"先验"的随机噪声信息进行优化迭代的极大似然估计,得到更优的模态参数识别结果。根据Cramer Rao下界不等式,在几乎不增加计算量的情况下获得所识别结果的不确定性信息,提高了模态参数识别的可靠性。采用GARTEUR飞机模型作为仿真算例,对本算法进行了仿真验证。     

基于左矩阵分式模型的模态参数识别方法

提出一种多输入多输出(MIMO)系统的宽频模态参数识别算法。该方法基于频响函数(FRF)的左矩阵分式模型(LMFD),通过最小二乘法在z域内求解模态参数,避免了s域内矩阵的病态问题。针对左矩阵分式模型的特点,给出了一种通过主分量分析(PCA)建立稳定图的方法。指出了传统的频域多参考点(PRFD)方法与基于左矩阵分式模型识别方法之间的关系。最后采用GARTEUR模型仿真算例与飞机模型的实测算例对所提出的方法进行了验证,结果表明该方法具有良好的识别效果。     

模态参数识别的特征系统实现算法:研究与比较

以 GARTEUR飞机模型的飞行颤振和地面共振试验为例,对模态参数识别的特征系统实现算法的4种变形特征系统实现算法(ERA)、快速ERA(FERA)、相关ERA(ERA/ DC)和快速相关ERA(FERA/ DC),进行了深入的理论分析和仿真研究。结果表明:与ERA相比,ERA/ DC的阻尼识别精度在10%和30%噪声下可以提高6～60倍;FERA的识别速度可以比ERA提高4～1 0倍,且精度较高;而FERA/ DC的识别速度可以比ERA/ DC提高 3～5倍,并且精度不会降低。     

基于混合人工鱼群算法的结构有限元模型修正

将模拟退火算法(SAA)与具有交叉和高斯变异的人工鱼群算法(AFSA)相结合,提出了一种基于混合人工鱼群算法(HAFSA)的结构有限元模型修正方法;针对外编有限元模型修正程序直接嵌入Patran/Nas-tran软件存在困难的情况,设计了一种灵巧且方便的接口模块。以试验模型测试数据与有限元模型计算值的向量残差建立目标函数,在基本AFSA中引入交叉和高斯变异算子用于加快全局优化搜索速度,将目标函数优化值不断刷新公告板,再利用SAA进行局部细化搜索从而显著提高优化解的精度,在满足算法终止条件后获得设计参数的最优值;结合Fortran语言和Visual Basic语言编译接口模块,运行模型修正程序时循环修改Patran软件生成的建模文件并反复调用Nastran软件进行求解。以欧洲航空研究科技组织的基准模型——GARTEUR飞机模型为例,修正结果表明,应用HAFSA进行结构有限元模型修正是可行且有效的。     

桨叶实度及轴间距对摆线桨气动特性影响研究

悬停状态下,设计参数和摆线桨间距离对摆线桨的气动特性有较大影响。首先通过算例验证滑移网格计算方法应用于摆线桨悬停状态下气动力计算的准确性,然后研究摆线桨在不同半径、弦长和桨叶数时的气动参数特性,最后计算分析不同距离时,摆线桨间的气动干扰特性。结果表明:随着半径增大,桨叶气动力和单位面积上载荷均增大;弦长越大,气动力越大,桨叶单位面积上载荷反而越小;4叶片摆线桨产生的气动力比3叶片和6叶片大,而3叶片的桨叶载荷最大;合力偏转角分别随转速和实度的增大而减小;随着摆线桨间距离的增加,气动力损失系数和合力偏转角均减小。     

冷轧变形对Inconel 718合金δ相γ″相析出行为的影响

采用X射线衍射技术测定了冷轧Inconel718合金在860℃加热温度下的δ相和γ″相含量,研究了冷轧变形对δ相和γ″相析出行为的影响。结果表明,冷轧变形影响δ相的析出形貌,随冷轧变形量增加,δ相由针状向颗粒状转变。δ相析出的重量百分数与时间的关系符合Avrami方程,随冷轧变形量增加,n值减小,α值增加。在860℃加热温度下,等温15min时已有γ″相析出,随时间增加,γ″相含量增加,达到最大值后又降低。在试验中给定的时间条件下,随冷轧变形量增加,γ″相含量降低,而δ相含量增加。     

Magnetosphere Imaging Instrument (MIMI) on the Cassini Mission to Saturn/Titan

The magnetospheric imaging instrument (MIMI) is a neutral and charged particle detection system on the Cassini orbiter spacecraft designed to perform both global imaging and in-situ measurements to study the overall configuration and dynamics of Saturn’s magnetosphere and its interactions with the solar wind, Saturn’s atmosphere, Titan, and the icy satellites. The processes responsible for Saturn’s aurora will be investigated; a search will be performed for substorms at Saturn; and the origins of magnetospheric hot plasmas will be determined. Further, the Jovian magnetosphere and Io torus will be imaged during Jupiter flyby. The investigative approach is twofold. (1) Perform remote sensing of the magnetospheric energetic (E > 7 keV) ion plasmas by detecting and imaging charge-exchange neutrals, created when magnetospheric ions capture electrons from ambient neutral gas. Such escaping neutrals were detected by the Voyager l spacecraft outside Saturn’s magnetosphere and can be used like photons to form images of the emitting regions, as has been demonstrated at Earth. (2) Determine through in-situ measurements the 3-D particle distribution functions including ion composition and charge states (E > 3 keV/e). The combination of in-situ measurements with global images, together with analysis and interpretation techniques that include direct “forward modeling’’ and deconvolution by tomography, is expected to yield a global assessment of magnetospheric structure and dynamics, including (a) magnetospheric ring currents and hot plasma populations, (b) magnetic field distortions, (c) electric field configuration, (d) particle injection boundaries associated with magnetic storms and substorms, and (e) the connection of the magnetosphere to ionospheric altitudes. Titan and its torus will stand out in energetic neutral images throughout the Cassini orbit, and thus serve as a continuous remote probe of ion flux variations near 20R _S (e.g., magnetopause crossings and substorm plasma injections). The Titan exosphere and its cometary interaction with magnetospheric plasmas will be imaged in detail on each flyby. The three principal sensors of MIMI consists of an ion and neutral camera (INCA), a charge–energy–mass-spectrometer (CHEMS) essentially identical to our instrument flown on the ISTP/Geotail spacecraft, and the low energy magnetospheric measurements system (LEMMS), an advanced design of one of our sensors flown on the Galileo spacecraft. The INCA head is a large geometry factor (G ∼ 2.4 cm² sr) foil time-of-flight (TOF) camera that separately registers the incident direction of either energetic neutral atoms (ENA) or ion species (≥5^∘ full width half maximum) over the range 7 keV/nuc < E < 3 MeV/nuc. CHEMS uses electrostatic deflection, TOF, and energy measurement to determine ion energy, charge state, mass, and 3-D anisotropy in the range 3 ≤ E ≤ 220 keV/e with good (∼0.05 cm² sr) sensitivity. LEMMS is a two-ended telescope that measures ions in the range 0.03 ≤ E ≤ 18 MeV and electrons 0.015 ≤ E≤ 0.884 MeV in the forward direction (G ∼ 0.02 cm² sr), while high energy electrons (0.1–5 MeV) and ions (1.6–160 MeV) are measured from the back direction (G ∼ 0.4 cm² sr). The latter are relevant to inner magnetosphere studies of diffusion processes and satellite microsignatures as well as cosmic ray albedo neutron decay (CRAND). Our analyses of Voyager energetic neutral particle and Lyman-α measurements show that INCA will provide statistically significant global magnetospheric images from a distance of ∼60 R _S every 2–3 h (every ∼10 min from ∼20 R _S). Moreover, during Titan flybys, INCA will provide images of the interaction of the Titan exosphere with the Saturn magnetosphere every 1.5 min. Time resolution for charged particle measurements can be < 0.1 s, which is more than adequate for microsignature studies. Data obtained during Venus-2 flyby and Earth swingby in June and August 1999, respectively, and Jupiter flyby in December 2000 to January 2001 show that the instrument is performing well, has made important and heretofore unobtainable measurements in interplanetary space at Jupiter, and will likely obtain high-quality data throughout each orbit of the Cassini mission at Saturn. Sample data from each of the three sensors during the August 18 Earth swingby are shown, including the first ENA image of part of the ring current obtained by an instrument specifically designed for this purpose. Similarily, measurements in cis-Jovian space include the first detailed charge state determination of Iogenic ions and several ENA images of that planet’s magnetosphere.This revised version was published online in July 2005 with a corrected cover date.     

Deep Impact: Working Properties for the Target Nucleus – Comet 9P/Tempel 1

In 1998, Comet 9P/Tempel 1 was chosen as the target of the Deep Impact mission (A’Hearn, M. F., Belton, M. J. S., and Delamere, A., Space Sci. Rev., 2005) even though very little was known about its physical properties. Efforts were immediately begun to improve this situation by the Deep Impact Science Team leading to the founding of a worldwide observing campaign (Meech et al., Space Sci. Rev., 2005a). This campaign has already produced a great deal of information on the global properties of the comet’s nucleus (summarized in Table I) that is vital to the planning and the assessment of the chances of success at the impact and encounter. Since the mission was begun the successful encounters of the Deep Space 1 spacecraft at Comet 19P/Borrelly and the Stardust spacecraft at Comet 81P/Wild 2 have occurred yielding new information on the state of the nuclei of these two comets. This information, together with earlier results on the nucleus of comet 1P/Halley from the European Space Agency’s Giotto, the Soviet Vega mission, and various ground-based observational and theoretical studies, is used as a basis for conjectures on the morphological, geological, mechanical, and compositional properties of the surface and subsurface that Deep Impact may find at 9P/Tempel 1. We adopt the following working values (circa December 2004) for the nucleus parameters of prime importance to Deep Impact as follows: mean effective radius = 3.25± 0.2 km, shape – irregular triaxial ellipsoid with a/b = 3.2± 0.4 and overall dimensions of ∼14.4 × 4.4 × 4.4 km, principal axis rotation with period = 41.85± 0.1 hr, pole directions (RA, Dec, J2000) = 46± 10, 73± 10 deg (Pole 1) or 287± 14, 16.5± 10 deg (Pole 2) (the two poles are photometrically, but not geometrically, equivalent), Kron-Cousins (V-R) color = 0.56± 0.02, V-band geometric albedo = 0.04± 0.01, R-band geometric albedo = 0.05± 0.01, R-band H(1,1,0) = 14.441± 0.067, and mass ∼7×10¹³ kg assuming a bulk density of 500 kg m⁻³. As these are working values, {i.e.}, based on preliminary analyses, it is expected that adjustments to their values may be made before encounter as improved estimates become available through further analysis of the large database being made available by the Deep Impact observing campaign. Given the parameters listed above the impact will occur in an environment where the local gravity is estimated at 0.027–0.04 cm s⁻² and the escape velocity between 1.4 and 2 m s⁻¹. For both of the rotation poles found here, the Deep Impact spacecraft on approach to encounter will find the rotation axis close to the plane of the sky (aspect angles 82.2 and 69.7 deg. for pole 1 and 2, respectively). However, until the rotation period estimate is substantially improved, it will remain uncertain whether the impactor will collide with the broadside or the ends of the nucleus.     

进口速度分布对钝体稳定器贫油点熄火性能的影响研究

为了探究燃烧室不均匀进口速度分布对燃烧性能的影响,采用试验的方法,开展了0.101MPa,700K进口条件下四种进口速度分布对钝体稳定器贫油点熄火性能的影响研究,结合流场特性分析了贫油点熄火性能变化的原因,四种进口速度分布依次为:h/H=0,3/6, 4/6和5/6 (其中h为速度峰值距离通道底部的高度,H为试验通道的高度)。结果表明:整体而言,均匀进口贫油点熄火性能优于非均匀进口。当h/H=3/6时,贫油点熄火性能最差;而当h/H=5/6时,贫油点熄火性能最优。随着h/H由3/6增大到5/6时,贫油点火当量比下降7.39%,贫油熄火当量比下降18.45%。当进口速度分布为h/H=0和3/6时,钝体稳定器下游回流区基本对称;而当h/H=4/6和5/6时,钝体下游回流区不对称,且每个涡出现主副双涡心,存在流体由一个涡心向另一个涡心流动的现象。同时,当进口速度分布由h/H=3/6增大到h/H=5/6时,钝体下游回流区变长,其特征长度Lvc_A增大14.56%,Lvc_B增大50.70%。     

Investigations of entrainment characteristics and shear-layer vortices evolution in an axisymmetric rear variable area bypass injector

In this study,firstly,for the axisymmetric RVABI,the change-rule of adverse pressure gradient caused by radial velocity during the transition of internal flow mode in variable geometry is summarized,and a Bypass Ratio(BR) iterative algorithm based on the empirical correlation of non-equilibrium pressure is proposed.The algorithm can estimate the nonlinear relationship between area ratio and BR,with an error range falling below 6.5%.Then,we discuss the favorable effect of uniform mixing on the th...     

Understanding stress corrosion cracking behavior of 7085-T7651 aluminum alloy in polluted atmosphere

The electrochemical and Stress Corrosion Cracking (SCC) behaviors of 7085-T7651 aluminum alloy in different environments are studied by electrochemical and mechanical testing. The research shows that the type, concentration of the corrosive medium and electrolyte state affect the electrochemical and SCC controlling processes of aluminum alloys. The Thin Electrolyte Layer (TEL) state and the addition of HSO₃^– increase the corrosion rate and SCC susceptibility. The presence of HSO₃^– in a corrosive environment can significantly accelerate the corrosion rate and mechanical property degradation, and this effect increases with the increase of HSO₃^– concentration. Compared with the solution environment, the TEL environment will further aggravate corrosion and mechanical property degradation. With the increase of HSO₃^– concentration, the pH of the corrosive environment exhibits little change, while the SCC degradation is significantly promoted. This is attributed to the HSO₃^– induced buffer effect and film-assisted stress effect, yielding the overshadowing effect against solution pH.     

求解具有多层试验数据成败型单元混联系统可靠性近似限的信息论方法

研究了求解具有多层成败型试验数据时,系统可靠性置信下限近似解的信息论方法,给出了各层试验数据综合的方法和步骤,推导了各层数据信息论方法折合及综合的计算公式。根据单元试验信息提供的信息量与系统折合试验应提供的信息量相等的原则,将多层试验数据逐级折合为系统的等效成败型数据,导出了等效成败型数据信息论方法折合的基本公式;结合可靠性工程的基本原理,根据单个成败型单元可靠性评定的经典精确置信限方法,给出了系统可靠性置信下限的近似解。并以实例形式说明了该方法的具体应用。     

焊透深度和前进侧位置对FSW 贮箱锁底接头性能的影响

开展了2219MCS 叉形环和2219C10S 短壳组成的锁底接头的搅拌摩擦焊工艺试验,详细分析了

搅拌针长度和前进侧位置对锁底接头Hook 型缺陷、力学性能、断裂方式的影响规律。结果表明:搅拌摩擦焊

锁底接头在短壳一侧存在Hook 型缺陷,短壳位于前进侧时的搭接界面上翘曲率和迁移量均大于叉形环位于

前进侧,且随着搅拌针长度的增加,搭接界面的向上迁移量逐渐增大。相同的焊透深度时,叉形环位于前进侧

的力学性能优于短壳位于前进侧;相同的前进侧位置时,随着焊透深度的逐渐增加,接头力学性能逐渐降低。

锁底接头搭接界面缺陷形貌及迁移量的变化是引起力学性能变化的主要原因。优化的试验结果显示,当焊透

深度和短壳板材厚度相同,且叉形环位于焊缝前进侧的力学性能最优,常温可达到300 MPa,低温可达到370

MPa,延伸率均超过3. 5%。锁底接头的拉伸断裂方式与焊缝前进侧位置密切相关。当短壳位于前进侧时,从

短壳一侧热力影响区断裂;当叉形环为前进侧时,从焊缝焊核区断裂。

     

Effects of Alloying Elements Ti, Cr, Al, and Hf on β-Nb5Si3 from First-principles Calculations

The energy, lattice parameters, electronic structures, and elastic constants of the intermetallic compound β-Nb₅Si₃ alloyed by Ti, Cr, Al, and Hf elements are investigated using first-principles methods based on plane-wave pseudopotential theory. From the impurity formation energy calculated, it is found that Ti, Cr, and Hf prefer to occupy the Nb_I, Nb_I, and Nb_II site, respectively, and that Al decreases the stability of β-Nb₅Si₃. Ti and Cr atoms reduce the c/a ratio of crystal lattices and Hf atom transforms the crystal lattice of β-Nb₅Si₃ from the tetragonal system to the orthorhombic system. The total state density of pure β-Nb₅Si₃ system and Ti, Cr, and Hf doped systems shows that Ti, Cr, and Hf improve the conductibility of β-Nb₅Si₃ system. The bulk modulus, shear modulus, and elastic modulus are obtained using Voight approximation equation. Ti and Cr increase the hardness and reduce the ductility of β-Nb₅Si₃. In contrast, Hf decreases the hardness and improves the ductility.     

Non-linear resonant excitation of whistler mode waves in the Earth's ionosphere

We examine the resonant non-linear interaction in the Earth's ionosphere of two powerful high frequency radio beams with frequencies f ₁ and f ₂ (both larger than the plasma frequency at F2_max) and wave numbers k ₁ and k ₂ such that a whistler mode wave can be excited with a frequency f ₃ = f ₁ — f ₂ and a wave number k ₃ = k ₁ – k ₂. The feasibility of an effective ground based installation, sited at low latitudes, is discussed and the field strength of the wave emerging from a 10 km wide ionospheric region illuminated by the beams is evaluated for a range of transmitted frequencies, beam orientations and plasma frequencies in the interaction region. It is suggested that the longitude dependence of the enhancement of VLF noise bands detected by the Ariel 3 satellite may be due to a non-linear interaction of this type between any two or more medium wavelength signals from areas where there is a high concentration of commercial broadcasting stations, such as the NE region of the U.S.A.     

Energetic Hydrogen and Oxygen Atoms Observed on the Nightside of Mars

We present measurements of energetic hydrogen and oxygen atoms (ENAs) on the nightside of Mars detected by the neutral particle detector (NPD) of ASPERA-3 on Mars Express. We focus on the observations for which the field-of-view of NPD was directed at the nightside of Mars or at the region around the limb, thus monitoring the flow of ENAs towards the nightside of the planet. We derive energy spectra and total fluxes, and have compiled maps of hydrogen ENA outflow. The hydrogen ENA intensities reach 10⁵ cm⁻² sr⁻¹ s⁻¹, but no oxygen ENA signals above the detection threshold of 10⁴ cm⁻² sr⁻¹ s⁻¹ are observed. These intensities are considerably lower than most theoretical predictions. We explain the discrepancy as due to an overestimation of the charge-exchange processes in the models for which too high an exospheric density was assumed. Recent UV limb emission measurements (Galli et al., this issue) point to a hydrogen exobase density of 10¹⁰ m⁻³ and a very hot hydrogen component, whereas the models were based on a hydrogen exobase density of 10¹² m⁻³ and a temperature of 200 K predicted by Krasnopolsky and Gladstone (1996). Finally, we estimate the global atmospheric loss rate of hydrogen and oxygen due to the production of ENAs.