超临界碳氢燃料的射流特性研究

针对未来先进航空发动机的超临界燃油喷射混合问题,采用纹影法对超临界正十烷(n-decane)/正戊烷(n-pent ane)混合物在静止环境中的射流激波结构进行试验,同时采用理论分析的方法研究了射流的相变途径和流量特性。纹影照片显示,在试验工况下射流在喷口附近呈现出马赫波等激波结构,燃料的压力是激波结构的主要影响因素。理论分析表明:在混合物的临界点附近,燃料压力较高时更有可能导致相变。由于物性的不同,大分子与小分子碳氢燃料的相变途径存在一定的差异,小分子燃料在喷射过程中更容易发生冷凝。采用1维等熵计算方法可以较精确地计算高温高压碳氢燃料的流量。     

前缘喷淋射流对导叶压力面冷却特性的影响

为了评估涡轮导叶的前缘喷淋射流对压力面多排气膜孔冷却特性的影响,在高亚声速风洞中进行了实验,获得了有无前缘喷淋射流时叶片表面的气膜冷却效率和传热系数。叶栅进口雷诺数(基于叶片弦长)范围为2.0×105~4.0×105,出口等熵马赫数为0.95,叶片前缘和压力面分别都包含6排圆形孔,质量流量比的范围分别为2.46%~4.57%和2.00%~3.71%。实验结果表明:在没有前缘喷淋射流时,压力面前半段的气膜冷却效率受质量流量比的影响较小,而后半段的气膜冷却效率随着质量流量比升高而增大。前缘喷淋射流使压力面多排气膜孔的冷却效率提高了20%~70%,并且使气膜冷却效率沿流向分布更均匀。不论是否有前缘喷淋射流,压力面的传热系数比都随质量流量比升高而增大,沿流向看,前缘喷淋射流提高了压力面前缘和尾缘区域的传热系数比而对压力面中间区域影响较小。     

聚碳硅烷的分子量和流体力学特性表征

通过研究聚碳硅烷溶液的流体力学参数与分子量的关系以及比浓黏度与浓度的关系,得到了聚碳硅烷的分子结构信息。结果表明,聚碳硅烷绝对重均分子量M_w为1.098×10⁴ g/mol,分子量分布MWD为6.7,第二维利系数A₂为1.57×10^-3 cm³·mol/g²,Huggins常数k’为1.85,流体力学半径与分子量间的标度指数b为0.21。在室温条件下,良溶剂四氢呋喃稀溶液中,聚碳硅烷链段空间分布较为紧密,分子链为非线型结构。     

超燃冲压发动机流量匹配机理

采用基于集总参数方程的燃烧室性能计算模型,辅以临界面积法,应用于隔离段和燃烧室的一维流场计算,实现了双模态超燃冲压发动机各种模态下的隔离段和燃烧室的流量匹配计算,并分析了流量匹配工作机理.结果表明:在未分离超燃模态与分离超燃模态下,增加燃烧室供油流量,隔离段和燃烧室流量匹配是通过流道中的喉道处马赫数降低来实现的;在跨燃模态与亚燃模态下,增加燃烧室供油流量,流量匹配主要是通过提高燃烧室流道中热力喉道处的总压来实现的.      

双辐板涡轮盘/榫结构优化设计方法

提出双辐板涡轮盘/榫三维结构优化设计方法,包括:以盘/榫总质量作为目标函数,分部管理的设计参数,盘/榫结构分部快速优化/整体精细优化策略;基于ANSYS软件,建立了双辐板涡轮盘/榫结构优化设计平台.针对某高压涡轮转子,设计了两种双辐板涡轮盘/榫模型,分析了盘缘喉部半径、盘缘厚度参数对盘/榫危险区应力的影响.优化结果表明:双辐板涡轮盘比单辐板涡轮盘应力分布更加均匀;在满足结构强度约束条件下,两种双辐板涡轮盘分别比单辐板涡轮盘减质19.90%和17.35%;对双辐板涡轮盘/榫模型进行优化,采用该优化设计方法的计算时间仅为采用常规三维优化方法的1/3,表明其优化设计方法的合理性及高效性.      

吸附式压气机叶型和抽吸方案优化设计

将智能优化算法与准三维叶栅计算程序相结合,对某吸附式压气机叶型进行了优化设计,对优化设计前后的流场进行了详细分析.优化设计之后叶型总压损失下降40%,静压升提高0.6%.优化得到最佳抽吸位置位于分离区起始点上游,优化叶型具有更均匀的负荷分布,并且优化后叶型的性能在全攻角范围内均得到了提升.结果表明:更均匀的负荷分布会提高叶型的性能,减小叶型分离,降低抽吸所需要的能量.对于在尾缘处存在轻微分离的叶型其最优抽吸位置位于分离区上游.     

基于序列采样算法的轮盘减质优化

介绍了一种基于蒙特卡罗表述的空间缩减策略和局部边界线搜索的序列采样算法,该算法利用已有样本点的信息缩减原有设计空间,使得在缩减设计空间上生成的新样本点能够同时具有良好的空间填充特性和投影特性.与已有的序列采样算法的比较结果表明,该算法具有较高的采样效率和采样质量.采用此序列采样算法结合Kriging模型和遗传算法进行轮盘减质优化,优化结果减质10%.该序列采样算法为工程结构的优化提供了一条灵活有效的途径.      

轮体结构颗粒阻尼器设计方法

利用离散元法及正交设计方法,对典型轮体结构发生伞形振动时的二维等效振动模型进行了空腔尺寸及颗粒填充方案的数值设计,并结合振动试验结果给出了轮体结构颗粒阻尼器的设计流程及设计准则.研究表明:1建立的二维等效振动模型在能够反映轮体结构伞形振动基本特征的同时,也可以较为准确地模拟内部颗粒运动对结构产生的影响;2颗粒阻尼对轮体结构的振动有明显的改善作用,但填充不同材质的颗粒,其减振效果会有较为明显的区别;3空腔的尺寸及颗粒的质量率对颗粒阻尼的影响显著,应首先保证的是较高的颗粒质量率;4由于碰撞间隙的作用,对于固定规格的空腔和颗粒,存在最佳颗粒体积填充率使得颗粒阻尼的减振效果最佳.由试验与数值模拟的最佳方案的一致性可知,发展的设计方法可以较为准确地给出轮体结构颗粒阻尼器的最优空腔尺寸及其对应的最佳填充方法,可用于轮体结构伞形振动减振方案的前期设计.     

An empirical relation to correct storm-time thermospheric mass density modeled by NRLMSISE-00 with CHAMP satellite air drag data

With the help of STAR (Spatial Triaxial Accelerometer for Research) accelerometer measurements on board CHAMP (Challenging Minisatellite Payload), the global distributions of total mass density changes at about 400 km height during major magnetic storms are studied, aiming to improve the capability of current thermospheric model for predicting the storm-time mass density distribution. The density calculated by the NRLMSISE-00 model without using the geomagnetic active index as input is taken as a reference on top of which the storm-time changes are added. In total 19 storm events during 2001–2004 are used to perform a comprehensive statistical analysis. A relative calibration of drag coefficient along with accelerometer calibration parameters is made by fitting the CHAMP observed initial mass densities in with the NRLMSISE-00 model on quiet days before each storm. The dependences of the storm-time changes in mass density on both the total global Joule heating power, ∑_Qj$\sum Q_{\text{j}}$ and the high-resolution ring current index, Sym-H, are investigated. The lag times of mass density changes with respect to the Joule heating and Sym-H variation are obtained as a function of latitude and sunlight. By using a multiple linear regression analysis with proper time shift, an empirical relation connecting storm-time changes in mass density for 400 km height with the two parameters, ∑_Qj$\sum Q_{\text{j}}$ and Sym-H, has been worked out for different latitude and sunlight conditions (day-side or night-side). Adding a correction calculated from the empirical relation to the NRLMSISE-00 model reference leads to a better prediction of storm-time thermospheric mass density distribution.     

Kuafu and the studies of CME initiation

We first briefly review the current trend in the studies of coronal mass ejections (CMEs), then summarize some recent efforts in understanding the CME initiation. Emphasis has been put on the studies of Earth-directed CMEs whose associated surface activity and large scale magnetic source have been well identified. The data analysis by combining the MDI full disc magnetograms, vector magnetograms of active regions, EUV waves and dimmings, non-thermal radio sources, and the SOHO LASCO observations has shed new light in understanding the CME magnetism. However, the current studies seem to invoke new observations in a few aspects: (1) The observations which enable us to trace CMEs from the earliest associated surface activity to its initial acceleration and key development in the low corona in the height of 1–3 R; (2) The imaging spectroscopic observations which can be used to diagnose the early plasma outflow and the line-of-sight velocity in understanding the kinematics of CMEs; (3) The accurate timing from primary magnetic energy release, manifested by chromospheric activity, non-thermal radio bursts, and EUV, X-ray and γ-ray emissions, to the CME initiation, early acceleration and propagation, and the consequences in the interplanetary space and magnetosphere. The Kuafu Mission will meet the basic requirement for the new observations in CME initiation studies and serve as a monitor of space weather of the Sun–Earth system.