量子惯性仪表用磁屏蔽材料进展

量子惯性仪表是利用光场和磁场等手段操控原子、电子等微观粒子实现载体运动信息测量的新型惯性设备,量子惯性仪表对外界磁场的大小、稳定性和均匀性等提出了很高的要求,需要高性能的磁屏蔽技术与之相匹配。回顾了目前常用的磁屏蔽方式,针对最常用的被动型磁屏蔽所涉及的材料铁镍合金、非晶合金和软磁铁氧体等进行了梳理和总结,阐述了上述三种材料的优缺点以及适用范围,并展望了量子惯性仪表用磁屏蔽材料的发展趋势。     

基于热磁耦合分析的高性能磁屏蔽系统设计

近零磁工作环境是实现无自旋交换弛豫(SERF)原子自旋惯性测量装置的必要条件,但在实际中由于装置内部气室加热和环境温度变化引起的磁屏蔽性能变化是影响系统性能的一个主要因素.基于热-磁耦合理论建立了惯性测量装置的有限元分析模型,对加热条件下磁屏蔽筒内磁场均匀性及其剩余磁场进行了分析.结果表明,气室加热至200℃时,附近温...     

核磁共振陀螺用高均匀磁场线圈设计方法

核磁共振陀螺代表了新一代高精度、微小型陀螺的发展方向之一,随着陀螺体积的降低,磁屏蔽层与磁场线圈随之减小,且二者贴合更加紧密,高导磁性的磁屏蔽层及低导磁性的空气介质交错分布,改变了线圈的磁通路径,导致线圈的磁场均匀性下降,制约了陀螺精度的提高。针对这一问题,提出了磁场等效增益系数,模拟磁屏蔽边界对线圈磁场的影响,据此建立了磁屏蔽边界条件下高均匀磁场线圈模型,优化了线圈参数。对所设计线圈的磁场均匀性进行了测试,表明该设计方法可以得到磁屏蔽边界条件下高均匀磁场线圈,可为发展微小型、高精度的核磁共振陀螺高均匀磁场线圈设计方法提供参考。     

超磁致伸缩材料作动器的研制及特性分析

 采用自制的TbDyFe超磁致伸缩材料设计并制作了主动振动控制用超磁致伸缩作动器 ,并对其偏置磁场、激励磁场、静态特性、动态特性和主动控制减振效果进行了测试和分析。研究结果表明 ,作动器工作应变在TbDyFe材料的线性区 ,其总伸缩量可达 70 μm。低频动态特性好 ,谐频影响小。在自适应滤波控制方式下使用该作动器对正弦振动进行主动控制减振 ,减振效果达到 30dB。磁场均匀性对作动器输出特性有明显影响 ,采用Ansys有限元软件精确设计作动器激励磁场 ,可提高超磁致伸缩材料沿轴向磁场均匀性。     

基片摆动对磁控溅射膜厚均匀性的影响研究

研究了基片摆动和基片自转的磁控溅射系统中基片摆动角振幅和基片自转角速度对磁控溅射膜厚均匀性的影响。在理论分析的基础上,进行了铜膜溅射实验,实验结果和理论分析符合,在摆动角振幅为π/3弧度,自转角速度为π弧度/秒的条件下,于4英寸硅基片上得到了±5.6%的膜厚均匀性。     

关于粒子图像测速仪精度的数值测试

利用数值模拟的方法对粒子图像测速仪的精度问题进行了数值实验。速度场是通过对一个片光源上两次曝光的图像进行互相关处理来得到的。为了研究流体运动的不均匀性对于一个诊断区内速度矢量测量结果的影响，针对五种典型的不均匀性进行讨论。数值实验的结果表明有几种流体运动不均匀性会显著地影响这种粒子图像测速方法的精度。     

AlNiCo合金中α1相取向程度对磁稳定性的影响

AlNiCo合金具有优异的温度稳定性和磁稳定性，在惯性仪表中广泛应用，其磁稳定性对于仪表的精度和寿命具有重要影响。AlNiCo合金中主要包括强磁性的α1相和弱磁性的α2相，通常情况下取向一致的α1相为磁体提供矫顽力和磁化强度。通过磁场热处理的方法控制α1相的取向，研究其对磁稳定性的影响规律，探索提高AlNiCo合金磁稳定性的新思路。研究发现，随机取向的AlNiCo-0样品虽然矫顽力和剩磁较低，但是具备更低的磁粘滞系数，稳定性优于各向异性的AlNiCo-0.25样品，这主要是由于其能垒分布更加平缓。微磁模拟的结果进一步表明，取向垂直于易轴的α1相更有助于形成稳定的磁畴结构。     

捷联航姿传感器的误差补偿标定方法

磁航向传感器作为机载设备,它的工作情况与载体环境的影响有着密切的关系,测得的磁航向角存在着较大的误差,不能直接用来进行导航定位。所以,必须对其进行误差补偿,提高磁航向角的测量精度,才能用于导航定位。罗差是磁阻罗盘的主要误差源,文中介绍了罗差方程式,并重点推导了基于最小二乘法的七参数八位置误差标定方法。基于该方法的磁航向补偿算法的性能试验结果证明,磁航向误差基本维持在0.5°左右,满足了精度的要求。     

滚珠自转对高速球轴承环下润滑内部流动的影响

高速球轴承正常工作时,处于高速旋转状态,此时油相和气相因重力和离心力的作用在轴承环间剧烈运动。为了更准确地分析轴承环间的两相流动,采取VOF模型进行内部流场的模拟,采用多重旋转坐标系描述部件运动。建立球轴承环下润滑计算模型,分析了考虑滚珠自转因素下轴承内部的流动,并在此基础上探究了转速及供油量对轴承工作状态的影响。结果表明,对比整体模型与滚珠自转模型,发现滚珠自转使得轴承内部油体积分数增大,同时也使得滑油穿透间隙达到外环的能力增加;在考虑滚珠自转情况下,转速的不断增大,使得轴承内部的油相体积分数不断减小,在低转速情况下滚珠自转对流体运动影响较为明显,在高转速情况下公转速度对流体运动起到主导作用,滚珠自转对流体运动影响减弱;供油量不断的增大,使得滚珠自转模型内部的油相体积分数也在不断增大,而且滚珠自转运动会加强滑油在轴承内部的分布。     

基于三轴磁传感器运动噪声消除方法的系数搜索

基于三轴磁传感器运动噪声消除方法的系数搜索,是实现三轴磁信号标量接收技术的前提.根据三轴磁传感器运动噪声消除方法的数学模型,提出适合单片机编程的梯度法结合自适应的系数搜索方法,并给出仿真结果.仿真结果表明,该方法噪声消除效果良好.     

旋转惯导中加速度计尺寸效应误差分析及补偿

 对旋转调制惯导转位过程中系统精度受加速度计尺寸效应影响的问题进行了研究。通过分析尺寸效应引起惯导系统(INS)导航误差的机理,推导了尺寸效应作用下加速度测量误差与速度误差的解析表达式。根据理论分析结果,分别给出了以速度误差和加速度误差作为观测量进行尺寸参数辨识的方法,并进行了必要讨论。结合旋转惯导转位过程中的速度误差特征,选取加速度测量误差为观测量对尺寸参数进行试验标定,尺寸参数辨识精度优于1.29 mm(1σ)。在此基础上给出了尺寸效应误差补偿方法,并在不同初始方位下对补偿效果进行试验验证,结果表明,通过尺寸效应补偿可以有效提高旋转惯导转位过程中的速度精度。     

经济型微机电台阶测量仪的研究

针对微机电系统(MEMS)中微小器件的表面刻蚀沟槽及台阶的测量,研制采用步进电机运动平台和微力电感测头,用变截面片簧作回转运动的测头支撑机构,对运动平台存在的偏心作用力和振动噪声问题做了分析和研究,提出了有效的解决方案。     

Geophysical Constraints on the Evolution of Mars

The evolution of Mars is discussed using results from the recent Mars Global Surveyor (MGS) and Mars Pathfinder missions together with results from mantle convection and thermal history models and the chemistry of Martian meteorites. The new MGS topography and gravity data and the data on the rotation of Mars from Mars Pathfinder constrain models of the present interior structure and allow estimates of present crust thickness and thickness variations. The data also allow estimates of lithosphere thickness variation and heat flow assuming that the base of the lithosphere is an isotherm. Although the interpretation is not unambiguous, it can be concluded that Mars has a substantial crust. It may be about 50 km thick on average with thickness variations of another ±50 km. Alternatively, the crust may be substantially thicker with smaller thickness variations. The former estimate of crust thickness can be shown to be in agreement with estimates of volcanic production rates from geologic mapping using data from the camera on MGS and previous missions. According to these estimates most of the crust was produced in the Noachian, roughly the first Gyr of evolution. A substantial part of the lava generated during this time apparently poured onto the surface to produce the Tharsis bulge, the largest tectonic unit in the solar system and the major volcanic center of Mars. Models of crust growth that couple crust growth to mantle convection and thermal evolution are consistent with an early 1 Gyr long phase of vigorous volcanic activity. The simplest explanation for the remnant magnetization of crustal units of mostly the southern hemisphere calls for an active dynamo in the Noachian, again consistent with thermal history calculations that predict the core to become stably stratified after some hundred Myr of convective cooling and dynamo action. The isotope record of the Martian meteorites suggest that the core formed early and rapidly within a few tens of Myr. These data also suggest that the silicate rock component of the planet was partially molten during that time. The isotope data suggest that heterogeneity resulted from core formation and early differentiation and persisted to the recent past. This is often taken as evidence against vigorous mantle convection and early plate tectonics on Mars although the latter assumption can most easily explain the early magnetic field. The physics of mantle convection suggests that there may be a few hundred km thick stagnant, near surface layer in the mantle that would have formed rapidly and may have provided the reservoirs required to explain the isotope data. The relation between the planform of mantle convection and the tectonic features on the surface is difficult to entangle. Models call for long wavelength forms of flow and possibly a few strong plumes in the very early evolution. These plumes may have dissolved with time as the core cooled and may have died off by the end of the Noachian.     

Thermal Evolution and Magnetic Field Generation in Terrestrial Planets and Satellites

Of the terrestrial planets, Earth and Mercury have self-sustained fields while Mars and Venus do not. Magnetic field data recorded at Ganymede have been interpreted as evidence of a self-generated magnetic field. The other icy Galilean satellites have magnetic fields induced in their subsurface oceans while Io and the Saturnian satellite Titan apparently are lacking magnetic fields of internal origin altogether. Parts of the lunar crust are remanently magnetized as are parts of the crust of Mars. While it is widely accepted that the magnetization of the Martian crust has been caused by an early magnetic field, for the Moon alternative explanations link the magnetization to plasma generated by large impacts. The necessary conditions for a dynamo in the terrestrial planets and satellites are the existence of an iron-rich core that is undergoing intense fluid motion. It is widely accepted that the fluid motion is caused by convection driven either by thermal buoyancy or by chemical buoyancy or by both. The chemical buoyancy is released upon the growth of an inner core. The latter requires a light alloying element in the core that is enriched in the outer core as the solid inner core grows. In most models, the light alloying element is assumed to be sulfur, but other elements such as, e.g., oxygen, silicon, and hydrogen are possible. The existence of cores in the terrestrial planets is either proven beyond reasonable doubt (Earth, Mars, and Mercury) or the case for a core is compelling as for Venus and the Moon. The Galilean satellites Io and Ganymede are likely to have cores judging from Galileo radio tracking data of the gravity fields of these satellites. The case is less clear cut for Europa. Callisto is widely taken as undifferentiated or only partially differentiated, thereby lacking an iron-rich core. Whether or not Titan has a core is not known at the present time. The terrestrial planets that do have magnetic fields either have a well-established inner core with known radius and density such as Earth or are widely agreed to have an inner core such as Mercury. The absence of an inner core in Venus, Mars, and the Moon (terrestrial bodies that lack fields) is not as well established although considered likely. The composition of the Martian core may be close to the Fe–FeS eutectic which would prevent an inner core to grow as long as the core has not cooled to temperatures around 1500 Kelvin. Venus may be on the verge of growing an inner core in which case a chemical dynamo may begin to operate in the geologically near future. The remanent magnetization of the Martian and the lunar crust is evidence for a dynamo in Mars’ and possibly the Moon’s early evolution and suggests that powerful thermally driven dynamos are possible. Both the thermally and the chemically driven dynamo require that the core is cooled at a sufficient rate by the mantle. For the thermally driven dynamo, the heat flow from the core into the mantle must by larger than the heat conducted along the core adiabat to allow a convecting core. This threshold is a few mW?m^?2 for small planets such as Mercury, Ganymede, and the Moon but can be as large as a few tens mW?m^?2 for Earth and Venus. The buoyancy for both dynamos must be sufficiently strong to overcome Ohmic dissipation. On Earth, plate tectonics and mantle convection cool the core efficiently. Stagnant lid convection on Mars and Venus are less efficient to cool the core but it is possible and has been suggested that Mars had plate tectonics in its early evolution and that Venus has experienced episodic resurfacing and mantle turnover. Both may have had profound implications for the evolution of the cores of these planets. It is even possible that inner cores started to grow in Mars and Venus but that the growth was frustrated as the mantles heated following the cessation of plate tectonics and resurfacing. The generation of Ganymede’s magnetic field is widely debated. Models range from magneto-hydrodynamic convection in which case the field will not be self-sustained to chemical and thermally-driven dynamos. The wide range of possible compositions for Ganymede’s core allows models with a completely liquid near eutectic Fe–FeS composition as well as models with Fe inner cores or cores in with iron snowfall.     

Gravity Sensors and the Principle of Equivalence

The tensor characteristics of the inertial fields created by acceleration and rotation, and the gravitational fields created by masses are discussed. Although it is sometimes thought that it is impossible to distinguish between gravitational and inertial effects because of Einstein's principle of equivalence, these effects do have different, detectable tensor characteristics. The principle of equivalence is only strictly applicable at a point, while the instruments to measure these tensor fields exist over a finite region. The inertial field created by acceleration is a uniform vector field and has no gradients, while the inertial field created by rotation has a uniform cylindrically symmetric tensor gradient but none of higher order. The gravitational field created by a mass is highly nonuniform with essentially no limit to the number of higher order gradients. These differences make it theoretically possible to independently measure gravitation, rotation, and acceleration effects; to do so, some form of differential force sensor with tensor response characteristics must be used. The standard technique is static, using differential accelerometers to sense the spatial gradient characteristics of the fields. A more promising technique is dynamic; by rotation of the differential sensor, the static spatial variations are transformed into temporal variations with various frequency components. It is then possible to distinguish between the various fields by frequency filtering.     

轴流压气机机匣变形对多排转子流场特性的影响

在实际轴流压气机加工、装配、使用过程中,机匣的圆度控制、叶片的高度控制、转子和机匣之间的同轴度控制等都普遍存在误差,意味着叶尖间隙的不均匀性必然地存在于每台压气机中。随着对轴流压气机流动研究的不断深入,叶尖周向非均匀间隙成为了需要考虑的问题。针对由机匣变形造成的非均匀叶尖间隙,研究了其对多排转子流场特性的影响。首先介绍了表征机匣变形程度的新参数,进而引进了非轴对称压气机模型的建模方法。针对3种不同的间隙周向布局,采用定常和非定常方法进行了数值模拟,对比了均匀与非均匀间隙下多排转子的气动性能,分析了机匣变形对气动损失分布和传播的影响,并研究了非均匀间隙下非定常压力和气动力的脉动特征。结果表明：非均匀间隙会降低转子性能,转子叶排叶尖区域的流场在非均匀间隙下呈现明显的周向非对称性,在上游叶排“尾迹”的干扰下,后排转子叶尖流场的周向非对称性要大于前排转子。非均匀间隙布局与各叶片气动力分布呈现明显的对应关系,小间隙区域叶片的气动力高,大间隙区域叶片气动力相对较低,从而增加了非均匀间隙下转子叶片的气动力幅值。     

阻旋栅对密封静力与动力特性影响的数值分析与实验研究

密封动力特性对旋转机械转子系统稳定性影响较大,在密封入口端部设置阻旋栅是提高密封稳定性的有效方法。设计加工了无/有阻旋栅共5种密封结构,从数值分析与实验研究两个方面研究阻旋栅对密封静力与动力特性的影响规律。建立阻旋栅密封静力特性CFD理论模型,数值分析阻旋栅对密封泄漏量、切向速度以及周向压力分布的影响;应用不平衡同频激励法实验研究阻旋栅对密封动力特性的影响。研究结果表明:阻旋栅可降低密封的泄漏量,减小密封内流体的切向速度,进而降低密封内流体的周向压力差,且随着阻旋栅周向稠度与径向长度的增加,这种作用逐渐增大,这是阻旋栅抑制气流激振力的主要原因;预旋是密封产生交叉刚度的重要因素,密封的交叉刚度随进出口压比与转速的增加而增大;阻旋栅可有效降低密封的交叉刚度,增加密封的主阻尼,提高密封的稳定性。本文研究揭示了阻旋栅抑制密封气流激振力的机理,为设计阻旋栅密封提供理论依据。     

Dynamo Scaling Laws and Applications to the Planets

Scaling laws for planetary dynamos relate the characteristic magnetic field strength, characteristic flow velocity and other properties to primary quantities such as core size, rotation rate, electrical conductivity and heat flux. Many different scaling laws have been proposed, often relying on the assumption of a balance of Coriolis force and Lorentz force in the dynamo. Their theoretical foundation is reviewed. The advent of direct numerical simulations of planetary dynamos and the ability to perform them for a sufficiently wide range of control parameters allows to test the scaling laws. The results support a magnetic field scaling that is not based on a force balance, but on the energy flux available to balance ohmic dissipation. In its simplest form, it predicts a field strength that is independent of rotation rate and electrical conductivity and proportional to the cubic root of the available energy flux. However, rotation rate controls whether the magnetic field is dipolar or multipolar. Scaling laws for velocity, heat transfer and ohmic dissipation are also discussed. The predictions of the energy-based scaling law agree well with the observed field strength of Earth and Jupiter, but for other planets they are more difficult to test or special pleading is required to explain their field strength. The scaling law also explains the very high field strength of rapidly rotating low-mass stars, which supports its rather general validity.     

旋转状态边界层速度场及温度场特性实验

针对涡轮转子叶片内冷技术,使用TR-PIV(time resolved particle image velocimetry)技术与热线技术同步原位测量了壁面加热条件下旋转通道内边界层速度场和温度场特性。结果显示:旋转数大于0.48时前缘面附近出现了回流现象,并从受力分析的角度给出了解释;回流区一般出现于流场下游、较大密度比、较高旋转数下,可以利用回流区的影响达到增强前缘面换热的目的;得到了旋转条件下无量纲温度型、温度脉动量和努塞尔数的变化规律,可以看出湍流边界层内部的温度场分布在旋转效应的影响下产生了强烈的不对称性,与静止条件下的标准规律相比会产生一定的偏差。     

计及诱速和风切变的直升机自转前飞特性

研究直升机自转前飞时在风切变条件下的稳定性和操纵性。风切变采用非线性模型，旋翼模型考虑桨叶的刚性挥舞运动，桨叶根部具有水平铰外伸量和弹性约束，诱速在桨盘处的分布采用固定涡系所表示的诱速非均匀分布模型，以Ｚ９飞机为算例，算出计及风切变与否的自转前飞平衡参数和稳定根及操纵响应，显示了风切变对自转前飞操稳特性的影响。