外端壁收缩与单向倾斜组合涡轮导叶的三维气动力研究

低展弦比涡轮导叶的外端壁收缩与单向正倾斜组合设计是既可减小两端二次流损失又可以满足冲击冷却叶片叶身需平直要求的技术措施。本文简要阐述了组合设计可减小二次流损失的力学机制、流场特征及三维流场设计分析的评价准则。通过三维流场计算 ,详细分析了诸如单向倾斜角度、子午面外端壁轮廓收缩起点、内外曲率半径等主要特征参数对流场品质的影响。给出了组合设计的方法与步骤及评价流场的定性准则。该组合设计方法对低展弦比高温涡轮导向叶片的成功设计具有指导意义。     

用纤内Bragg光栅进行动态应变测量的研究

描述了用纤内Bragg光栅进行动态应变测量研究的意义，原理和方法，提出了两种用纤内Bragg光栅动态应变测量时进行Bragg波长偏移量的解调方法；光干涉相位检测Bragg光栅反射波长偏移的解调方法和用DWDM密集波分复用器解调Bragg波长的方法，前者适用于高频宽带动态应变测量，后者适用于有限频率或中等频率响应的动态应变测量。     

具有软件特征的一种CTI应用模式

计算机电信集成技术是 2 0世纪 90年代新兴的计算机通信技术。通过使用最新的数字处理技术 ,CTI把计算机和通信紧密地结合到一起。本文论述目前CTI的发展趋势 ,即传统呼叫中心与WEB呼叫中心统一的方案向“软件”方向靠拢的趋势 ,核心是提出一种分层的CTI体系结构。     

燃烧室出口径向温度分布试验及分析模型

在二元试验燃烧室上,研究了四种掺混孔设计方案对燃烧室出口径向温度分布影响。结果表明,不同掺混孔设计方案对出口径向温度分布的影响有规律可循。本文建立了半经验半分析模型,能够由第一次试验得到的出口温度分布,推算修改后出口径向温度分布曲线的变化。模型计算结果和试验结果吻合。     

Optimal speckle reduction in polarimetric SAR imagery

Speckle is a major cause of degradation in synthetic aperture radar (SAR) imagery. With the availability of fully polarimetric SAR data, it is possible to use the three complex elements (HH, HV, VV) of the polarimetric scattering matrix to reduce speckle. The optimal method for combining the elements of the scattering matrix to minimize image speckle is derived, and the solution is shown to be a polarimetric whitening filter (PWF). A simulation of spatially correlated, K-distributed, fully polarimetric clutter is then used to compare the PWF with other, suboptimal speckle-reduction methods. Target detection performance of the PWF, span, and single-channel |HH|² detectors is compared with that of the optimal polarimetric detector (OPD). A novel, constant-false-alarm-rate (CFAR) detector (the adaptive PWF) is as a simple alternative to the OPD for detecting targets in clutter. This algorithm estimates the polarization covariance of the clutter, uses the covariance to construct the minimum-speckle image, and then tests for the presence of a target. An exact theoretical analysis of the adaptive PWF is presented; the algorithm is shown to have detection performance comparable with that of the OPD     

某型机外形数模修形设计

在某型机外形数模修形设计过程中,探讨如何确定修形原则,即针对存在各种问题的曲面形态,如何确定不同的修形方法,使整个飞机外型数模达到光顺性、结构可实施性、曲面连续性要求。     

微量钪对Al-Zn-Mg-Zr焊接接头组织性能的影响

采用铸锭冶金法制备了 Al-6.0Zn-2.0Mg-0.12Zr 和 Al- 6.0Zn - 2.0Mg - 0.2Sc - 0.12Zr 两种合金板材,以 Al-Mg-Sc-Zr焊丝为焊接填充材料,对3 mm厚的上述两种合金板材进行氩弧焊接,之后对两种接头的显微组织和力学性能进行对比研究.结果表明:第一,微量Sc可以显著提高Al-Zn-Mg-Zr合金基材的拉伸性能,基材强度的提高来源于晶粒细化强化、Al3(Sc,Zr)粒子的析出强化和Al3(Sc,Zr)粒子引起的亚结构强化;第二,焊接过程中,不含 Sc 的合金焊接接头热影响区内η相(MgZn2)粒子和晶粒明显粗化,含 Sc的合金焊接接头热影响区内η相(MsZn2)粒子也明显粗化,但晶粒大小没有明显变化,由于Al3(Sc、Zr)粒子稳定性高,不容易粗化和团聚,对位错和亚晶界仍然起钉扎作用,热影响区仍然保持未再结晶组织,过时效软化现象相对于传统的铝镁合金来说不是很严重;第三,微量 Sc 可以明显提高 Al-Zn-Mg-Zr 合金焊接接头的强度,与不加 Sc 的合金焊接接头相比,添加Sc的合金拉伸强度从395 MPa提高到447 MPa,强度系数从 0.7 提高到0.8.强度的提高主要来源于晶粒细化强化、Al3(Sc,Zr)粒子的析出强化和由于Al3(Sc,Zr)粒子的高稳定性导致的的抗热循环软化能力的提高.     

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.