绕任意轴旋转的管道流动和换热特性研究

当管道绕任意轴旋转时，管道内的轴向速度分布发生改变，截面上产生二次流动，管道的对流换热特性将引起变化。本文对绕任意轴旋转的管道流动与换热进行了数值模拟，研究结果表明：绕任意轴旋转管道内的对流换热特性主要由Re（雷诺数），Ro(Rossby数），Pr（普朗特数）数，和α（旋转轴与管道轴线的夹角）四个参数决定。文中分析了在不同情况下流场结构与摩擦系数比以及温度场与管道Nu数比率随Re数和Ro数的变化规律，为工程实际应用提供了理论依据。     

干摩擦面上接触应力分布的混合分析法

为准确而方便地获得诸如航空发动机风扇（转子）叶片凸肩（叶冠）之间的干摩擦接触面上的应用力分布，将光测弹性实验方法与有限元数值计算方法结合，建立一种求解接触应力的滋合法。用云纹干涉法提取光弹模型接触面的位称作为计算的边界条件，获得接触面上的接触应力。该方法提高了计算方法的精度和效率，也克服了单纯用实验方法求解接触应力的困难和花费大的缺点。应用混合法分析了航空发动机带凸肩风扇叶片在高速旋转时凸肩间接触面上的接触应力，比较混合法一光弹性法所得接触应力分布，两的结果比较一致。     

Imaging Plasma Density Structures in the Soft X-Rays Generated by Solar Wind Charge Exchange with Neutrals

Both heliophysics and planetary physics seek to understand the complex nature of the solar wind’s interaction with solar system obstacles like Earth’s magnetosphere, the ionospheres of Venus and Mars, and comets. Studies with this objective are frequently conducted with the help of single or multipoint in situ electromagnetic field and particle observations, guided by the predictions of both local and global numerical simulations, and placed in context by observations from far and extreme ultraviolet (FUV, EUV), hard X-ray, and energetic neutral atom imagers (ENA). Each proposed interaction mechanism (e.g., steady or transient magnetic reconnection, local or global magnetic reconnection, ion pick-up, or the Kelvin-Helmholtz instability) generates diagnostic plasma density structures. The significance of each mechanism to the overall interaction (as measured in terms of atmospheric/ionospheric loss at comets, Venus, and Mars or global magnetospheric/ionospheric convection at Earth) remains to be determined but can be evaluated on the basis of how often the density signatures that it generates are observed as a function of solar wind conditions. This paper reviews efforts to image the diagnostic plasma density structures in the soft (low energy, 0.1–2.0 keV) X-rays produced when high charge state solar wind ions exchange electrons with the exospheric neutrals surrounding solar system obstacles.The introduction notes that theory, local, and global simulations predict the characteristics of plasma boundaries such the bow shock and magnetopause (including location, density gradient, and motion) and regions such as the magnetosheath (including density and width) as a function of location, solar wind conditions, and the particular mechanism operating. In situ measurements confirm the existence of time- and spatial-dependent plasma density structures like the bow shock, magnetosheath, and magnetopause/ionopause at Venus, Mars, comets, and the Earth. However, in situ measurements rarely suffice to determine the global extent of these density structures or their global variation as a function of solar wind conditions, except in the form of empirical studies based on observations from many different times and solar wind conditions. Remote sensing observations provide global information about auroral ovals (FUV and hard X-ray), the terrestrial plasmasphere (EUV), and the terrestrial ring current (ENA). ENA instruments with low energy thresholds (\(\sim1~\mbox{keV}\)) have recently been used to obtain important information concerning the magnetosheaths of Venus, Mars, and the Earth. Recent technological developments make these magnetosheaths valuable potential targets for high-cadence wide-field-of-view soft X-ray imagers.Section 2 describes proposed dayside interaction mechanisms, including reconnection, the Kelvin-Helmholtz instability, and other processes in greater detail with an emphasis on the plasma density structures that they generate. It focuses upon the questions that remain as yet unanswered, such as the significance of each proposed interaction mode, which can be determined from its occurrence pattern as a function of location and solar wind conditions. Section 3 outlines the physics underlying the charge exchange generation of soft X-rays. Section 4 lists the background sources (helium focusing cone, planetary, and cosmic) of soft X-rays from which the charge exchange emissions generated by solar wind exchange must be distinguished. With the help of simulations employing state-of-the-art magnetohydrodynamic models for the solar wind-magnetosphere interaction, models for Earth’s exosphere, and knowledge concerning these background emissions, Sect. 5 demonstrates that boundaries and regions such as the bow shock, magnetosheath, magnetopause, and cusps can readily be identified in images of charge exchange emissions. Section 6 reviews observations by (generally narrow) field of view (FOV) astrophysical telescopes that confirm the presence of these emissions at the intensities predicted by the simulations. Section 7 describes the design of a notional wide FOV “lobster-eye” telescope capable of imaging the global interactions and shows how it might be used to extract information concerning the global interaction of the solar wind with solar system obstacles. The conclusion outlines prospects for missions employing such wide FOV imagers.     

Potential Effects of Surface Temperature Variations and Disturbances and Thermal Convection on the Mars InSight HP<Superscript>3</Superscript> Heat-Flow Determination

The HP³ instrument on the InSight lander mission will measure subsurface temperatures and thermal conductivities from which heat flow in the upper few meters of the regolith at the landing site will be calculated. The parameter to be determined is steady-state conductive heat flow, but temperatures may have transient perturbations resulting from surface temperature changes and there could be a component of thermal convection associated with heat transport by vertical flow of atmospheric gases over the depth interval of measurement. The experiment is designed so that it should penetrate to a depth below which surface temperature perturbations are smaller than the required measurement precision by the time the measurements are made. However, if the measurements are delayed after landing, and/or the probe does not penetrate to the desired depth, corrections may be necessary for the transient perturbations. Thermal convection is calculated to be negligible, but these calculations are based on unknown physical properties of the Mars regolith. The effects of thermal convection should be apparent at shallow depths where transient thermal perturbations would be observed to deviate from conductive theory. These calculations were required during proposal review and their probability of predicting a successful measurement a prerequisite for mission approval. However, their uncertainties lies in unmeasured physical parameters of the Mars regolith.     

悬停状态下旋翼旋转噪声的分析

对直升机悬停时旋翼的旋转噪声进行了初步研究，分别用单极子和偶极子声源描述旋翼的厚度噪声和载荷噪声，并根据悬停状态下旋翼气动载荷的特点，用傅立叶级数表示旋翼桨盘上各点的气动力和法向气流速度，然后代入单极子和偶极子声源声辐射公式中，求出旋翼桨盘外某观察点的声压值。最后结合一算例，分析悬停状态下旋翼旋转噪声的辐射特性和不同的展向载荷分布模型对计算结果的响应。     

舰载机变长度减振牵制装置动力学分析

舰载机弹射起飞过程中,由于牵制载荷突卸而产生的前起落架沿航向的快速振动对机体结构和设备都会带来严重的疲劳问题。本文建立了舰载机弹射起飞动力学模型,设计了具有减振功能的舰载机弹射起飞变长度牵制装置,分析了该装置的动力学特性,并对该装置的减振效果进行了参数分析。研究结果表明:牵制载荷沿下扭力臂轴向的载荷分量所造成的缓冲器活塞杆的向后弯曲是导致牵制载荷突卸后前起落架振动的主要原因;变长度减振牵制装置通过实时改变牵制杆长度和牵制角,可大幅降低牵制载荷突卸后前起落架振动以及各铰接点振荡载荷,该装置在解决牵制载荷突卸振动问题中效果明显。     

三维攻击角度约束部分制导控制一体化设计

针对侧滑转弯(STT)导弹带有攻击角度约束的机动目标拦截问题,提出一种基于自适应终端滑模动态面控制的三维部分制导控制一体化(PIGC)设计方法。首先,建立了针对机动目标拦截的侧滑转弯导弹三维部分制导控制一体化设计模型,且不需要导弹速度微分体轴系分量信息。然后,使用终端滑模控制理论构建误差向量与虚拟控制量,达成精确拦截与攻击角度约束的控制目的;引入有限时间非线性收敛扩张状态观测器(ESO)来在线估计系统不确定性;设计自适应算子与自适应更新律对观测器的估计误差进行补偿,以提高方法的鲁棒性。最后,三维空间拦截仿真校验了方法在提高拦截精度与增强角度约束收敛性能的有效性。     

Volatile Trapping in Martian Clathrates

Thermodynamic conditions suggest that clathrates might exist on Mars. Despite observations which show that the dominant condensed phases on the surface of Mars are solid carbon dioxide and water ice, clathrates have been repeatedly proposed to play an important role in the distribution and total inventory of the planet’s volatiles. Here we review the potential consequences of the presence of clathrates on Mars. We investigate how clathrates could be a potential source for the claimed existence of atmospheric methane. In this context, plausible clathrate formation processes, either in the close subsurface or at the base of the cryosphere, are reviewed. Mechanisms that would allow for methane release into the atmosphere from an existing clathrate layer are addressed as well. We also discuss the proposed relationship between clathrate formation/dissociation cycles and how potential seasonal variations influence the atmospheric abundances of argon, krypton and xenon. Moreover, we examine several Martian geomorphologic features that could have been generated by the dissociation of extended subsurface clathrate layers. Finally we investigate the future in situ measurements, as well as the theoretical and experimental improvements that will be needed to better understand the influence of clathrates on the evolution of Mars and its atmosphere.     

发汗冷却喷管在火箭发动机上的应用

较系统地介绍了发汗冷却的机理和发汗冷却研究的发展历程，说明了发汗喷管不同研究阶段的典型结构，并重点阐述了可望很快应用于工程上的发汗喷管结构，同时列出了发汗喷管计算中关键技术－热量交换的有关数学模型和各参数的取值。指出了近期需要开展的工作。     

信号采集卫星系统星地资源快速调度优化方法

针对信号采集卫星系统中,采集目标的优先级和携带的信息量在星地资源调度过程中不断随时间变化的特点,提出了一种基于二次映射编码的动态调度差分演化算法（QMDSDE）。算法将采集目标的优先级和携带的信息量进行加权,作为采集的收益。在迭代求解时,根据卫星可见时间窗口的周期性特点设置固定的检测频率,以当前时刻所有目标收益的平均值和敏感系数的乘积作为检测环境变化的阈值。当检测算子的值大于阈值时,算法通过前向预测模型动态调整搜索方向,寻找问题的实时Pareto最优解。算法采用二次映射编码消除星地资源组合中的无效解,降低了算法的搜索空间,提高了算法的求解速度。经仿真校验,该方法在信号采集过程中,可以得到收益较好的星地资源调度方案,且具备较快的收敛速度。