环状针刺C/C复合材料的压缩性能及破坏机理

以碳纤维针刺毡为预制体,采用CVI致密工艺制作准三维C/C薄壁回转体,具有各向异性的力学性能.本文主要对三个主方向的材料压缩性能及破坏机理进行了研究讨论.结果表明:轴向压缩与环向压缩性能相似具有较高的压缩模量.材料的径向压缩表现为假塑性断裂行为,在材料的断裂面上具有大量纤维及基体碎屑,材料发生剪切破坏及基体压溃破坏.材料的轴向压缩与环向压缩表现为脆性断裂行为,材料主要以分层劈裂方式破坏.     

LD10网格加强肋结构壁板的化学铣切工艺研究

为了寻找到化铣槽液各组分的最佳含量范围,使零件达到稳定化铣侧切率,减少板材铣切厚度差,本研究通过测量对比试片在各组分含量的槽液中铣切壁板的侧切率和均匀度参数来实现.结果表明,当NaOH初始浓度为200 g/L、溶解Al3+为70～110 g/L、温度(90±5)℃的技术条件下能够得到肋条偏差Tw±0.75 mm、壁厚偏差Ts±0.15 mm的较理想的化铣产品.     

PIP 工艺对2D C/ SiC-ZrB2 复合材料结构和力学性能的影响

采用CVI结合SI及PIP工艺制备2D C/SiC-ZrB2复合材料.研究了PIP工艺中循环浸渍次数及热处理对复合材料结构和力学性能的影响.比较了多孔C/SiC浸渍浆料后用PIP结合CVI致密化和仅用CVI致密化的效果.结果表明:浸渍裂解后,热处理温度相同,热处理次数对复合材料的开孔率和弯曲强度影响不大.2D C/SiC-ZrB2复合材料的弯曲强度不随PIP次数的增多而增加,PIP处理二次后,复合材料的强度逐渐增加,PIP处理五次,强度达到最大值,制备的复合材料开孔率为8.0%、弯曲强度为423 MPa.SI后用PIP结合CVI致密化比仅用CVI致密化效果好.     

热氧、湿热和热水老化对T300/ BHEP 复合材料玻璃化转变温度的影响

通过对碳纤维/环氧复合材料(T300/BHEP)进行热氧、湿热和热水老化研究,得到了材料的质量变化率和Tg随老化条件的演变规律,分析了老化机理.结果表明:T300/BHEP复合材料在热氧老化条件下,因后固化和自由体积收缩,Tg升高;在湿热和热水老化条件下,因水分塑化作用和水对分子链间氢键的破坏,Tg降低.三种老化条件下,Tg与质量变化率均呈线性关系.对比80℃热氧、80℃/RH75%湿热和80℃热水老化条件下的结果,发现水分的塑化作用对Tg的影响要大于因热的作用产生的后固化,且湿度越大,Tg降低越明显.     

圆锥脉冲等离子体诱导流场特性分析

对等离子体诱导流场特性进行研究,有利于解决双稳态非对称分离涡带来的连续比例控制困难的问题。在封闭光学玻璃箱体内,应用介质阻挡放电等离子体对20°顶角圆锥附近静止大气进行了定常和脉冲循环控制,对等离子体诱导的圆锥截面绕流速度场进行了二维PIV测量,对定常控制和脉冲循环控制下最大绕流速度及最大轴向涡量进行了比较分析。实验结果表明：相对于定常控制模式,脉冲循环控制下沿垂直于圆锥截面对称面径线分布的时间平均切向速度和轴向涡量范围较广;在脉冲循环控制下,动量传递的主要表现在离散涡的形成而不是气流的加速。     

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。     

超机动飞机飞行控制及大迎角飞行品质研究

超机动飞机飞行控制和大迎角飞行品质研究,对于强调超机动能力的第四代战斗机的飞行控制律设计、验证和试飞评定有着重要意义。以鸭式布局飞机为研究对象,应用推力矢量技术,结合奇异摄动原理和逆系统理论,设计了基于非线性动态逆理论的超机动飞行控制律。从过失速状态飞机空气动力的非线性和非定常迟滞效应、大气紊流等方面初步验证了控制律的...     

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.