New ways to rotation rates

Progress in determining rotation rates of Algol primary stars from light curves is assessed. Included are elementary ideas on why the new method works, how to carry out solutions, and how and when to apply the constraint on rotational lobe filling. Some comments are made on desirable improvements for measuring rotation from line broadening. A few remarks are made about the problem of identifying likely fast rotating Algols.     

Determining rotation rates from light curves: RW Mon and RW Tau

We present light curve solutions for the non-synchronously rotating Algols RW Mon and RW Tau, and we illustrate how rotation rates are determined from light curves. We find RW Mon's primary component to spin at about 5 times the synchronous rate, which confirms the indication of fast rotation from reported emission line activity. RW Tau turns out to be only a mildly rapidly rotating Algol system, and our light curve solutions do not yield any firm value for the rotation rate of the primary component. It is suggested that continued efforts should be made to do good quality line broadening studies in order to find rotation rates for systems with only modest degrees of rapid rotation, and in order to further test photometric rotation rates against those of line broadening studies.     

Determining rotation rates from light curves: RW Mon and RW Tau

We present light curve solutions for the non-synchronously rotating Algols RW Mon and RW Tau, and we illustrate how rotation rates are determined from light curves. We find RW Mon's primary component to spin at about 5 times the synchronous rate, which confirms the indication of fast rotation from reported emission line activity. RW Tau turns out to be only a mildly rapidly rotating Algol system, and our light curve solutions do not yield any firm value for the rotation rate of the primary component. It is suggested that continued efforts should be made to do good quality line broadening studies in order to find rotation rates for systems with only modest degrees of rapid rotation, and in order to further test photometric rotation rates against those of line broadening studies.     

双转子涡喷发动机的转差调整

本文分析了双转子涡喷发动机转差的概念和作用,指出转差的大小将影响高低压压气机的稳定工作裕度和高压转子的转速n_2与涡轮前燃气温度T_3的匹配问题。本文提出如何正确调整转差,其结果与实际台架试车数据基本符合。此外,还提供转差对推力、单位燃油消耗率、n_2和T_3的影响关系,可供实际应用参考。     

高回转精度微柱状电极电化学加工模型及试验

为实现高回转精度微柱状电极的精确高效在线制备,对微电极电化学刻蚀过程进行了深入的研究与改进。首先,根据电化学刻蚀原理,分析了电极旋转对柱状电极加工的影响,试验证明电极旋转可以提高电极的回转精度;其次,根据试验归纳,确立了加工电压、浸液深度和电极转速之间的函数关系,建立了高回转精度微柱状电极加工控制数学模型;最后,在上述模型的指导下,选择优化的加工参数组合,成功加工得到一系列直径为100 μm左右、同轴度误差小于1 μm的柱状电极。     

关于起落架收放中转轴及转动的确定

 本文对用解析法确定起落架收放中转轴及转动的问题,进行一些探讨,除提出如何利用刚体绕斜轴的转动矩阵进行求解外,还对转轴和转角的某些求法进行补充。文中附有一飞机起落架收放算例。本文内容也可用于航空、航天器中一些天线、传感器等的收放设计。     

旋转方截面U型通道分离流二阶相关分量测量

为了深入了解旋转涡轮叶片内冷通道中的紊流特性，并为CFD研究提供实验数据，用激光多普勒测速仪（LDA）测量了旋转U型通道中分离流的雷诺应力分量。通道的转轴与弯道的曲率轴平行，测量是在与转轴垂直的对称平面中进行的，流动状态为Re=100,000,Ro=0,0.2和－0．2。直接测量的分量为ux^2^-,Ux^2^-和uxux^-，结果表明旋转对紊流分布的形式有很强的影响。在测量的三种旋转状态中Ro=0.2的正转和Ro=0.2的负转分别具有最低和最高的紊流强度。根据测量到的信息估算了雷诺应力uiuj^-的产生率，结果显示负转的产生率比正转时高。     

The Solar Dynamo

It is generally accepted that the strong toroidal magnetic fields that emerge through the solar surface in sunspots and active regions are formed by the action of differential rotation on a poloidal field, and then stored in or near the tachocline at the base of the Sun’s convection zone. The problem is how to explain the generation of a reversed poloidal field from this toroidal flux—a process that can be parametrised in terms of an α-effect related to some form of turbulent helicity. Here we first outline the principal patterns that have to be explained: the 11-year activity cycle, the 22-year magnetic cycle and the longer term modulation of cyclic activity, associated with grand maxima and minima. Then we summarise what has been learnt from helioseismology about the Sun’s internal structure and rotation that may be relevant to our subject. The ingredients of mean-field dynamo models are differential rotation, meridional circulation, turbulent diffusion, flux pumping and the α-effect: in various combinations they can reproduce the principal features that are observed. To proceed further, it is necessary to rely on large-scale computation and we summarise the current state of play.     

旋转光滑及带肋U形通道的局部换热特性

用实验方法研究了旋转状态下光滑及带肋U形方截面通道的换热特性。带肋通道中,90°直肋对称布置在前后缘,肋片高径比为0.143,节距比为7。在实验雷诺数及旋转数范围分别为6100~25100和0~0.26下,对比分析了光滑及带肋通道的旋转换热特性。结果表明,带肋通道的换热明显好于光滑通道;旋转强化了第1通道后缘及第2通道前缘的换热,但削弱了第1通道前缘及第2通道后缘的换热;旋转效应对带肋结构的第1通道前后缘换热的影响最为明显;光滑通道中,弯道效应对其下游换热的影响较为显著。     

The Magnetic Field of the Milky Way from Faraday Rotation of Pulsars and Extragalactic Sources

Faraday rotation towards polarised pulsars and extragalactic sources is the best observable for determining the configuration of the magnetic field of the Galaxy in its plane and also at high latitudes. The Galactic magnetic field plays an important role in numerous astrophysical processes, including star formation and propagation of ultrahigh-energy cosmic rays; it is also an important component in measurements of the cosmological microwave background. This review article provides a brief overview of the latest advancements in the field, from an observer’s point of view. The most recent results based on pulsar rotation measures are discussed, which show that we have begun to confidently resolve the main features of the Galactic magnetic field on kiloparsec scales, both in the Solar neighbourhood and at larger distances. As we are currently in great anticipation of polarisation observations with new, state-of-the-art telescopes and hardware, a brief overview of how much this field of research will benefit from the upcoming pulsar surveys is also given.     

The relation of Algols and W Serpentis stars

Evidence on the issues of whether the W Serpentis stars are a coherent class, and how they may interface with the Algol systems, is reviewed, with emphasis on the idea that they are semi-detached systems in the latter part of the rapid phase of mass transfer, with optically and geometrically thick disks of transferred gas around the (now) more massive star. We are interested in what will be seen when the gas clears away, and mainly examine the idea that it will be an Algol-type system. More particularly, consideration is given to centrifugally limited accretion as a mechanism to build up a substantial disk, and the presumed evolutionary sequence is from a W Ser to a rapidly rotating Algol to a normal Algol system. Systems such as V367 Cyg and RW Tau fit into this scheme only with difficulty. Because it is extremely difficult to measure the rotation of some W Ser (mass) primaries, it is natural to look at the rotation statistics of Algols to test this idea. The badly behaved light curves and spectroscopy of some Algols (eg. U Cep, RZ Sct) may be attributable to the double contact condition, and the ramifications of this possibility are discussed. If so, the rotation statistics of Algols should show two spikes, corresponding to the two special conditions into which a system should be driven by tidal braking and centrifugally limited spinup. Present rotation statistics do show these spikes. Algols should flip between these states fairly quickly, depending on the mass transfer rate. Thus, to the extent that the meager statistics can be accepted as meaningful, the new (fourth) morphological type of close binary (double contact) has attained demonstrable reality. The rotation statistics are presented in terms of a particular rotation parameter, R, which is zero for synchronism and unity for the centrifugal limit. Future work should develop rotation statistics to see if the rotational lobe-filling (R = 1) spike persists. It should also look into whether W Ser primaries are on the hydrogen burning main sequence, or in general what they are. We also need more light curves of W Ser type systems, high resolution line profiles for the (mass) primaries (with particular attention to the W Ser-Algol transition cases), and spectroscopy of low inclination W Serpentis systems, such as KX And.     

The relation of Algols and W Serpentis stars

Evidence on the issues of whether the W Serpentis stars are a coherent class, and how they may interface with the Algol systems, is reviewed, with emphasis on the idea that they are semi-detached systems in the latter part of the rapid phase of mass transfer, with optically and geometrically thick disks of transferred gas around the (now) more massive star. We are interested in what will be seen when the gas clears away, and mainly examine the idea that it will be an Algol-type system. More particularly, consideration is given to centrifugally limited accretion as a mechanism to build up a substantial disk, and the presumed evolutionary sequence is from a W Ser to a rapidly rotating Algol to a normal Algol system. Systems such as V367 Cyg and RW Tau fit into this scheme only with difficulty. Because it is extremely difficult to measure the rotation of some W Ser (mass) primaries, it is natural to look at the rotation statistics of Algols to test this idea. The badly behaved light curves and spectroscopy of some Algols (eg. U Cep, RZ Sct) may be attributable to the double contact condition, and the ramifications of this possibility are discussed. If so, the rotation statistics of Algols should show two spikes, corresponding to the two special conditions into which a system should be driven by tidal braking and centrifugally limited spinup. Present rotation statistics do show these spikes. Algols should flip between these states fairly quickly, depending on the mass transfer rate. Thus, to the extent that the meager statistics can be accepted as meaningful, the new (fourth) morphological type of close binary (double contact) has attained demonstrable reality. The rotation statistics are presented in terms of a particular rotation parameter, R, which is zero for synchronism and unity for the centrifugal limit. Future work should develop rotation statistics to see if the rotational lobe-filling (R = 1) spike persists. It should also look into whether W Ser primaries are on the hydrogen burning main sequence, or in general what they are. We also need more light curves of W Ser type systems, high resolution line profiles for the (mass) primaries (with particular attention to the W Ser-Algol transition cases), and spectroscopy of low inclination W Serpentis systems, such as KX And.     

A Test of the Effect of Satellite Spin on Two-Way Doppler Range-Rate Measurements

Analysis indicates that the rotation of a satellite can cause an error in the range-rate measurements of a two-way Doppler tracking system. The error is proportional to the rotation rate, and the constant of proportionality depends on the polarization of the satellite transponder antennas. Measurements made by ground-based simulation confirmed the analytical prediction.     

Large Scale Flows in the Solar Convection Zone

We discuss the current theoretical understanding of the large scale flows observed in the solar convection zone, namely the differential rotation and meridional circulation. Based on multi-D numerical simulations we describe which physical processes are at the origin of these large scale flows, how they are maintained and what sets their unique profiles. We also discuss how dynamo generated magnetic field may influence such a delicate dynamical balance and lead to a temporal modulation of the amplitude and profiles of the solar large scale flows.     

用最佳旋转轴方法形成误差信号的飞行器姿态控制系统

本文重点讨论采用所谓最佳旋转轴方法来形成飞行器纵轴指向控制的误差信号,对于绕飞行器纵轴本身转动的控制主要讨论了滚动稳定和倾斜稳定两种情况下误差信号的形成。详细推导了它们的计算公式。作为这个方法应用的例子,我们还讨论了如果飞行器上安装一个三轴平台或一组捷联式速率陀螺时,怎样由它们敏感的信号形成姿态控制误差信号,并给出了相应的姿态控制系统原理结构图。     

基于傅里叶变换的航迹对准关联算法

研究了在组网雷达存在系统误差情况下的目标航迹关联问题,理论分析了雷达系统误差对目标航迹的影响,并将该影响表示为目标航迹的旋转和平移量。在此基础上,提出了一种基于傅里叶变换的系统误差配准前航迹对准关联算法,该算法将组网雷达的航迹数据看做为一种整体信息,采用傅里叶变换理论来估计和补偿组网雷达目标航迹数据到融合中心航迹数据的相对旋转量和平移量,将雷达网中雷达上报的目标航迹数据对准到融合中心,从而不依赖于估计雷达网系统误差,实现了误差配准前的航迹准确关联,能够为后端的系统误差配准提供可靠的关联目标航迹数据。     

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。     

Voyager 2 Solar Wind Observations in the Outer Heliosphere

We discuss the solar wind parameters measured in the distant heliosphere from the Voyager 2 spacecraft. Periodic variations in the speed of the wind observed at roughly the solar rotation period may correspond to interaction regions between slower and faster streams of wind. Since the interplanetary magnetic field is enhanced in such regions, they are important for the study of modulation of cosmic rays. Unfortunately, direct observation of the enhanced magnetic field from Voyager 2 has been made difficult by spacecraft-associated noise since 1989.     

Solar flux and its variations

We present data on the solar irradiance as derived from a number of sources. An attempt was made to bring these data onto a uniform scale. The results are presented in Table IV and Figure 6. Summation of fluxes at all wavelengths yields a figure of 1357.826 W m^-2 for the solar constant. Estimates are made of the solar flux variations due to flares, active regions (slowly varying component), solar rotation and the 11-year cycle.Solar activity does not produce a significant variation in the value of the solar constant. Nevertheless, variations in the X-ray and extreme ultraviolet portions of the solar flux may be several orders of magnitude during solar activity, especially at times of major flares. It is well established that these short wavelength flux enhancements cause significant changes in the terrestrial ionosphere.     

楔形扰流柱通道流动与传热特性

针对处在高速旋转(哥氏力、离心力以及诱导产生的浮升力)状态下的涡轮转子叶片尾缘独特的几何结构(带扰流柱的楔形通道)和特殊的流动方式(径向进气侧向出流),采用实验的方法在实际工况参数范围内对其传热和流阻特性进行了详细研究:雷诺数和旋转数的变化范围为20 000~45 000、0~0155。实验结果表明:扰流柱的存在使得径向区域底部的滞止区域变大,但这也让中部传热有明显的提升;流阻和综合传热系数的比光滑参数随着雷诺数的增加而下降;旋转对顶部传热有增强作用,底部传热减弱;总地来说旋转使得通道的平均传热减弱,流阻增加,综合传热系数下降。