旋转状态下气膜冷却换热特性的实验研究

基于一个平板叶片模型对旋转状态下气膜冷却现象的换热特性进行了实验研究,得到不同吹风比情况下气膜冷却换热系数随主流雷诺数和旋转数变化的分布规律。实验利用热色液晶(TLC)测温技术对叶片表面的二维温度场进行测量,采用空气和二氧化碳模拟不同冷气与主流的密度比,并使用无线遥测技术对旋转系中的温度信号加以采集。结果表明：由于受到离心力与哥氏力的综合作用,叶片压力面与吸力面上的强化换热区域向高半径处发生偏转,且偏转趋势在吸力面上更为明显;随着主流雷诺数的增大,压力面上的换热系数不断增大,而在吸力面上则先减小后增大;此外,主流雷诺数的变化对压力面和吸力面上强化换热区域的偏转现象没有明显影响。     

Interactions of solar wind plasma with dust grains: Effects of strong plasma anisotropy

In this paper we re-examined the fundamental physics of charging of a dust particle in the moon environment by tenuous anisotropic solar wind plasma. The majority of work on dusty (complex) plasmas is largely concerns with laboratory plasmas, in which charging process of dust grains is very fast, thus making practical the working concept of dynamically equilibrium floating potential and grain charge. However, solar wind plasma parameters are considerably different at the moon orbit, and we found the characteristic charging time of lunar dust grains to be considerably longer, ranging from 3 to 4.6 min for micron size particles, and up to 7.6 h for 10-nm grains, depending on the value of plasma streaming velocity. These findings make it clear that the transient stage of charging process is important in the moon environment, and equilibrium floating potential and grain charge could be considered as long time asymptotic values. For this reason we re-formulated the moon dust charging process as an inherently time-dependent problem and derived the time-dependent charging equation for the grain potential for general case of anisotropic solar wind plasma. Using the results of our kinetics analysis we found that the distribution of charge density over grain surface submerged into solar wind plasma is highly anisotropic, thus making the OML model, which is based on the assumption of isotropic distribution of surface charge density, not applicable to the grain charging problem by the solar wind plasma.     

December 2006 solar extreme events and their influence on the near-Earth space environment: “Universitetskiy-Tatiana” satellite observations

The Russian microsatellite “Universitetskiy-Tatiana” was launched on Jan. 20, 2005 and was both a scientific and educational mission. Its two main aims were declared as: (1) monitoring of the energetic particles dynamics in the near-Earth space environment after solar events and during quiet times, (2) educational activities based on experimental data obtained from the spacecraft. In this paper observations acquired during Dec. 5–16, 2006, known as “Solar Extreme Events 2006”, were analyzed. The “Universitetskiy-Tatiana” microsatellite orbit permits one to measure both solar energetic particle dynamics, variations of the boundary of solar particle penetration, as well as relativistic and sub-relativistic electrons of the Earth’s outer radiation belt during and after magnetic storms. Both relativistic electrons of the Earth’s outer radiation and solar energetic particles are an important source of radiation damage in near-Earth space. Therefore, the presented experimental results demonstrate the successful application of a small educational spacecraft both for scientific and educational programs.     

Solar particle dynamics during magnetic storms of July 23–27, 2004

It is a case study of a chain of three magnetic storms with a special attention to the particle dynamics based on CORONAS-F and SERVIS-1 low altitude satellite measurements. Solar proton penetration inside the polar cap and inner magnetosphere and dynamics at different phases of the magnetic storms was studied. We found, that solar protons were captured to the inner radiation belt at the recovery phase of the first and the second magnetic storms and additionally accelerated during the last one. No evidence of sudden commencement (SC) particle injection was found. Enhanced solar proton belt intensity with small pitch angles decreased slowly during satellite orbits for 30 days until the next magnetic storm. Then in 20–30 h we registered strong precipitation of these protons followed by the trapped proton flux dropout. Intensity decrease was more pronounced at lower altitudes and higher particle energies.     

Global dynamics of high area-to-mass ratios GEO space debris by means of the MEGNO indicator

In this paper we provide an extensive analysis of the global dynamics of high-area-to-mass ratios geosynchronous (GEO) space debris, applying a recent technique developed by Cincotta and Simó [Cincotta, P.M., Simó, C.Simple tools to study global dynamics in non-axisymmetric galactic potentials–I. Astron. Astrophys. (147), 205–228, 2000.], Mean Exponential Growth factor of Nearby Orbits (MEGNO), which provides an efficient tool to investigate both regular and chaotic components of the phase space.     

The Expansion of Coronal Plumes in the Fast Solar Wind

Coronal plumes are believed to be essentially magnetic features: they are rooted in magnetic flux concentrations at the photosphere and are observed to extend nearly radially above coronal holes out to at least 15 solar radii, probably tracing the open field lines. The formation of plumes itself seems to be due to the presence of reconnecting magnetic field lines and this is probably the cause of the observed extremely low values of the Ne/Mg abundance ratio. In the inner corona, where the magnetic force is dominant, steady MHD models of coronal plumes deal essentially with quasi-potential magnetic fields but further out, where the gas pressure starts to be important, total pressure balance across the boundary of these dense structures must be considered. In this paper, the expansion of plumes into the fast polar wind is studied by using a thin flux tube model with two interacting components, plume and interplume. Preliminary results are compared with both remote sensing and solar wind in situ observations and the possible connection between coronal plumes with pressure-balance structures (PBS) and microstreams is discussed. This revised version was published online in June 2006 with corrections to the Cover Date.     

航空发动机风车不平衡适航符合性验证

CCAR 25部《运输类飞机适航标准》对航空发动机的持续转动提出明确要求,即航空发动机的持续转动不会危及飞行安全。参考美国联邦航空局（FAA）第25-141号修正案,详细分析了FAR 25.362条款对发动机失效载荷的要求及其适用的符合性验证方法。通过对服役数据进行统计学分析研究了风车不平衡符合性验证条件。结果表明,不平衡量等于1.0与1 h备降时间组合、不平衡量等于1.0与最大不超过3 h备降时间组合可以满足安全性的要求,在此基础上从载荷、强度、耐久性、系统完整性以及人为因素5个方面开展符合性验证。采用完整的飞机模型和发动机模型进行符合性验证是可以接受的。机体结构模型要通过地面振动试验进行校验,发动机模型要通过风扇叶片脱落试验进行校验。     

宽温范围内光纤陀螺输入轴失准角误差 及补偿技术研究

随着光纤陀螺使用精度的提升,输入轴失准角误差对光纤惯组精度的影响也愈发突出.为了抑制光纤陀螺失准角误差,提升惯性系统精度,分析了失准角误差的产生原因,提出了设计与生产过程中减小失准角误差的工艺要求;分析了温度环境下失准角误差补偿方法的物理意义,进而推导得出其方法误差;对多组全温范围内(-40℃~+60℃)失准角实测数据进行逐步回归分析,确定失准角误差拟合模型.试验表明,采用该补偿方法最高能够降低92%的失准角误差.     

UMAC伺服同步控制技术在轨迹制孔上的实现

根据轨迹制孔设备的结构特点和工艺需求,设计研制了一套基于UMAC多轴运动控制器的轨迹制孔控制系统.阐述了UMAC多轴运动控制器的硬件调试系统搭建、软件的应用和设计方法,同时重点介绍了虚轴同步技术在轨迹制孔控制系统中的应用,通过运动控制并给出了测试记录和制孔试验,验证了基于UMAC的伺服同步控制技术在多轴运动控制器在轨迹制孔设备中的实际应用效果的有效性.     

航空发动机自动平衡技术发展综述

针对航空发动机在运行过程中不平衡振动过大的问题,采用自动平衡技术进行在线质量补偿,可有效降低其振动水平。目前自动平衡技术主要运用于航空发动机结构、控制算法、工程应用3个方面。基于影响系数法的电磁驱动型自动平衡在美国空军C-130H运输机上得到工程应用,飞行测试4个发动机螺旋处的振动均低于1.27mm/s,降低了94%,因螺旋桨振动导致的压气机处振动降低了75%。研究结果表明:航空发动机自动平衡技术可实现在线持续动平衡,能有效降低发动机及其组件的振动疲劳损伤,降低发动机维护费用,延长维修周期。自动平衡技术在航空发动机领域得到工程应用是一个循序渐进的过程,还需要进一步开展结构设计、控制策略、系统集成等方面的研究工作,并在航空发动机设计阶段就考虑纳入自动平衡结构。