航空发动机转子系统动力学模型的可逆化简化方法

针对航空发动机高压转子系统动力学模型,给出了一种模型可逆化简化的方法.首先采用有限元法建立了较为精确的动力学模型,然后基于质心集中方法对该模型进行了不同程度的简化,分别得到了单跨双盘模型和单盘模型,并将其与原始模型进行了临界转速的对比.这是一种从结构特点将实际多盘转子简化成单盘转子的方法,它使得在考虑到支承等非线性因素后利用低维非线性动力学理论进行分析和参数优化成为可能.另一方面,研究了模型简化方法的可逆性,即基于质心位置及总质量最优的原则,由单跨双盘模型的圆盘结构参数反推了多级圆盘的等效内外半径、厚度、位置等参数,构建了新的工程结构模型,对比该模型和原始模型的前3阶临界转速,误差均在3%之内.这种由简化模型参数反推多级圆盘的方法,为由非线性动力学理论优化分析所得到的简化模型优化结构参数反推设计多级圆盘工程结构参数奠定了基础.      

突肩叶尖尾缘开槽对间隙流动换热特性的影响

通过数值计算对带有尾缘开槽结构的突肩叶尖间隙流场结构、泄漏流量、泄漏损失、表面传热系数进行了对比研究.研究结果显示:相比全突肩叶尖,吸力侧尾缘开槽突肩叶尖可以改变开槽附近泄漏流的流动路径,有效抑制其与主流的掺混.压力侧尾缘开槽和吸力侧尾缘开槽均会增加间隙泄漏流量.压力侧尾缘开槽突肩叶尖会增加间隙泄漏损失,开槽长度越大损失越大.研究范围内的吸力侧尾缘开槽均会减小间隙泄漏损失,但存在最佳开槽长度.压力侧和吸力侧尾缘开槽均会轻微地增加叶尖表面传热系数.      

涡扇发动机空气流量测量飞行试验

以某型涡扇发动机科研试飞为平台,设计搭建了发动机空气流量测量试验系统,进行了各种飞行工况及涡扇发动机工作状态下的空气流量测量试验研究.通过对试验数据的分析和研究,评估了各计算参数对涡扇发动机空气流量测量结果的影响规律,验证了一种简化流量测量方法的可行性和结果的准确性.获得了空气流量测量、计算方面的若干重要结论,为后续型号流量测量和计算提供了工程参考依据.应用试验数据对三维数值计算模型进行修正,并计算了相应工况下的空气流量,计算数据和试验数据进行比较,发现吻合良好,误差较小.      

TiN/Ti强韧涂层在砂尘高速冲蚀下的失效机理

利用高速连续冲蚀试验系统,在不同的冲击角及供砂量下,对有无TiN/Ti强韧涂层的不锈钢试件进行了砂尘高速冲蚀试验,获得了试件的质量冲蚀率。采用扫描电镜(SEM)对涂层损伤表面及断面形貌进行观测与分析,研究TiN/Ti涂层在不同冲击条件下的失效机理。结果表明:TiN/Ti涂层质量冲蚀率随冲击角及供砂量的增加而增加。在低冲击角下,砂尘粒子的切削作用是导致涂层材料剥落的主要原因;高冲击角下,砂尘冲击引起的裂纹萌生及扩展致使涂层材料块状破碎而剥落。TiN/Ti涂层显著提高了不锈钢的抗冲蚀性能,尤其是在低冲击角下。低冲击角下,涂层能将不锈钢的冲蚀性能提高约5倍;高冲击角下能提高约2倍。      

基于前缘平行射流的缝翼噪声控制研究

为了降低缝翼噪声,提出了一种基于前缘平行射流的缝翼噪声控制技术,利用数值计算验证了该方法的有效性,并分析了其噪声控制机理。采用FREQUENZ两段翼型,利用DDES混合方法进行二维非定常数值计算,获取声源分布,采用FW-H积分获得远场噪声特性。计算结果表明平行射流基本不影响翼型的气动力特性,同时缝翼的中低频噪声得到有效的抑制,宽频噪声强度也有所减弱。通过对时均流场和瞬态流场的分析,初步阐述了两种降噪机理:(1)平行射流与缝翼尖端分离流相互作用,改变了剪切层中的大尺度拟序结构,展向涡的尺度及其不稳定性均得到有效抑制,从而减弱了剪切层与缝翼压力面撞击而产生的压力脉动,达到降低声源强度的目的;(2)射流减小了回流速度,削弱了声反馈机制。     

克努森数在微尺度相似流动特性研究中的作用

为了研究克努森数对微尺度相似流动的影响,选取孔径分别为3,1,0.5,0.3mm的相似小孔模型并视流体为连续介质,在相同的雷诺数下对各尺度小孔流体克努森数不同和相同的情况进行数值模拟,计算小孔的质量流量系数并分析其内部流场特征.结果表明:在相同的雷诺数下,原件与放大件的内部流场在克努森数相同时表现出更好的相似性,小孔质量流量系数也表现出更好的吻合性,因此在采用相似放大模型研究微小尺度结构的流动特性时,为了得到更为准确的结果,必须保证相似放大件和微尺度原件克努森数相同.      

RBCC-RKT两级入轨飞行器起飞质量估算方法

针对液体火箭发动机真空比冲基本不变,火箭基循环组合发动机(RBCC)比冲随着飞行条件不断变化的特点,提出了将增广拉格朗日遗传算法优化第一级飞行弹道与传统液体火箭质量估算方法估算第二级起飞质量相结合,获得水平起飞两级入轨RBCC-RKT飞行器第一级起飞质量的估算方法,为总体方案初步设计论证提供参考.通过算例,分析了一级RBCC飞行器惰性质量比、最高动压,气动特性与起飞质量之间的关系.计算表明,降低RBCC飞行器惰性质量比、提高一级飞行器最大飞行动压、提高飞行器升阻比,都能有效地降低一级起飞质量.     

涡轮与冲压组合动力高温进气预冷特性

针对涡轮基冲压组合循环发动机中高温进气影响涡轮发动机性能的问题,开展实际某高空模拟试验进气预冷段的数值分析.基于欧拉-拉格朗日多相流方法解析气液两相热质传输过程,探索射流冷却对不同高空高马赫数进气条件时预冷段内温度和压力的沿程变化规律.结果表明,射流冷却对流场具有明显地温降效果.带有射流装置的预冷段内流动损失是以由黏性...     

Two energy release processes for CMEs: MHD catastrophe and magnetic reconnection

It remains an open question how magnetic energy is rapidly released in the solar corona so as to create solar explosions such as solar flares and coronal mass ejections (CMEs). Recent studies have confirmed that a system consisting of a flux rope embedded in a background field exhibits a catastrophic behavior, and the energy threshold at the catastrophic point may exceed the associated open field energy. The accumulated free energy in the corona is abruptly released when the catastrophe takes place, and it probably serves as the main means of energy release for CMEs at least in the initial phase. Such a release proceeds via an ideal MHD process in contrast with nonideal ones such as magnetic reconnection. The catastrophe results in a sudden formation of electric current sheets, which naturally provide proper sites for fast magnetic reconnection. The reconnection may be identified with a solar flare associated with the CME on one hand, and produces a further acceleration of the CME on the other. On this basis, several preliminary suggestions are made for future observational investigations, especially with the proposed Kuafa satellites, on the roles of the MHD catastrophe and magnetic reconnection in the magnetic energy release associated with CMEs and flares.     

Solar energetic particle events during the rise phases of solar cycles 23 and 24

We present a comparative study of the properties of coronal mass ejections (CMEs) and flares associated with the solar energetic particle (SEP) events in the rising phases of solar cycles (SC) 23 (1996–1998) (22 events) and 24 (2009–2011) (20 events), which are associated with type II radio bursts. Based on the SEP intensity, we divided the events into three categories, i.e. weak (intensity < 1 pfu), minor (1 pfu < intensity < 10 pfu) and major (intensity ? 10 pfu) events. We used the GOES data for the minor and major SEP events and SOHO/ERNE data for the weak SEP event. We examine the correlation of SEP intensity with flare size and CME properties. We find that most of the major SEP events are associated with halo or partial halo CMEs originating close to the sun center and western-hemisphere. The fraction of halo CMEs in SC 24 is larger than the SC 23. For the minor SEP events one event in SC23 and one event in SC24 have widths < 120° and all other events are associated with halo or partial halo CMEs as in the case of major SEP events. In case of weak SEP events, majority (more than 60%) of events are associated with CME width < 120°. For both the SC the average CMEs speeds are similar. For major SEP events, average CME speeds are higher in comparison to minor and weak events. The SEP event intensity and GOES X-ray flare size are poorly correlated. During the rise phase of solar cycle 23 and 24, we find north–south asymmetry in the SEP event source locations: in cycle 23 most sources are located in the south, whereas during cycle 24 most sources are located in the north. This result is consistent with the asymmetry found with sunspot area and intense flares.