非标准大气条件下航空发动机地面起动性能

为了得到非标准大气条件对航空发动机地面起动性能的影响,对非标准大气条件下空气涡轮起动机输出功率特性、标准大气条件下理想起动过程的影响因素进行了分析.研究了非标准大气条件对航空发动机地面起动性能影响,分析了大气温度对起动点火时间、起动时间、起动过程排气温度的影响.应用均匀加速原理,对某型涡扇发动机起动时间进行估算.基于地面台架起动试验条件,对试验数据统计分析:大气温度增加或降低,将增加起动点火及脱开时间.对大气温度在293.15K以上的开车次的平均起动时间与293.15K以下的平均起动时间进行对比,热天起动时间比冷天要短约3s,试验结果符合理论分析.      

某型飞机后减速板振动试验

某型飞机后减速板在部队使用中多次出现减速板梁断裂、蒙皮裂纹等故障 ,打孔加型材结构改进方案经实际飞行测试取得了满意效果。为给出打孔加型材结构改进方案的使用寿命 ,进行了 2种结构后减速板的地面振动对比试验。本文对后减速板地面振动对比试验方法进行简要介绍。     

噪声载荷作用下薄壁柱壳结构的随机振动响应的估算方法

给出了噪声载荷作用下薄壁柱壳结构随机振动加速度响应功率谱密度的计算公式和计算方法,并与实际测量获得的加速度响应功率谱密度进行了比较,计算的功率谱与实测的功率谱具有较好的一致性,说明这种估算噪声载荷作用下薄壁柱壳结构随机振动加速度响应功率谱密度的方法是合理可行的。用同样方法导出的Von Mises应力响应的功率谱密度及其均方值的计算公式,可直接用于疲劳强度分析。      

高过载条件下绝热层烧蚀实验方法研究 (Ⅰ)方案论证及数值模拟

分析了高过载对固体火箭发动机流场和绝热层烧蚀的影响规律，提出一种新的研究思路：采用数值模拟方法来预示发动机三维两相流场，建立高过载流场模拟实验装置，开展绝热层烧蚀实验，建立高过载条件下的绝热层烧蚀模型，在此基础上发展高过载发动机绝热层设计和烧蚀预示方法。其中关键技术是高过载流场的模拟，对粒子加入法和弯管分离法两种方案进行了论证，认为弯管分离法原理上是可行的。为了验证这种方案的可行性，开展了弯管通道两相流的数值模拟研究，计算结果表明弯管装置具有使凝相粒子聚集形成高浓度粒子流的功能。     

不同温、湿度条件下硅橡胶密封圈贮存寿命研究

通过对硅橡胶P6144密封圈的加速老化试验,建立了该密封圈材料在贮存温度下的压缩永久变形和时间的关系,预测了25℃、35℃、45℃、55℃、65℃和75℃温度条件下硅橡胶P6144密封材料的贮存寿命,研究了温度对硅橡胶密封圈贮存寿命的影响规律。     

MESSENGER: Exploring Mercury’s Magnetosphere

The MErcury Surface, Space ENvironment, GEochemistry, and Ranging (MESSENGER) mission to Mercury offers our first opportunity to explore this planet’s miniature magnetosphere since the brief flybys of Mariner 10. Mercury’s magnetosphere is unique in many respects. The magnetosphere of Mercury is among the smallest in the solar system; its magnetic field typically stands off the solar wind only ∼1000 to 2000 km above the surface. For this reason there are no closed drift paths for energetic particles and, hence, no radiation belts. Magnetic reconnection at the dayside magnetopause may erode the subsolar magnetosphere, allowing solar wind ions to impact directly the regolith. Inductive currents in Mercury’s interior may act to modify the solar wind interaction by resisting changes due to solar wind pressure variations. Indeed, observations of these induction effects may be an important source of information on the state of Mercury’s interior. In addition, Mercury’s magnetosphere is the only one with its defining magnetic flux tubes rooted beneath the solid surface as opposed to an atmosphere with a conductive ionospheric layer. This lack of an ionosphere is probably the underlying reason for the brevity of the very intense, but short-lived, ∼1–2 min, substorm-like energetic particle events observed by Mariner 10 during its first traversal of Mercury’s magnetic tail. Because of Mercury’s proximity to the sun, 0.3–0.5 AU, this magnetosphere experiences the most extreme driving forces in the solar system. All of these factors are expected to produce complicated interactions involving the exchange and recycling of neutrals and ions among the solar wind, magnetosphere, and regolith. The electrodynamics of Mercury’s magnetosphere are expected to be equally complex, with strong forcing by the solar wind, magnetic reconnection, and pick-up of planetary ions all playing roles in the generation of field-aligned electric currents. However, these field-aligned currents do not close in an ionosphere, but in some other manner. In addition to the insights into magnetospheric physics offered by study of the solar wind–Mercury system, quantitative specification of the “external” magnetic field generated by magnetospheric currents is necessary for accurate determination of the strength and multi-polar decomposition of Mercury’s intrinsic magnetic field. MESSENGER’s highly capable instrumentation and broad orbital coverage will greatly advance our understanding of both the origin of Mercury’s magnetic field and the acceleration of charged particles in small magnetospheres. In this article, we review what is known about Mercury’s magnetosphere and describe the MESSENGER science team’s strategy for obtaining answers to the outstanding science questions surrounding the interaction of the solar wind with Mercury and its small, but dynamic, magnetosphere.     

Galactic Wind: Mass Fractionation and Cosmic Ray Acceleration

The dynamical and chemical effects of the Galactic Wind are discussed. This wind is primarily driven by the pressure gradient of the Cosmic Rays. Assuming the latter to be accelerated in the Supernova Remnants of the disk which at the same time produce the Hot Interstellar Medium, it is argued that the gas removed by the wind is enriched in the nucleosynthesis products of Supernova explosions. Therefore the moderate mass loss through this wind should still be able to remove a substantial amount of metals, opening the way for stars to produce more metals than observed in the disk, by e.g. assuming a Salpeter-type stellar initial mass function beyond a few Solar masses. The wind also allows a global, physically appealing interpretation of Cosmic Ray propagation and escape from the Galaxy. In addition the spiral structure of the disk induces periodic pressure waves in the expanding wind that become a sawtooth shock wave train at large distances which can re-accelerate “knee” particles coming from the disk sources. This new Galactic Cosmic Ray component can reach energies of a few×10¹⁸ eV and may contribute to the juncture between the particles of Galactic and extragalactic origin in the observed overall Cosmic Ray spectrum.     

基于退化模型的失效机理一致性检验方法

有效的加速试验必须保证产品的失效机理不变。针对加速退化试验(ADT)可靠性建模的特点,提出了一种基于退化模型的失效机理一致性检验方法。以基于随机过程和基于退化轨迹拟合的退化模型为例,通过加速系数的2种等效定义分别建立了模型参数与失效机理不变的内在联系,进一步推导出其参数在不同应力下须满足的关系。在合理假定检验样本服从正态分布的基础上,利用t统计量对样本的一致性进行检验。通过2个ADT实例验证了所提检验方法的合理性与可行性。     

RT-11燃油调节器加速性不稳定原因分析

介绍了某型发动机的RT-11燃油调节器加速性不稳定、起飞状态燃油供油量停滞的情况,分析了产生故障的原因和故障机理,并提出了修理中的改进措施。     

某型民用飞机电源系统负加速度试飞研究

首先对民用飞机电源系统负加速度试飞进行简要说明,提出民用飞机电源系统负加速度试飞的原因和目的。其次对电源系统负加速度试飞条件、试飞方法和试飞程序进行说明。对电源系统负加速试飞结果进行分析评估,表明电源系统设计是满足设计要求和民用航空标准要求的。最后对负加速度试飞中注意事项进行了详细说明,为其它机型飞机进行负加速度试飞提供借鉴。