高负荷吸附式压气机叶栅开槽方案实验研究

在低速条件下对三种吸气槽方案的高负荷吸附式压气机叶栅进行了详细的实验研究.通过墨迹流场显示法对叶栅壁面流场进行了测量,利用五孔气动探针对叶栅出口截面进行了扫掠,并对不同叶高的型面静压进行了采集,详细分析了全叶高吸气方式和两种局部吸气方式对叶栅流场结构和负荷能力的影响.结果表明,采用吸力面两端吸气对抑制角区分离流动、减弱通道涡强度和尺度、提高叶栅内流动性能的效果要优于其它两种方式,积聚在角区的低能流体由于较大的吸气量而被大量吸除是性能改善的关键.     

一类新的速度入流条件在管道流模拟的应用

基于经典边界层理论,发展了一类简化的、按边界层厚度描述的速度入流边界条件。基于入流条件,对低速后向台阶流动和超声速压缩拐角流动进行了数值模拟。通过细致比较空间流场、边界层内速度型、表面摩擦阻力和压力分布等特性,对该类型边界条件进行了计算确认。结果表明,所发展的简化边界层厚度速度入流条件提法正确、合理,具有描述方法简单、鲁棒性好、适合工程计算的优点,可显著简化不同流速的管道流动的数值模拟。     

舱外航天服热试验外热流模拟方法研究

出舱行走所必需的舱外航天服具有复杂外表面形状,其空间外热流极其复杂。文章对舱外航天服在热试验中所采用的外热流模拟方法进行了对比分析研究,结合航天服的特点对热试验中外热流模拟的方式进行了探讨, 论证了用接触式电加热片及红外加热笼两种外热流施加方式的可行性,并通过分析的手段对不同热试验方法中施加的热流和太空中的热流大小及分布进行了对比。     

薄膜电阻温度计原理性误差分析及数据处理方法研究

薄膜电阻温度计是高超声速测热试验中一种常用的传感器,多用于激波风洞中.改进薄膜电阻温度计测热数据的后处理方法,分析其原理性误差,提出修正方法,可以进一步提高热流测量精度,为防热设计提供可靠数据.应用三维热传导理论,考虑热流和温升的耦合影响,计算了气动加热条件下薄膜电阻温度计结构温升情况,得到了铂层内的温度分布规律,并与一维半无限简化理论得到的薄膜电阻温度计表层温度相互对比,得到了模型简化带来的原理性误差;建立了由表面温升计算表面热流的导热反问题计算方法,与经典的Cook-Felderman处理公式和热电模拟网络处理方法相互对比,提出了修止热流值的方法,为提高热流测量精度提供了一种可行的手段.     

新电位移边界条件下的压电介质断裂问题

应用边界元法,并结合一种特殊的复变函数基本解,研究了压电介质的断裂问题。由于该基本解完全遵循本构方程没有对电位移边界作假设,所以结论同非穿透性裂纹假设的结果有较大差异。通过计算表明,外加力载荷不但会引起裂纹尖端应力奇异性,也会引起电场奇异性,同样,外加电压也会引起裂纹尖端应力奇异性。     

八丝热线探针制作及其应用

介绍了八丝热线探针的制作工艺,有效地消除了各热丝探头之间的电信号干扰和动力学干扰。实验中使用该探针检测到了湍流边界层内的大尺度旋涡,并测量了它们的强度和尺度。与此同时还获得了速度、湍流强度和功率谱等流场参数,结果与现有典型数据一致。说明本文所述的多丝热线探针具有很强的实用性。     

风洞地板边界层厚度控制新方法

本文介绍了一种风洞固定地板边界层厚度控制新方法。风洞试验结果比较表明,这种方法不但能显著降低地板边界层厚度,而且边界层控制装置对风洞气流干扰较小,流场较均匀,气流品质较好。与国内外现有的风洞地板边界层厚度控制方法相比,这种方法颇具特色。     

某类跨大气层飞行器全航程红外辐射特性分析

针对某类跨大气层飞行器飞行过程中需要进出大气层,且飞行速度跨度大等特点,建立了不同空域、不同飞行速度下的机体头部受热模型。当在大气层内飞行时分别使用经验公式和Lees公式计算马赫数小于5和大于5时头部受热情况,当在大气层外飞行时建立了考虑太阳直射、地球反照和地球红外加热情况下的受热模型。利用普朗克定律得到了相同温度下不同波段的红外辐射能量占比情况。最后利用本方法对某类跨大气层飞行器进行了温度和红外辐射计算,得到的计算结果能够大致反映全航程头部温度和红外辐射变化情况。     

Upper limit of the total magnetic flux in an active region according to the photometric-magnetic dynamical model

The photometric-magnetic dynamical model handles the evolution of an individual sunspot as an autonomous nonlinear, though integrable, dynamical system. One of its consequences is the prediction of an upper limit of the sunspot areas. This upper limit is analytically expressed by the model parameters, while its calculated value is verified by the observational data. In addition, an upper limit for the magnetic strength inside the sunspot is also predicted, and then, we obtain the following significant result: The upper limit of the total magnetic flux in an active region is found to be of about 7.23 × 10²³ Mx, namely, phenomenologically equal to the magnetic flux concentrated in the totality of the granules of the quiet Sun, having a typical maximum magnetic strength of about 12G. Therefore, the magnetic flux concentrated in an active region cannot exceed the magnetic flux concentrated in the photosphere as a whole.     

Driving major solar flares and eruptions: A review

This review focuses on the processes that energize and trigger M- and X-class solar flares and associated flux-rope destabilizations. Numerical modeling of specific solar regions is hampered by uncertain coronal-field reconstructions and by poorly understood magnetic reconnection; these limitations result in uncertain estimates of field topology, energy, and helicity. The primary advances in understanding field destabilizations therefore come from the combination of generic numerical experiments with interpretation of sets of observations. These suggest a critical role for the emergence of twisted flux ropes into pre-existing strong field for many, if not all, of the active regions that produce M- or X-class flares. The flux and internal twist of the emerging ropes appear to play as important a role in determining whether an eruption will develop predominantly as flare, confined eruption, or CME, as do the properties of the embedding field. Based on reviewed literature, I outline a scenario for major flares and eruptions that combines flux-rope emergence, mass draining, near-surface reconnection, and the interaction with the surrounding field. Whether deterministic forecasting is in principle possible remains to be seen: to date no reliable such forecasts can be made. Large-sample studies based on long-duration, comprehensive observations of active regions from their emergence through their flaring phase are needed to help us better understand these complex phenomena.