飞机座舱盖载荷谱编制应注意的几个问题

介绍了某型飞机座舱盖载荷谱编制中,采用包括飞行训练大纲和内厂、外场试飞大纲作为飞行剖面编制依据、以飞参数据作为温度载荷原始输入、温度计算以实测结果进行校对以及温度计算采用大气状态的几个应注意的问题。使座舱盖载荷谱更接近飞机使用的真实情况。     

弹射过程座舱盖抛放轨迹的预测

通过分析座舱盖在各个不同抛放阶段的受力关系,并着重考虑了抛放过程中气动系数的修正和铆钉剪切的影响,最终建立了座舱盖抛放轨迹的预测模型.该模型可广泛用于预测不同型号座舱盖在各种飞行状态下的抛放轨迹.算例表明计算结果与实验数据一致,证明了模型的实用性和有效性.     

飞机座舱盖疲劳试验玻璃老化问题处理方法

通过统计海南日照时间和飞机实际暴露时间的方法,确定座舱盖老化试验的曝晒时间;通过测试新、老玻璃的疲劳性能曲线,确定老化玻璃的寿命保持率,继而计算用曝晒后的座舱盖进行疲劳试验的时间。     

座舱盖静载荷数值模拟及其应用

建立了计算飞机座舱盖静载荷的数学模型,并以某型飞机座舱盖为例模拟了不同飞行状态座舱盖内、外表面受力分布,研究了飞机座舱盖载荷随飞行状态改变而变化的趋势,最后部分给出了座舱盖静载荷在座舱盖抛放过程中所起作用的分析.结果表明:(1)在对流层内,座舱盖外表面气动力系数只是飞行马赫数的函数,与飞行高度无关;(2)座舱盖最大静载荷出现在飞行包线最大飞行高度,飞行马赫数为1的位置;(3)大部分飞行状态下,静载荷产生的绕座舱盖后铰点转动力矩都要大于活塞推力所产生力矩.     

飞机座舱盖透明件使用温度的确定

座舱盖透明件使用温度采取飞行实测和近似计算相结合的方法确定。空测温度工作是一项系统工程,既要保证飞行安全,又要取得飞参、温度随时间变化的数据。涉及方案制定、飞机改装、测温电偶的制做、标定及粘贴、数据采集与处理等项工作。1991年A型飞机座舱盖透明件首次成功地实测了M=2.0、H=14～15km、飞行时间为3min的数据。依实测数据修改了温度计算方法。修正后的温度计算值与实测值误差小于5％。计算了典型飞行剖面,确定了A型飞机座舱透明件最高使用温度值为111.1℃。     

飞行过程中座舱盖透明件温度计算分析

介绍了飞机座舱盖透明件飞行过程中温度效应的理论计算方法。通过温度载荷计算结果,分析了气动加热对座舱盖透明件产生热应力的影响,为飞机座舱盖透明件疲劳定寿中考虑其影响提供了思路和方法。     

某型飞机新旧座舱盖有机玻璃的疲劳性能研究

对某型飞机新成型座舱盖及使用后座舱盖有机玻璃的疲劳性能进行了试验研究.利用升降法试验得到了指定目标寿命下两种不同情况有机玻璃的条件疲劳极限,利用三参数法拟合得到了两种情况有机玻璃的S-N曲线.对新成型座舱盖及使用后座舱盖有机玻璃的疲劳性能进行了对比分析.对比分析的结果表明,与新成型座舱盖相比,使用后座舱盖有机玻璃的疲劳性能没有显著下降.     

MDYB-3有机玻璃疲劳性能温度效应研究

 对MDYB-3有机玻璃进行了不同温度下等幅载荷拉-拉疲劳试验，对实验结果按照疲劳寿命的幂函数公式进行拟合，得到了几个典型温度下的S-N曲线。结果表明随着温度的升高，疲劳强度有大幅度的降低。在对实验数据线性回归分析结果的基础上进行多项式拟合，建立了考虑温度效应的疲劳寿命估算方程，并用疲劳包络线粗略地表示了不同温度下达到指定疲劳寿命时的应力水平。分析了疲劳总应变与循环次数比之间的关系，给出了不同温度下第二阶段总应变增长率与疲劳寿命之间的关系式。研究结果为飞机风挡和舱盖的设计和寿命评估提供了参考和依据。     

座舱盖抛放过程中的非定常气动特性研究

通过对N-S方程的数值求解模拟了座舱盖在静止和旋转两种状态下的气动力分布,分析了来流马赫数、旋转角速度以及迎角对气动系数的影响,研究了座舱盖自由抛放过程的非定常效应,并最终建立了预测座舱盖自由抛放过程气动系数的气动系数图。计算表明:(1)非定常效应是影响抛放过程座舱盖气动力分布的主要因素;(2)外形左右对称的座舱盖,均有非定常气动系数平均值与无量纲角速度成线性关系的规律,而且变化斜率几乎与舱盖形状尺寸等无关。     

航空发动机轴承腔换热特性研究

轴承腔是航空发动机机械系统的重要组成部分,其换热特性对滑油系统热分析有决定性影响,为此,对航空发动机典型轴承腔的换热特性进行研究。以ANSYS有限元分析软件结合APDL语言,对典型轴承腔进行有限元建模,并对边界条件进行计算加载,得到了在不同供油量和滑油供油温度下的轴承腔换热特性曲线。采用本方法计算的轴承腔特性与发动机地面试车数据符合性良好,所得到的典型轴承腔换热特性曲线可简化滑油系统热分析,取得很好的系统计算结果。并开辟了通过提高轴承腔换热特性曲线精度而提高系统计算精度的研究途径。本文的计算方法及结果可为发动机整机试车及润滑系统设计提供参考。     

大气参数偏差对再入弹头爆点射程的影响

统计出了实际大气状态参数与标准大气状态参数的最大偏差值，以等高程和等过载引信两种弹头引信方式建立了大气参数偏差对弹道式导弹弹头引爆点射程影响的数学模型，从理论上分析了大气参数偏差对弹道式导弹弹头引爆点对应射程产生影响的物理实质；进而以一种洲际弹道导弹为例，讨论出大气参数偏差引起弹头命中点射程偏差的具体数值。     

Atmospheric/Exospheric Characteristics of Icy Satellites

The atmospheres/exospheres of icy satellites greatly vary from one to the next in terms of density, composition, structure or steadiness. Titan is the only icy satellite with a dense atmosphere comparable in many ways to that of the Earth’s atmosphere. Titan’s atmosphere prevents the surface from direct interaction with the plasma environment, but gives rise to Earth-like exchanges of energy, matter and momentum. The atmospheres of other satellites are tenuous. Enceladus’ atmosphere manifests itself in a large water vapor plume emanating from surface cracks near the south pole. Io’s SO₂ atmosphere originates from volcanoes. Europa’s tenuous O₂ atmosphere is produced by intense radiation bombardment. This chapter reviews the characteristics of the atmospheres of Titan, Enceladus, Io and Europa based on observations.     

Origin of planetary atmospheres

The near absence of noble gases on earth, other than those of radioactive origin, indicates that the earth was formed by the accumulation of planetesimals; this process systematically excluded all constituents that did not enter into the solid phase. The atmosphere and the ocean with many of its dissolved salts have arisen from gases emitted from the earth's interior, a process that continues today. The oxygen in the earth's atmosphere plus a greater quantity that has been removed from the atmosphere to oxidize geologic materials, has arisen mainly from a small excess of photosynthesis over decay of organic material. The atmospheres of Mars and Venus have probably arisen in a manner similar to the atmosphere on earth, by emission from the planetary interiors. However, they have not received any oxygen from photosynthesis and so are nearly oxygen free. Mars has very little water in its atmosphere, and this can be explained by its lower than freezing average surface temperature. Venus also has very little water, and this requires an ad hoc explanation; one possibility is that Venus was formed from much drier planetesimals than was the earth. Mercury and the moon are virtually without atmospheres. Although some gases may be emitted from their interiors, they are presumably rapidly lost by escape. Whatever atmosphere they possess is probably due to the neutralized solar wind that impinges upon them. The outer planets retained volatiles, including hydrogen and helium, to a much greater extent than did the terrestrial planets.     

Profiles of Ion and Aerosol Interactions in Planetary Atmospheres

In planetary atmospheres the nature of the aerosols varies, as does the relative importance of different sources of ion production. The nature of the aerosol and ion production is briefly reviewed here for the atmospheres of Venus, Mars, Jupiter and Titan using the concepts established for the terrestrial atmosphere. Interactions between the ions formed and aerosols present cause (1) charge exchange, which can lead to substantial aerosol charge and (2) ion removal. Consequences of (1) are that (a) charged aerosol are more effectively removed by conducting liquid droplets than uncharged aerosol and (b) particle–particle coagulation rates are modified, influencing particle residence times in the relevant atmosphere. Consequences of (2) are that ions are removed in regions with abundant aerosol, which may preclude charge flow in an atmosphere, such as that associated with an atmospheric electrical circuit. In general, charge should be included in microphysical modeling of the properties of planetary aerosols.     

New Horizons: Anticipated Scientific Investigations at the Pluto System

The New Horizons spacecraft will achieve a wide range of measurement objectives at the Pluto system, including color and panchromatic maps, 1.25–2.50 micron spectral images for studying surface compositions, and measurements of Pluto’s atmosphere (temperatures, composition, hazes, and the escape rate). Additional measurement objectives include topography, surface temperatures, and the solar wind interaction. The fulfillment of these measurement objectives will broaden our understanding of the Pluto system, such as the origin of the Pluto system, the processes operating on the surface, the volatile transport cycle, and the energetics and chemistry of the atmosphere. The mission, payload, and strawman observing sequences have been designed to achieve the NASA-specified measurement objectives and maximize the science return. The planned observations at the Pluto system will extend our knowledge of other objects formed by giant impact (such as the Earth–moon), other objects formed in the outer solar system (such as comets and other icy dwarf planets), other bodies with surfaces in vapor-pressure equilibrium (such as Triton and Mars), and other bodies with N₂:CH₄ atmospheres (such as Titan, Triton, and the early Earth).     

Atmospheric science on the Galileo mission

Observations from the ground and four fly-by spacecraft have provided initial reconnaissance of Jupiter's atmosphere. The Pioneer and Voyager data have raised new questions and underlined old ones about the basic state of the atmosphere and the processes determining the atmosphere's behavior. This paper discusses the main atmospheric science objectives which will be addressed by the Galileo (Orbiter and Probe) mission, organizing the discussion according to the required measurements of chemical composition, thermal structure, clouds, radiation budget, dynamics, upper atmosphere, and satellite atmospheres. Progress on the key questions will contribute not only to our knowledge of Jupiter's atmosphere but to a general understanding of atmospheric processes which will be valuable for helping us to understand the atmosphere and climate of the Earth.Realization of the atmospheric science objectives of the Galileo mission depends upon: (a) coordinated measurements from the entry probe and the orbiter; (b) global observations; and (c) observations over the range of time-scales needed to characterize the basic dynamical processes.The Atmospheres Working Group also includes: M. D. Allison, M. J. S. Belton, R. W. Boese, R. W. Carlson, C. R. Chapman, T. Encrenaz, V. R. Eshleman, P. J. Gierasch, C. W. Hord, H. T. Howard, L. J. Lanzerotti, H. B. Niemann, G. S. Orton, T. Owen, C. B. Pilcher, J. B. Pollack, B. Ragent, W. B. Rossow, A. Seiff, A. I. Stewart, P. H. Stone, F. W. Taylor, G. L. Tyler, U. von Zahn, and R. A. West.     

Isotopic Fractionation by Gravitational Escape

Present natural data bases for abundances of the isotopic compositions of noble gases, carbon and nitrogen inventories can be found in the Sun, the solar wind, meteorites and the planetary atmospheres and crustal reservoirs. Mass distributions in the various volatile reservoirs provide boundary conditions which must be satisfied in modelling the history of the present atmospheres. Such boundary conditions are constraints posed by comparison of isotopic ratios in primordial volatile sources with the isotopic pattern which was found on the planets and their satellites. Observations from space missions and Earth-based spectroscopic telescope observations of Venus, Mars and Saturn's major satellite Titan show that the atmospheric evolution of these planetary bodies to their present states was affected by processes capable of fractionating their elements and isotopes. The isotope ratios of D/H in the atmospheres of Venus and Mars indicate evidence for their planetary water inventories. Venus' H₂O content may have been at least 0.3% of a terrestrial ocean. Analysis of the D/H ratio on Mars imply that a global H₂O ocean with a depth of ≤ 30 m was lost since the end of hydrodynamic escape. Calculations of the time evolution of the ¹⁵N/¹⁴N isotope anomalies in the atmospheres of Mars and Titan show that the Martian atmosphere was at least ≥ 20 times denser than at present and that the mass of Titan's early atmosphere was about 30 times greater than its present value. A detailed study of gravitational fractionation of isotopes in planetary atmospheres furthermore indicates a much higher solar wind mass flux of the early Sun during the first half billion years. This revised version was published online in August 2006 with corrections to the Cover Date.     

Exospheres and Energetic Neutral Atoms of Mars, Venus and Titan

Our understanding of the upper atmosphere of unmagnetized bodies such as Mars, Venus and Titan has improved significantly in this decade. Recent observations by in situ and remote sensing instruments on board Mars Express, Venus Express and Cassini have revealed characteristics of the neutral upper atmospheres (exospheres) and of energetic neutral atoms (ENAs). The ENA environment in the vicinity of the bodies is by itself a significant study field, but ENAs are also used as a diagnostic tool for the exosphere and the interaction with the upstream plasmas. Synergy between theoretical and modeling work has also improved considerably. In this review, we summarize the recent progress of our understanding of the neutral environment in the vicinity of unmagnetized planets.     

Atmospheric Escape and Evolution of Terrestrial Planets and Satellites

The origin and evolution of Venus’, Earth’s, Mars’ and Titan’s atmospheres are discussed from the time when the active young Sun arrived at the Zero-Age-Main-Sequence. We show that the high EUV flux of the young Sun, depending on the thermospheric composition, the amount of IR-coolers and the mass and size of the planet, could have been responsible that hydrostatic equilibrium was not always maintained and hydrodynamic flow and expansion of the upper atmosphere resulting in adiabatic cooling of the exobase temperature could develop. Furthermore, thermal and various nonthermal atmospheric escape processes influenced the evolution and isotope fractionation of the atmospheres and water inventories of the terrestrial planets and Saturn’s large satellite Titan efficiently.