薄壁交叉圆柱滚子轴承最佳径向工作游隙

以型号为RA8008UUCC0对数修形的薄壁交叉圆柱滚子轴承为分析对象,借助RomaxDesigner软件对比分析在联合载荷作用下径向工作游隙对承载滚子数、滚子最大载荷、滚道应力分布、轴承刚度、最小油膜厚度和疲劳寿命的影响情况,得出径向工作游隙是影响轴承力学性能的关键因素,结果表明:轴承受载滚子数随游隙的减小而增多,滚子与滚道接触应力分布趋于均匀化,相同条件下,倾覆力矩的影响比较显著。联合载荷作用下,随着工作游隙的减小,轴承刚度增大。当径向工作游隙小于-0.002mm时,随着径向工作游隙绝对值的增大,滚子与滚道接触变形减小,接触应力增大,刚度增大,最小油膜厚度减小,轴承寿命降低。同一径向工作游隙下,倾覆力矩可以减小滚子与轴承内外圈之间的油膜厚度,从而显著降低轴承疲劳寿命,轴承最佳径向工作游隙范围为-0.004~0mm。     

磁控等离子体对尾喷管壁传热特性的影响

根据磁场作用下等离子体的湍流和传热能力将受到抑制的现象, 提出利用磁场控制低温等离子体隔离高温燃气与喷管壁的方法, 以减少高温燃气对壁面的传热, 从而达到降低壁面温度的目的.分别建立诱导磁场方程求解洛伦兹力和磁场作用下的k-ε湍流模型求解湍流粘度, 数值模拟了不同强度磁场作用下的磁控等离子体流动和传热特性.结果表明, 磁场能够有效地抑制湍流强度, 降低传热能力, 从而有效地降低壁面温度;并且磁场越强, 效果越明显.      

滚动轴承支承下的转子碰摩故障动力分析、特征提取与智能诊断

针对滚动轴承支承下的转子碰摩故障诊断问题,考虑滚动轴承非线性赫兹接触和轴承径向间隙,建立了含不平衡-碰摩耦合故障的转子-滚动轴承系统动力学模型.应用三维谱图分析碰摩诊断依据和确定频段特征,利用仿真数据获取结构最优的神经网络模型,并对试验碰摩故障数据进行诊断,识别率高达90%以上.计算结果充分表明了建立的动力学模型的有效性,同时,研究结果为有效结合故障机理分析与故障智能诊断提供了新的方法.      

应力状态对磁记忆信号的影响

 通过对20#钢试件拉伸时表面磁场的在线测量和20#钢试件经过不同程度拉伸并卸载后的表面磁场的测量,研究应力状态对磁记忆信号的影响。20#钢进行拉伸试验时,在应力集中部位,当变形很小时磁场信号变化平缓;产生一定程度塑性变形后磁场信号变化相对剧烈;出现颈缩现象时磁场信号变化非常剧烈。经分析认为,磁记忆信号的变化与材料内部微观组织的状态有关,试件变形很小时,磁弹性效应对试件表面磁场的变化起主要作用;试件变形较大时,其表面磁场的变化主要受塑性变形区内位错聚集产生的微缺陷的影响。     

Model Development and Adaptive Imbalance Vibration Control of Magnetic Suspended System

对星载磁悬浮单框架控制力矩陀螺,建立其转子的平动与转动的动力学方程。所建模型反映了转子的动、静不平衡特性,以及转子运动与框架、星体运动的耦合关系。模型是主动磁悬浮控制与动框架效应分析的基础。对动、静不平衡量未知的转子,设计了自适应对中控制器。在分散PD、比例交叉反馈控制器与高低通滤波器的基础上,通过动、静不平衡量的辨识与补偿控制,使转子绕其惯量主轴旋转,衰减角动量交换执行机构高速转子因不平衡而对基座产生的干扰力,消除星上主要颤振源,达到降低卫星姿态抖动的目的。     

无电极洛伦兹力推力器技术发展研究

近年来,为了适应深空探测、载人航天、航天器在轨服务等空间任务的需求,大推力、高比冲、长寿命、高推力密度的高功率电推进技术吸引了众多学者的持续关注.相比于其他类型的高功率电推进技术,无电极洛伦兹力推力器(ELF)在推力密度、推重比等指标上具有明显优势,且从原理上克服了电极烧蚀对高功率电推力器寿命的制约,具有广阔的应用前景...     

添加微量铜对FeCoNbSiB合金非晶形成能力及磁性的影响

采用工业用硼铁为主要原料制备一种FeCoNbSiBCu大块非晶合金.采用差示扫描量热分析、X射线衍射分析、扫描电镜及能谱分析对合金的非晶形成能力进行研究.结果表明,通过添加微量Cu可以显著提高FeCoNbSiB合金玻璃形成能力,当添加Cu的原子比含量为0.5at%～0.7at%时,合金的非晶形成能力明显提高.采用振动样品磁强计对铸态样品的软磁性能进行研究.结果表明,当Cu的加入量为0.5at%时,非晶合金的软磁性能得到提高.     

Monopolar structure of the Sun in between polar reversals and in Maunder Minimum

After a polar reversal in one hemisphere the Sun has two polar caps of the same sign, leaving it in a kind of monopolar state. It may take months before a polar reversal occurs in the other hemisphere. The situation may have been extreme in the Maunder Minimum where the northern hemisphere most probably did not have polar reversals during several cycles, while the southern hemisphere may have had some. This may affect the interplanetary field and thus the cosmic rays reaching the Earth. Using the relation between the Wolf number and the speed of the global magnetic field regions the yearly mean Wolf number has to exceed 40 in order to have polar reversals, hence per hemisphere we expect that it must exceed 20. This may be used to give a definition of a deep minimum.     

Variation of energetic particle precipitation with local magnetic time

The detailed study of the precipitation of magnetospheric particles into the atmosphere is complicated by the rather complex spatial configuration of the precipitation region and its variability with geomagnetic activity. In this paper we will introduce polar oval coordinates and apply them to POES observations of 30 keV to 2.5 MeV electrons and comparable protons to illustrate the dependence of particle precipitation on local time and geomagnetic activity. These coordinates also allow an easy separation of the spatial precipitation patterns of solar and magnetospheric particles. The results indicate that (a) the spatial precipitation pattern of energetic magnetospheric electrons basically follows the pattern of the field parallel Birkeland currents up to MeV energies and (b) at least in the mesosphere the influence of magnetospheric electrons is comparable to the one of solar electrons. Implications for modeling of atmospheric chemistry will be sketched.     

New index of long-term variations of galactic cosmic ray intensity

We find that the soft rigidity spectrum of the Galactic Cosmic Ray (GCR) intensity variations for the maximum epoch and the hard rigidity spectrum for the minimum epoch calculated based on the neutron monitors experimental data (1960–2002) are related with the various dependence of the diffusion coefficient on the GCR particle’s rigidity for different epoch of solar activity. This dependence is stronger in the maximum epoch than in the minimum epoch of solar activity, and is provided by the essential temporal rearrangements of the structure of the Interplanetary Magnetic Field (IMF) turbulence from the maxima to minima epoch of solar activity. We also show that the rigidity spectrum of GCR intensity variations is harder for the effective rigidities ∼(10–15) GV (by neutron monitors data), than for the effective rigidities ∼(25–30) GV (by neutron monitors and muon telescopes data). A general scenario of GCR modulation versus solar activity is settled on the essential temporal rearrangements of the structure of the IMF turbulence. Therefore, the temporal changes of the power law rigidity spectrum exponent can be considered as a vital (new) index to explain the 11-year variations of the GCR intensity. We assume that ∼(70–80)% of the changes of the amplitudes of the 11-year variations of GCR intensity is related with the changes of the IMF turbulence versus solar activity.