基于Euler／N—S方程的跨音速非线性静气动弹性问题研究

在C-H网格的基础上,采用Jameson的中心差分有限体积法求解Euler/N-S方程,采用结构影响系数法计算结构的弹性变形,用三角元面积加权法和常体积转换法(CVT)实现流固耦合,计算了弹性后掠机翼在跨音速状态的静气动弹性问题     

Global Response of Martian Plasma Environment to an Interplanetary Structure: From Ena and Plasma Observations at Mars

As a part of the global plasma environment study of Mars and its response to the solar wind, we have analyzed a peculiar case of the subsolar energetic neutral atom (ENA) jet observed on June 7, 2004 by the Neutral Particle Detector (NPD) on board the Mars Express satellite. The “subsolar ENA jet” is generated by the interaction between the solar wind and the Martian exosphere, and is one of the most intense sources of ENA flux observed in the vicinity of Mars. On June 7, 2004 (orbit 485 of Mars Express), the NPD observed a very intense subsolar ENA jet, which then abruptly decreased within ∼10 sec followed by quasi-periodic (∼1 min) flux variations. Simultaneously, the plasma sensors detected a solar wind structure, which was most likely an interplanetary shock surface. The abrupt decrease of the ENA flux and the quasi-periodic flux variations can be understood in the framework of the global response of the Martian plasma obstacle to the interplanetary shock. The generation region of the subsolar ENA jet was pushed towards the planet by the interplanetary shock; and therefore, Mars Express went out of the ENA jet region. Associated global vibrations of the Martian plasma obstacle may have been the cause of the quasi-periodic flux variations of the ENA flux at the spacecraft location.     

A Comparative Study of the Influence of the Active Young Sun on the Early Atmospheres of Earth, Venus, and Mars

Because the solar radiation and particle environment plays a major role in all atmospheric processes such as ionization, dissociation, heating of the upper atmospheres, and thermal and non-thermal atmospheric loss processes, the long-time evolution of planetary atmospheres and their water inventories can only be understood within the context of the evolving Sun. We compare the effect of solar induced X-ray and EUV (XUV) heating on the upper atmospheres of Earth, Venus and Mars since the time when the Sun arrived at the Zero-Age-Main-Sequence (ZAMS) about 4.6 Gyr ago. We apply a diffusive-gravitational equilibrium and thermal balance model for studying heating of the early thermospheres by photodissociation and ionization processes, due to exothermic chemical reactions and cooling by IR-radiating molecules like CO₂, NO, OH, etc. Our model simulations result in extended thermospheres for early Earth, Venus and Mars. The exospheric temperatures obtained for all the three planets during this time period lead to diffusion-limited hydrodynamic escape of atomic hydrogen and high Jeans’ escape rates for heavier species like H₂, He, C, N, O, etc. The duration of this blow-off phase for atomic hydrogen depends essentially on the mixing ratios of CO₂, N₂ and H₂O in the atmospheres and could last from ∼100 to several hundred million years. Furthermore, we study the efficiency of various non-thermal atmospheric loss processes on Venus and Mars and investigate the possible protecting effect of the early martian magnetosphere against solar wind induced ion pick up erosion. We find that the early martian magnetic field could decrease the ion-related non-thermal escape rates by a great amount. It is possible that non-magnetized early Mars could have lost its whole atmosphere due to the combined effect of its extended upper atmosphere and a dense solar wind plasma flow of the young Sun during about 200 Myr after the Sun arrived at the ZAMS. Depending on the solar wind parameters, our model simulations for early Venus show that ion pick up by strong solar wind from a non-magnetized planet could erode up to an equivalent amount of ∼250 bar of O⁺ ions during the first several hundred million years. This accumulated loss corresponds to an equivalent mass of ∼1 terrestrial ocean (TO (1 TO ∼1.39×10²⁴ g or expressed as partial pressure, about 265 bar, which corresponds to ∼2900 m average depth)). Finally, we discuss and compare our findings with the results of preceding studies.     

The Genesis Solar Wind Concentrator Target: Mass Fractionation Characterised by Neon Isotopes

The concentrator on Genesis provided samples of increased fluences of solar wind ions for precise determination of the oxygen isotopic composition. The concentration process caused mass fractionation as a function of the radial target position. This fractionation was measured using Ne released by UV laser ablation and compared with modelled Ne data, obtained from ion-trajectory simulations. Measured data show that the concentrator performed as expected and indicate a radially symmetric concentration process. Measured concentration factors are up to ∼30 at the target centre. The total range of isotopic fractionation along the target radius is 3.8%/amu, with monotonically decreasing ²⁰Ne/²²Ne towards the centre, which differs from model predictions. We discuss potential reasons and propose future attempts to overcome these disagreements.     

静叶片时序效应对压气机叶片非定常气动负荷的影响

采用数值方法对两级低速压气机中径处的流场进行非定常模拟。研究第二排静叶在两个典型周向位置上的叶片气动负荷,分析各列叶栅气动负荷的非定常波动以及静叶时序效应对叶栅气动负荷的影响。对各列叶栅的非定常气动力和气动力矩进行频谱分析,探讨叶列间的非定常气动干扰。结果表明,时序效应对静叶片气动负荷的影响明显高于动叶片的。时序效应能够提高压气机的性能与叶片寿命.      

临近空间动能拦截器神经反演姿态控制器设计

为满足临近空间动能拦截器姿态控制快速性、准确性和鲁棒性的要求,设计了一种自适应神经反演姿态控制器。首先,建立了姿控发动机侧喷干扰模型,并推导了包含质心漂移、参数摄动和外界干扰的三通道强耦合模型;其次,设计了自适应神经反演姿态控制器,为提高控制精度,采用径向基函数（RBF）神经网络对各个通道的不确定项进行估计和补偿,并基于最小学习参数的思想,将神经网络学习参数拟合为一个参数,提高了RBF计算效率,保证了估计的实时性。最后,采用伪速率（PSR）脉冲调制器将设计的连续控制律转化为脉冲控制律,实现了拦截器的变推力控制,并克服了脉冲脉宽调制（PWPF）调制器相位滞后问题。数字仿真表明,所设计的控制器收敛速度快,控制精度高,对强扰动具有鲁棒性。     

吸气式高超声速飞行器非均匀尾喷流试验

在中国空气动力研究与发展中心0.5m高超声速风洞中,开展了非均匀喷流条件下的吸气式高超声速飞行器后体尾喷流/外流干扰测压试验研究。采用非均匀内喷管,模拟飞行器尾喷管非均匀入流,测量了飞行器后体膨胀面及水平翼表面压力,采用高清纹影观测了喷流干扰区域的流场结构,获得了不同工况下非均匀入流对尾部及水平翼表面压力分布的影响规律。试验结果显示尾喷管非均匀入流对飞行器尾部壁面压力分布及流场结构有明显影响,喷管入流的非均匀特征在吸气式高超声速飞行器喷流模拟中不可忽视。非均匀喷流核心区压力分布明显高于均匀喷流时的结果;核心区域外,非均匀喷流的作用面积略小于均匀喷流,且非均匀喷流同外流交叉干扰区域的面积和强度要略小于均匀喷流;均匀喷流在喷管出口区域存在明显的膨胀波系,交叉干扰激波及剪切层的扩张角也大于非均匀入口条件时的结果。     

高阶谐波控制对旋翼桨-涡干扰载荷和噪声的影响

直升机小速度平飞和斜下降飞行时会产生严重的桨-涡干扰(BVI)噪声。基于修正Beddoes尾迹/桨叶动力学耦合方法和Farassat 1A公式,建立了一个新的能够计入高阶谐波控制(HHC)影响的旋翼桨-涡干扰气动载荷和噪声计算模型。在该模型中,高阶谐波控制引起的桨尖涡附加位移通过对高阶入流进行时间积分推导得出,而单一阶次的谐波输入引起的各阶谐波响应通过传递函数来确定,传递函数则由桨叶的动力学特性计算。首先对HARTⅡ旋翼斜下降飞行状态的桨-涡干扰气动载荷进行了计算模拟,验证了所建立方法的可靠性。然后,着重研究了在典型的三阶谐波桨根激励下,不同输入相位对HARTⅡ旋翼桨-涡干扰气动载荷和噪声特性的影响。结果表明:桨叶的动力学特性尤其是扭转特性对高阶谐波控制效果影响显著,且高阶谐波输入的相位选择对桨-涡干扰噪声的控制至关重要,若控制相位选择不当,反而会增大旋翼噪声。     

共轴刚性双旋翼/机身干扰流场数值模拟

采用滑移网格技术求解Navier-Stokes (RANS)方程的方法,研究了共轴刚性双旋翼/机身的干扰问题。通过Caradonna-Tung旋翼、Robin直升机、Maryland直升机旋翼/机身干扰和Harrington 2共轴双旋翼等算例,验证了所提出的旋翼流场数值模拟方法的正确性。在此基础上,以Maryland机身为原型,分析了不同桨距的共轴刚性双旋翼与机身之间的干扰特性。结果表明:所提出的数值模拟方法能够很好地模拟共轴刚性双旋翼/机身的气动干扰特性;由于机身对于共轴刚性双旋翼下洗流场的阻滞作用,旋翼的悬停效率增加5%左右,并且随着拉力系数的增大使得悬停效率的增量更加明显;旋翼的悬停效率增加主要来源于下旋翼0°方位角附近的桨叶升力系数的增大,并且拉力系数的增量由桨根向桨尖方向逐渐减小。      

钝体稳定射流火焰的火焰面模型数值研究

基于稳态火焰面(SLFM)和交互式非稳态欧拉颗粒火焰面(EPFM)模型对Sydney大学CH4/H2钝体稳定湍流扩散火焰行了数值研究,采用修正的雷诺应力模型(RSM),同时对两种不同规模的甲烷详细化学反应动力学机理进行研究,比较了燃烧模型和反应机理对湍流火焰结构、活性自由基以及氮氧化物预测精度的影响,与实验数据对比结果表明:两种反应机理得到的温度场和主要组分分布基本相同;SLFM模型能对速度场和标量场的分布进行较为准确预测,采用EPFM模型修正后,部分区域OH预测结果更加靠近实验结果;采用EPFM模型对SLFM模型耦合GRI-Mech 211的计算结果修正后,NO量级降低近2倍,预测精度明显改善,与实验结果实现较好的符合,验证了化学反应动力学机理以及非稳态效应对氮氧化物预测精度的影响。