模糊逻辑系统建模函数的数学描述

基于所建立的模糊规则定义式,由一组“如果一则”规则构造出模糊逻辑系统,按真值化处理与推理规则推导出最优系统数学表达式,在线性定常状态下,分别建立起连续与间断时间系统的数学模型,归纳出模糊控制的等效解法。最后,对一非线性实例绘制出双模控制框图,应用了模糊数学算法。     

舰载飞机对动力装置特殊要求的分析（下）

3 舰载机动力装置特殊要求 由于舰载飞机在起飞、着舰、作战使用和外界环境及停放和维护等方面与陆基飞机有很大不同,所以对其装配的动力装置就有许多特殊要求。这些要求概括起来就是:“一高”、“二降”、“三抗”、“四防”、“五性”等15项要求。 “一高”,就是固定翼舰载机发动机比同量级陆基飞机发动机要有更高的推力,一般要高12％～19％;而旋翼机的动力装置要有     

大型客机驾驶舱/客舱振动舒适性评估

通过某大型客机飞行测试,获得驾驶舱/客舱典型区域振动环境。根据ISO 2631-1:1997标准规定的频率计权加速度计算方法,对滑跑、起飞、爬升、巡航、下降、着陆和滑行等7种典型状态下,驾驶舱飞行员座椅和客舱前/中/后排座椅位置处的全身振动(WBV)加速度均方根值进行了计算与分析。依据标准中的计权加速度与舒适性等级对照关系,对各状态/各区域的人体振动舒适性进行了评估。结果表明,客舱在不同飞行状态不同区域的振动舒适性等级不同。从飞行阶段来看,在滑跑、爬升、巡航、下降和滑行阶段,所有舱位基本处于“没有不舒适”或“有点不舒适”等级,尤其是占据客机大部分飞行时间的巡航阶段,所有舱位都达到“没有不舒适”等级。但起飞和着陆阶段,所有舱位振动舒适性较差,驾驶舱和后排只得到了“非常不舒适”的评估等级;从舱位分布来看,中排区域的振动舒适性最佳,在大多飞机阶段都达到了“没有不舒适”或“有点不舒适”评估等级。前排区域舒适性也相对较好,只有在着陆阶段降为“不舒适”等级,而驾驶舱和后排相对较差,特别是驾驶舱在滑跑、起飞和着陆阶段,只得到“不舒适”或“非常不舒适”的评估等级。     

飞机惯性熔断器正负极性问题探讨

一、概述 熔断器的“正负极性”,指电源正负极必须按规定接在熔断器标有“ ”、“-”符号的接线端上,否则其工作特性将发生重大改变。 “正负极性”对某些直流熔断器(例如GB型惯性熔断器)的安—秒特性有严重影响,故HB 6-81-78《飞机熔断器技术条件》第3条对“正负极性”特别作了明确规定。     

武器装备研制中的质量监督效能研究

开展航空电子系统设备及武器装备研制的可靠性、维修性、测试性、安全性、保障性及环境适应性（“六性”）质量监督工作是提高装备质量的重要途径。分析了开展“六性”质量监督工作面临的困难和问题,并对提升“六性”质量监督工作效能提出了对策和建议。     

幂指函数在非线性规划中的应用

给出一种自适应近似函数－幂指函数f^-(x)在非线性规划中的收敛算法。它采用minx∈Enf^-(x)的最优解序列｛x^-｝去逼近原问题minx∈Enf^-(x)的最优解x^*.与传统优化算法相比：该算法最优解｛x^-｝可以通过f^-x(x)=0直接解析得出；该算法不要求序列｛f(x)^k｝具有单调减特性，却能够保证算法的收敛性，该算法的计算量对变量的维数不敏感，从而具有广泛的应用前景，从方法论上，它是采用“特殊非线性”来研究“一般非线性”的一种新方法。     

通用质量特性在航空装备修理中的应用研究

介绍了可靠性、维修性、保障性、测试性、安全性和环境适应性的概念及相关标准,分析了通用质量特性在装备研制与装备修理中的差异,在装备修理中对“六性”进行了解析,简述了重点分析控制方向,明确了装备修理中的“六性”组织环境、管理改进、项目实施,落地于识别与控制措施,确保“六性”分析有计划、过程受控、有实施效果。     

样本均值的随机加权逼近之必要条件

本证明了样本均值的随机加权统计量几乎处处有效的必要条件为EX^2<∞；若将“几乎处处”条件削弱为“依概率”，则必有X属于正态分布的吸收域。     

“隼”900EX挑战超远程公务机

几年前,达索公司曾认真考虑过推出三发超远程商务喷气机——“隼”9000.但在准备投资10亿美元起动该项目之前,达索公司的工程师和项目主管经过认真的市场调查,认为超远程公务机市场比较受限制,一架超远程公务机进行最大航程飞行的机会可能只有5%～10%.在考虑到拥有成本和营运成本等综合因素之后,认为航程为4500海里的三发“隼”900EX能达到性能、灵活性、舒适性和效率等方面最佳综合指标.因此,达索公司推出了更实用的“隼”900EX——一种远程、性     

平均数与统计离差的哲学思考

通过平均数与统计离差之间关系的研究，论述了马克思主义哲学中的“对立统一”观点“矛盾的偶然性与必然性”等理论在统计学中的广泛应用。     

The effect of rotation on the hydrodynamics of stellar collapse

Summary Using values of d, _min, and _max that Van Riper (1978) has found most promising for a hydrodynamic envelope ejection, we have shown that even a small amount of rotation in the initial core can stop its collapse before nuclear densities are reached. We expected _i > 0.02 to produce significant deviations from a spherically symmetric collapse, but have found that _i as much as ten times smaller than this will not allow the core to reach densities as high as in the spherical collapse. In no case, however, does the core flatten very much, nor does the value of become very large. Low final 's preclude the formation of an axisymmetric torus. They also indicate that deformation of an iron core into a triaxial configuration or fragmentation of the core during its collapse is an extremely unlikely event. (Note: Classically, must exceed 0.27 before a dynamic instability to non-axisymmetric perturbations is encountered.)The small degree of flattening of the core also suggests that the reduced moment of inertia I of the core will always be relatively small in magnitude and hence that the third time derivative of I, which is proportional to the energy emitted in gravity wave radiation, will not be very significant. Numerically calculated estimates of I- during some of these model evolutions supports this suspicion. If the _min and used here are found to be realistic values after the detailed physics of the core collapse is well understood, it is clear that gravitational radiation from a core collapse will be difficult to measure.Finally, we should point out that it is the relatively large values of Y_min (near 4/3) combined with values of d near unity that (a) prevented the core from flattening significantly in these models and (b) prevented the core from reaching high configurations. If realistic values of either one (or both) of these parameters are found to be much smaller in more complete models of the core collapse, then the core will have to become flatter (and denser) before pressure gradients will support it along the rotation axis. All of the conclusions drawn here would be modified accordingly under those circumstances. It should also be noted that in general relativistic models, the critical for spherical collapse is somewhat larger than 4/3 (Van Riper, 1979). Therefore, we predict that when fully general relativistic core collapses are performed including rotation, a given choice of _min and _i will produce a slightly flatter and slightly denser core than the corresponding model that has been presented here.     

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.     

Characteristics of nearby interstellar matter

There is a warm tenuous partially ionized cloud (T10⁴ K,n(HI)0.1 cm^–3,n(Hii 0.22–0.44 cm^–3) surrounding the solar system which regulates the environment of the solar system, determines the structure of the heliopause region, and feeds neutral interstellar gas into the inner solar system. The velocity (V–20 km s^–1 froml335°,b0° in the local standard of rest) and enhanced Caii and Feii abundances of this cloud suggest an origin as evaporated gas from cloud surfaces in the Scorpius-Centaurus Association. Although the soft X-ray emission attributed to the Local Bubble is enigmatic, optical and ultraviolet data are consistent with bubble formation caused by star formation epochs in the Scorpius-Centaurus Association as regulated by the nearby spiral arm configuration. The cloud surrounding the solar system (the local fluff) appears to be the leading region of an expanding interstellar structure (the squall line) which contains a magnetic field causing polarization of the light of nearby stars, and also absorption features in nearby upwind stars. The velocity vectors of the solar system and local fluff are perpendicular in the local standard of rest. Combining this information with the low column densities seen towards Sirius in the anti-apex direction, and the assumption that the cloud velocity vector is parallel to the surface normal, suggests that the Sun entered the local fluff within the historical past (less than 10 000 years ago) and is skimming the surface of the cloud. Comparison of magnesium absorption lines towards Sirius and anomalous cosmic-ray data suggest the local fluff is in ionization equilibrium.Reason has moons, but moons not hers, Lie mirror'd on her sea, Confounding her astronomers, But, O! delighting me.Ralph Hodgson     

Theoretical studies of the flux and energy spectrum of gamma radiation from the Sun

The purpose of this work is to study the various -ray-production mechanisms in solar flares and to calculate the flux, the spectrum, and the decay curves of radiation. Using the continuity equation and taking into account the energy losses for solar-flare-accelerated particles, we obtain the time-dependent particle distribution and thus the time behavior of the resulting rays. The important processes for producing rays in solar flares are found to be nonthermal electron bremsstrahlung, decay of neutral mesons, positron annihilation, neutron capture, and decay of excited nuclei. The results are applied to several known solar flares. For a large flare such as the class 3⁺ on February 23, 1956, continuous rays with energies up to 100 MeV from electron bremsstrahlung and neutral meson decays are observable at the orbit of the Earth by existing -ray detectors. Line rays from positron annihilation (0.51 MeV), neutron capture (2.23 MeV), and deexcitation of excited nuclei O¹⁶ (6.14 and 7.12 MeV) and C¹² (4.43 MeV) are particularly strong and well above the continuous -ray background due to electron bremsstrahlung. These lines can be detected at the Earth.NASA-NRC Resident Research Associate.     

The astrophysical interest of EUV observations of extra-solar objects

The feasibility of observation of EUV sources is assessed. Many stars have been detected in the EUV range ( 100–1000); line fluxes from others can be predicted. Selected astrophysical problems are reviewed that can benefit from EUV spectroscopy. Included among them are the physics and dynamics of stellar coronae, confirmation of nuclear surface burning on cataclysmic variables, evolutionary properties of white dwarfs, the helium abundance in the interstellar medium, and spectroscopic signatures of neutrino oscillations.Proceedings of the Conference Solar Physics from Space, held at the Swiss Federal Institute of Technology Zurich (ETHZ), 11–14 November 1980.     

High-resolution observations of Hα flare regions

This paper gives a review of the recent high-resolution H observations of solar flares and flare-productive active regions. From studies of the morphological and evolutional features of H flare emitting regions, two types of two-ribbon flares, which are termed separating two-ribbon flare and confined two-ribbon flare, are discussed. The former is characterized by conspicuous separating motions or expanding motions of the H two ribbons, whereas the latter shows only a short range of or no separating motions of the two ribbons. The explosive compact flares, which occur in some compact newly-emerging flux regions, are also discussed.Attention is paid to the successive and impulsive brightenings of H flare points which form the H flare kernels and the front lines of H two ribbons at the impulsive phases of flares. Temporal relationships between H line intensities or profiles and hard X-ray or microwave emissions are discussed to discriminate the energy transport mechanisms in the flare loops.H monochromatic image of high spatial resolution, at the present time, is the most sensitive detector for finding the first appearance of newly-emerging magnetic flux region and the developing features of sheared configuration of magnetic field, both of which are the key factors in flare energy build-up processes. It is suggested that the successive emergence of a twisted magnetic flux rope might be essential for the production of a major flare.Contributions from the Kwasan and Hida Observatories, Kyoto University, No. 292.     

Nonlinear theory of the two-point correlation function

We consider the influence of the nonlinear stage of gravitational instability on the two-point correlation functions of gravitationally bound objects. Based on the theory of nonlinear gravitational contraction of a single density peak of dissipationless matter (Gurevich and Zybin, 1988a,b; 1990) we develop a method for calculating the two-point correlation functions of different objects of any mass. The method works good in the region of strong correlations and can be easily extended to calculate higher correlation functions. We show that the main contribution to the correlation function _i in the region of strong correlations _i 1 is made by pair systems located outside large clusters of objects. In this region the shape of _i is determined only by the nonlinear dynamics of gravitational contraction of dissipationless matter and has the form _i C ^–, where 1.8 is a universal parameter.     

先进舰载战斗机强度设计技术发展与实践

舰载战斗机是航空母舰上的主要武器,为满足舰面起飞、着舰和停放等要求,舰载机需围绕起落架系统、拦阻钩系统和翼面折叠系统等"特征结构"进行设计。先进舰载战斗机着舰冲击能量是陆基飞机的6倍以上、拦阻带来的水平载荷超过陆基飞机的15倍,因此特征结构的高载荷对强度设计提出了更高的要求。围绕舰载机"特征结构"及"特征载荷",开展了主要的设计工作,包括："特征载荷"计算,即起落架载荷、拦阻载荷和折叠载荷计算;"特征结构"的强度设计及试验验证,包括起落架系统、拦阻系统、翼面折叠系统的动力学仿真计算、静/疲强度分析、折叠翼面的非线性颤振分析以及综合试验验证;"特征载荷"对其他机体结构强度的影响分析,包括着舰载荷对起落架支撑结构强度的影响、拦阻载荷对后机身支撑结构强度的影响、拦阻着舰的全机动力学响应以及着舰载荷与拦阻载荷的共同作用对全机结构强度的影响;体现舰载机"特征结构"强度特点的试验验证方法等。上述研究成果已成功应用于先进舰载战斗机设计中。     

Determination of the characteristics of the gamma-ray telescope Gamma-1

The Gamma-1 telescope has been developed through a collaboration of scientists in the USSR and France in order to conduct -ray astronomical observations within the energy range from 50 to 5000 MeV. The major characteristics of the telescope were established by Monte-Carlo simulations and calibrations made with the aid of electron and tagged -ray beams produced by an accelerator, and these have been found to be as follows: the effective area for photons coming along the instrument's axis varies from about 50 cm² at E = 50 MeV to approximately 230 cm² at E 300 MeV; the angular resolution (half opening of the cone embracing 68% events) is equal to 2.7° at E = 100 MeV, and 1.8° at E = 300 MeV; the energy resolution (FWHM) varies from 70% to 35% as the energy of the detected photons increases from 100 to 550 MeV; the telescope's field-of-view at the half-sensitivity level is 300–450 square degrees depending upon the spectrum of the detected radiation, and the event selection logic. Proceeding from the thus obtained characteristics it is demonstrated that a point source producing a photon flux J (E 100 MeV) = 3 × 10^-7 cm^-2 s^-1, can be detected with a 5 significance by observing it during 10⁶ s at the level of the Cygnus background, and a source having intensity J (E 100 MeV) = 10^-6 cm^-2 s^-1 can be detected to within a mean square positional accuracy of about 15.     

Latitude and solar-cycle dependence of radial IMF intensity

I describe a simple procedure for extrapolating the observed solar magnetic field into the heliosphere, which averages the asymptotic fields computed using the standard source surface and current sheet models. The resultant field is characterized by strong latitudinal gradients (maintained by volume currents outside the source surface) and by abrupt reversals in direction at the current sheets. The model yields good agreement with the observed long-term variation of the radial IMF component in the ecliptic, and is used to predict the variation of |B _r | along the latitudinal trajectory of Ulysses during 1990–1994. As found in earlier studies, the magnitude ofB _r at any latitude is determined largely by the strength and relative orientation of the Sun's dipole moment.