基于PIV技术的纵列式双旋翼尾迹特性实验研究

将现有单旋翼实验台进行改装,以适合于纵列式双旋翼的实验研究。基于PIV技术,针对悬停和前飞状态下的纵列式双旋翼时的桨尖涡特性进行了测量。通过改变前后旋翼的水平和轴向间距,调整两旋翼之间的重叠区域,研究了不同气动布局纵列式双旋翼干扰状态下的尾迹结构,并与单旋翼进行了对比。结果表明:悬停状态,随两旋翼纵向间距的增加,桨尖涡的轴向位移也逐渐增大,但桨尖涡径向位移并不是随纵向间距的改变而规律变化,在纵向间距为1.8R附近时最小;而双旋翼轴向间距的变化对桨尖涡的径向和轴向位移均有影响,但变化都不是很大。     

光纤陀螺的温度实验与仿真分析

热致非互易相移的存在影响了光纤陀螺的工作精度.通过对热致非互易相移的分析,把握了该相移与光纤陀螺温度特性的关系.在此基础上,进行了光纤陀螺的温度实验与仿真分析.结果表明,仿真分析光纤陀螺的整体温度分布是可行的;温度实验与仿真分析相结合的办法有助于光纤陀螺温度特性的把握.     

异种金属材料磁脉冲焊接技术

通过对磁脉冲焊接技术结合机理的阐述,采用5A03Al-5A06Al、1050Al-AZ31Mg异种金属材料进行焊接试验.对所得的焊接接头进行气密性试验和剥离试验,检测其结合质量;结合光学显微镜,对比分析Al-Al、Al-Mg焊接接头的微观形貌特点;并采用SEM/EDS分析界面附近的元素分布;最后通过硬度试验,检测接头界...     

多孔质节流空气静压轴承静态性能实验研究

本文采用不锈钢多孔质材料研制了一种新的空气静压轴承,并对不同平均孔径的多孔质空气静压轴承以及一种表面复合节流空气静压轴承的承载能力和刚度进行了实验测试和分析,结果表明,选用合适的不锈钢多孔质材料以及适当的加工方法可以制造高承载能力与高刚度的空气静压轴承。     

常开洞工业厂房风致内压试验研究

通过一系列不同条件下的单个常开洞单跨厂房刚性模型风洞测压试验,分析了风向角、开洞位置、开洞形状以及开洞大小对内压平均值与脉动值的影响,并与基于稳态理论与非定常理论的内压预测值进行了比较。研究发现,单个常开洞厂房内压的空间分布是均匀的,几乎处处相等,仅在开洞附近测点的风压系数值稍有差别;内压的脉动特性主要来源于来流湍流作用、旋涡脱落与尾流干扰以及赫姆霍兹共振等三个方面的影响;内压的均值与均方根值受开洞条件以及风向角等因素影响较大;稳态理论计算得到的内压系数均值与试验所得非常接近,但是均方根值的预测偏保守。非定常理论推导得到的内压响应方程在风速方向正对开洞时可以给出良好的预测,但由于受旋涡脱落、尾流干扰等影响,斜风向时运用该方法预测内压是不合适的。     

细长旋成体大迎角俯仰振荡的数值研究

为研究俯仰振荡对细长旋成体流场与气动特性的影响,利用雷诺平均方法与大涡模拟的混合方法相结合的脱体涡模拟方法对大迎角下细长旋成体俯仰运动进行了数值模拟研究。通过对背风面分离涡的强度和位置、细长体绕流形态、截面压强系数和侧向力系数的观察和分析,发现施加小振幅、特定频率的俯仰振荡对大迎角细长旋成体背风面流场有明显的控制能力,...     

教练机飞行模拟器视景系统的选择

视景系统是飞行模拟器的重要组成部分,是飞行员获取信息的主要渠道。本文以教练机训练任务对视景系统的需求为立足点,回顾了飞行模拟器视景系统的发展简况,分析了主要几种视景系统的原理及技术特点,阐述了教练机飞行模拟器该如何选择视景系统。     

The Magnetic Field of Mercury

The magnetic field strength of Mercury at the planet’s surface is approximately 1% that of Earth’s surface field. This comparatively low field strength presents a number of challenges, both theoretically to understand how it is generated and observationally to distinguish the internal field from that due to the solar wind interaction. Conversely, the small field also means that Mercury offers an important opportunity to advance our understanding both of planetary magnetic field generation and magnetosphere-solar wind interactions. The observations from the Mariner 10 magnetometer in 1974 and 1975, and the MESSENGER Magnetometer and plasma instruments during the probe’s first two flybys of Mercury on 14 January and 6 October 2008, provide the basis for our current knowledge of the internal field. The external field arising from the interaction of the magnetosphere with the solar wind is more prominent near Mercury than for any other magnetized planet in the Solar System, and particular attention is therefore paid to indications in the observations of deficiencies in our understanding of the external field. The second MESSENGER flyby occurred over the opposite hemisphere from the other flybys, and these newest data constrain the tilt of the planetary moment from the planet’s spin axis to be less than 5°. Considered as a dipole field, the moment is in the range 240 to 270 nT-R _M ³ , where R _M is Mercury’s radius. Multipole solutions for the planetary field yield a smaller dipole term, 180 to 220 nT-R _M ³ , and higher-order terms that together yield an equatorial surface field from 250 to 290 nT. From the spatial distribution of the fit residuals, the equatorial data are seen to reflect a weaker northward field and a strongly radial field, neither of which can be explained by a centered-dipole matched to the field measured near the pole by Mariner 10. This disparity is a major factor controlling the higher-order terms in the multipole solutions. The residuals are not largest close to the planet, and when considered in magnetospheric coordinates the residuals indicate the presence of a cross-tail current extending to within 0.5R _M altitude on the nightside. A near-tail current with a density of 0.1 μA/m² could account for the low field intensities recorded near the equator. In addition, the MESSENGER flybys include the first plasma observations from Mercury and demonstrate that solar wind plasma is present at low altitudes, below 500 km. Although we can be confident in the dipole-only moment estimates, the data in hand remain subject to ambiguities for distinguishing internal from external contributions. The anticipated observations from orbit at Mercury, first from MESSENGER beginning in March 2011 and later from the dual-spacecraft BepiColombo mission, will be essential to elucidate the higher-order structure in the magnetic field of Mercury that will reveal the telltale signatures of the physics responsible for its generation.     

多帧PML规整化湍流退化图像复原算法

从湍流退化图像中有效地恢复出原目标图像,是空间目标成像观测亟待解决的问题。为解决强模糊实际观测湍流退化图像的复原问题,本文提出了多帧PML规整化图像复原算法。该算法主要利用非线性规整化项在点扩散函数和目标图像的估计过程中进行平滑。为验证算法的有效性,针对强噪声退化图像进行了恢复实验,实验结果证明,该算法对于强噪声湍流退化图像的复原是非常有效的。     

Lithium Abundance in Pop.II Stars A post-HIPPARCOS discussion

The relation between the lithium abundance observed in Population II stars and the primordial abundance, is still an open question (see Cayrel and Duncan, this meeting). A few recent results are discussed. HIPPARCOS data show that the standard model of stellar evolution can explain the 6Li detection in HD 84937, suggesting a negligible depletion of 7Li. A slope in the Li/Teff relation for Pop II dwarfs and a spread of their Li abundance have been advocated, and both used as arguments in favor of Li depletion. The slope is not confirmed when two other independent temperature scales are used. The Li scatter around the plateau is hardly larger than the scatter predicted from determination errors. Hints from a scatter of Li in subgiants of the globular cluster M92 are not completely conclusive. The determination of more accurate Li abundances in the Pop II stars is an urgent but difficult task, requiring better model atmosphere (better convection treatment) and the help of observational data about Pop II stars (such as long base interferometry).