球面收敛二元矢量喷管气动及红外特性研究:模拟高空状态

针对高空状态下球面收敛二元矢量喷管排气系统,通过数值模拟研究了喷管俯仰偏转角对排气系统气动和红外辐射特性的影响,并与地面状态进行了对比分析.在该研究参数范围内,研究结果表明:在俯仰偏转角为20°范围内,俯仰偏转对排气系统推力系数和总压恢复系数的影响微弱,气动推力矢量角与俯仰偏转角几乎相等,高空状态下,喷管的推力系数和总压恢复系数下降0.5%与1.1%;热喷流峰值红外辐射强度仅为地面状态的12%~24%,排气系统的总体红外辐射强度峰值与地面状态下的比值峰值在0.35~0.45之间;随着下俯仰偏转角的增加,排气系统红外辐射峰值呈现下降的趋势.      

双列调心滚子轴承摩擦力矩的特性

基于滚动轴承的动力学理论,建立了双列调心滚子轴承动力学微分方程与摩擦力矩数学模型,采用预估-校正GSTIFF(gear stiff)变步长积分算法求解其动力学微分方程,研究了结构参数和工况参数对双列调心滚子轴承摩擦力矩特性的影响。研究结果表明:较小的内滚道密合度与较大的外滚道密合度有利于降低轴承的摩擦力矩;过大、过小的保持架兜孔曲率半径都不利于轴承摩擦力矩的降低,存在一个合理的保持架兜孔曲率半径使轴承摩擦力矩最小;保持架兜孔间隙对轴承的摩擦力矩影响较小,适当增大保持架引导间隙可有效减小轴承的摩擦力矩;适量的增大双列调心滚子轴承径向游隙有利于降低轴承的摩擦力矩。      

复杂形式球型收敛调节片喷管内流场计算及分析

为了分析复杂形式球型收敛调节片喷管(SCFN)三维内流场特性, 对六角形和领结形的SCFN进行几何建模, 并利用N-S方程和S-A模型, 对两种喷管在不同落压比(NPR)下进行了内流场数值模拟.研究表明, 计算结果与实验结果吻合较好;在此基础上, 对两种喷管的流场特性及性能进行了比较分析.      

矿化剂氧化铝的形貌对二氧化硅基陶瓷型芯性能的影响

制备了矿化剂为氧化铝的二氧化硅基陶瓷型芯,研究了矿化剂粉体粒径、形状等形貌特征对陶瓷型芯性能的影响。结果表明:随着氧化铝粉体粒径的增大,浆料流动性逐渐降低,加入氧化铝球形粉有利于改善浆料的充型性能;加入不规则形状氧化铝粉时,随着氧化铝粉体粒径的增大,型芯的烧结收缩率减小;加入球形氧化铝粉时,其粉体形状和粒径大小对收缩率和室温抗弯强度无明显影响,但导致较大的高温变形量。     

纤维缠绕球形贮箱刚度分析

对纤维缠绕球形贮箱在外压、内压和温差等作用下,进行应力、变形和稳定性等结构刚度分析。结果表明,与金属材料贮箱相比,纤维缠绕球形贮箱具有显著的刚度约束条件,如临界卸载内压和临界温差等。纤维缠绕球形贮箱在按强度要求进行结构设计和分析的基础上,还需校核刚度约束条件。为此,提出了纤维缠绕球形贮箱结构稳定性的各类临界载荷包括外压、卸载内压和温差等的计算公式及判据,为结构方案设计和研制的试验提供参考。     

精密球体零件加工工艺的研究与应用

球体零件是某国家重点型号发动机某一球阀的核心零件,它具有高形位公差要求、形状不规则、表面质量要求高等特点,给实际的加工生产带来极大难度,该零件被列入某国家重点型号发动机研制中的关键工艺技术之一.通过反复试加工与参数摸索,在充分了解铝材质球体零件结构特点及加工难点的基础上,总结出一套粗加工、半精加工、精加工的加工工艺流程方法,并依据金属材料热处理原理在粗加工后、精加工前分别穿插进行不同热处理以达到消除粗加工去除大余量过程中产生的机械加工应力与稳定零件尺寸的目的,最后采用自制辅助工装夹具、刀具选择以及优化切削参数等措施,成功生产出一批完全满足设计要求的精密球体零件,装配该球体零件的球阀顺利通过热试车考核.     

五棱镜面形误差对中心入射光线的转向角影响

针对五棱镜面形误差引起出射光线转向角误差,进而影响空间光电跟瞄系统多光轴标校精度的问题,提出了一种研究五棱镜面形误差对出射光线转向角影响的新方法.首先,在五棱镜不规则度较小的前提下,利用最佳拟合球面矢高适当简化了五棱镜的工作面模型,推导出了出射光线转向角计算公式,并将影响出射光线转向角误差的因素限定在了6个非独立随机变...     

半球型零件球面精密珩磨技术研究

作为精密加工技术之一,珩磨工艺往往用于内孔的光整加工.本文在分析球面研磨与珩磨加工特点的基础上,对球面精密珩磨加工技术进行深入研究,主要包括球面珩磨加工原理,珩磨头磨料选取和结构设计,球面珩磨速度参数对表面轨迹的影响,以及珩磨头压力对加工效果的影响研究.根据以上研究结果,对一批产品进行工艺试验,结果表明,采用球面珩磨技术加工出的零件能够满足产品的各项精度指标,同时加工效率较球面研磨提高3倍.     

Solar Wind Control of the Magnetospheric and Auroral Dynamics

A dependence of the polar cap magnetic flux on the interplanetary magnetic field and on the solar wind dynamic pressure is studied. The model calculations of the polar cap and auroral oval magnetic fluxes at the ionospheric level are presented. The obtained functions are based on the paraboloid magnetospheric model calculations. The scaling law for the polar cap diameter changing for different subsolar distances is demonstrated. Quiet conditions are used to compare theoretical results with the UV images of the Earth’s polar region obtained onboard the Polar and IMAGE spacecrafts. The model calculations enable finding not only the average polar cap magnetic flux but also the extreme values of the polar cap and auroral oval magnetic fluxes. These values can be attained in the course of the severe magnetic storm. Spectacular aurora often can be seen at midlatitude during severe magnetic storm. In particularly, the Bastille Day storm of July 15–16, 2000, was a severe magnetic storm when auroral displays were reported at midlatitudes. Enhancement of global magnetospheric current systems (ring current and tail current) and corresponding reconstruction of the magnetospheric structure is a reason for the equatorward displacement of the auroral zone. But at the start of the studied event the contracted polar cap and auroral oval were observed. In this case, the sudden solar wind pressure pulse was associated with a simultaneous northward IMF turning. Such IMF and solar wind pressure behavior is a cause of the observed aurora dynamics.     

A statistical analysis of low frequency geomagnetic field pulsations at two Antarctic geomagnetic observatories in the polar cap region

The aim of this study is to investigate the characteristics of low frequency (∼0.5–5 mHz) geomagnetic field fluctuations as recorded at two Antarctic stations within the polar cap: the Italian observatory Mario Zucchelli Station (TNB) and the French–Italian observatory Dome C (DMC) in order to investigate the spatial extension and propagation characteristics of the phenomena observed at very high latitude. The stations have approximately the same geographic latitude, but a very different corrected geomagnetic latitude, being DMC close to the geomagnetic pole and TNB closer to the auroral oval.