高温气冷堆核电站主氦风机驱动电机绝缘系统评定技术研究

设计了一套在0.1 MPa氦气和空气环境下测试绝缘系统电气绝缘性能的试验装置,完成了0.1 MPa气压下氦气和空气中主氦风机驱动电机绝缘系统模型的局部放电起始电压(PDIV)、起晕电压、匝间冲击、绝缘电阻和工频击穿电压对比试验。试验结果表明:在0.1 MPa气压下,绝缘系统在氦气环境下的部分绝缘性能较空气中大幅下降,氦气环境下绝缘系统的PDIV值约为空气中的50%,起晕电压值约为空气中的20%~25%, 闪络(击穿)电压约为空气中的50%。     

脉冲电晕放电对减少内燃机有害排放的研究

本文对脉冲电晕放电对减少内燃机有害排放的可行性进行了研究，实验中用NDIR(非分散红外线)气体分析仪测量了SY492Q-1型汽油机在等离子装置工作或不工作时排气中CO、CO2和HC的浓度，并通过等离子发生装置结构的变化调整阴极与阳极间的放电间隙，观察并测量其对实验结果的影响。初步实验结果证明，利用等离子体技术减少汽车尾气中的HC和CO的排放是可行的，并且等离子发生装置的放电电压和放电间隙对实验结果有重要影响。     

拉伸对变频电机用漆包线耐电晕性能的影响

为了分析耐电晕漆包线在电机实际使用过程中的耐电晕性能,通过拉力试验机模拟耐电晕漆包线使用过程中的拉伸情况。首先通过拉力试验机对耐电晕漆包线进行拉伸,拉伸率分别为10%、15%。然后分别进行未拉伸漆包线、拉伸率10%及15%的耐电晕漆包线的击穿电压试验和耐电晕性能试验,并进行漆包线拉伸前后击穿电压和耐电晕寿命的比较。结果表明:拉伸率为10%、15%后漆包线击穿电压与未拉伸试样相比略有下降,拉伸15%后漆包线的击穿电压保留率超过85%。拉伸率为10%、15%的漆包线耐电晕性能与未拉伸试样比较有较明显的下降,拉伸率为15%的漆包线的耐电晕性能略差于拉伸率10%的漆包线,耐电晕漆包线拉伸率为10%时,其耐电晕性能保留率不足20%。     

Partial Discharge Testing under Direct Voltage Conditions

DC partial discharge (PD) (corona) testing is performed using a multichannel analyzer for pulse storing, and data is collected during increase of voltage and at quiescent voltage levels. Thus high voltage ceramic disk capacitors were evaluated by obtaining PD data interspersed during an accelarated life test. Increased PD activity was found early in samples that later failed catastrophically. By this technique, trends of insulation behavior are revealed sensitively and nondestructively in high voltage dc components.     

电机绝缘系统在高频冲击下局部放电试验研究

高频冲击局部放电(PD)测试可以有效的检测电机绝缘系统的绝缘状态。根据传感器的不同,电机绝缘系统在高频冲击下PD测试方法主要有两种:高频电流传感器法和超高频天线法。试验表明:在高频冲击电压下,PD主要发生在冲击的上升沿和下降沿,在同一放电电压下,上升沿和下降沿的PD幅值较大;在风力发电机定子绝缘系统鉴别试验中,随着老化试验的进行,线圈的PD起始电压总体呈下降趋势。通过鉴别试验,可以确定绝缘系统的冲击电压绝缘等级及类型。     

高空低气压下电晕放电电磁脉冲辐射特性模拟实验

为研究高空低气压下飞行器表面电晕放电电磁脉冲辐射特性,以尖端导体电晕放电为研究对象,进行了低气压下电晕放电电磁脉冲辐射特性模拟实验,给出了辐射电场幅值与气压的关系表达式,并基于气体放电和电磁场理论总结了电晕放电电磁脉冲辐射特性随电压极性、气压以及测试距离的变化规律。结果表明:电晕放电电磁脉冲辐射电场时域波形呈衰减振荡形式,持续时间约为600 ns,首脉冲方向随电压极性的不同而不同,且辐射电场分量主要集中在与放电针相同的极化方向;辐射电场频谱主要分布在500 MHz以内,在35 MHz和170 MHz处出现稳定的波峰;在气压为4~30 kPa范围内,随着气压的降低,放电电磁脉冲辐射电场增强;随着测试距离的增加,电晕放电电磁脉冲辐射电场逐渐衰减。该研究结论可为低气压下飞行器电晕放电电磁脉冲辐射特性研究提供有益参考。     

电飘机升力机制和效率的研究

实验测量了电飘机在不同电压和电极几何参数情况下的升力值.采用离子风现象解释了电飘机的升力机制,在此基础上利用一维电流体动力学方法推导了升力和升力效率的公式.理论分析结果和实验值吻合良好,电飘机中升力的来源依赖于电晕电流的形成,并与电晕电流的大小相关.在电压不太高时,升力大小随电压的升高而增大,并大致呈抛物线关系,与电极间距成反比关系,与电极长度成正比关系.分析了空气参数对电飘机升力和效率的影响,发现减小离子在空气中的迁移率是提高效率的有效方法,但同时降低了升力.分析了电飘机的应用前景.      

非定常机匣处理对失速先兆波的抑制作用实验研究

非定常机匣处理在不影响效率的前提下可以明显提高压气机的稳定工作范围,针对这种通过改变斜槽和气室来调节壁面阻抗边界条件的新型处理机匣,从非定常角度,开展其对失速先兆波产生及发展的影响的实验研究.在压气机转子前缘附近沿圆周均匀布置八支高频响压力传感器,采集壁面动态压力信号,进行周向傅立叶分析(SFT)和功率谱密度分析(PSD),捕捉到旋转失速先兆波的出现和发展的动态细节,比较光壁和处理机匣两种情况的结果,证实了处理机匣并非阻止了失速先兆波的出现,而是有效的抑制了其非线性发展.非定常机匣处理改变了压气机系统的阻抗边界条件,能够在全过程中对低频扰动波进行有效的抑制,从而推迟旋转失速的发生,实现压气机的扩稳目的.      

绕不同头型回转体初生空化的实验研究

为了研究绕不同头型回转体初生空穴的形成、发展过程和流场特性,采用流动显示技术分别观察了绕平头和锥头回转体初生空化的形态,并应用粒子图像测速系统（PIV）测量了相应工况下的速度分布。结果表明,绕回转体的头型对初生空化数和空穴形态有重大影响。实验中平头回转体的初生空化数为1．2,而45。锥角头型的初生空化数则为0．9。绕回转体的初生空穴形成于回转体肩部稍靠后的位置且没有附着在其表面,呈游离型发夹状,同时绕平头回转体的初生空穴的尺度较大,其初生位置距离肩部及回转体的壁面均较远。流场测试结果表明,空化初生和绕回转体头部流场的旋涡强度有关。与锥头回转体相比,同一雷诺数条件下,绕平头回转体的分离涡尺度较大、边界层离壁面较远、高涡量区域较大且离壁面较远,这是造成两种头型具有不同初生空化特性的主要原因。     

The Structure and Dynamics of the Corona—Heliosphere Connection

Determining how the heliospheric magnetic field and plasma connect to the Sun’s corona and photosphere is, perhaps, the central problem in solar and heliospheric physics. For much of the heliosphere, this connection appears to be well understood. It is now generally accepted that so-called coronal holes, which appear dark in X-rays and are predominantly unipolar at the photosphere, are the sources of quasi-steady wind that is generally fast, >500?km/s, but can sometimes be slow. However, the connection to the Sun of the slow, non-steady wind is far from understood and remains a major mystery. We review the existing theories for the sources of the non-steady wind and demonstrate that they have difficulty accounting for both the observed composition of the wind and its large angular extent. A?new theory is described in which this wind originates from the continuous opening and closing of narrow open field corridors in the corona, which give rise to a web of separatrices (the S-Web) in the heliosphere. Note that in this theory the corona—heliosphere connection is intrinsically dynamic, at least for this type of wind. Support for the S-Web model is derived from MHD solutions for the corona and wind during the time of the August 1, 2008 eclipse. Additionally, we perform fully dynamic numerical simulations of the corona and heliosphere in order to test the S-Web model as well as the interchange model proposed by Fisk and co-workers. We discuss the implications of our simulations for the competing theories and for understanding the corona—heliosphere connection, in general.     

A Model to Predict Stall Inception of Transonic Axial Flow Fan/Compressors

A stall inception model for transonic fan/compressors is presented in this paper. It can be shown that under some assumptions the solution of unsteady flow field consists of pressure wave which propagates upstream or downstream, vortex wave and entropy wave convected with the mean flow speed. By further using the mode-matching technique and applying the conservation law and conditions reflecting the loss characteristics of a compressor in the inlet and outlet of the rotor or stator blade rows, a group of homogeneous equations can be obtained from which the stability equation can be derived. Based on the analysis of the unsteady phenomenon caused by casing treatments, the function of casing treatments has been modeled by a wall impedance condition which has been included in the stability model through the eigenvalues and the corresponding eigenfunctions of the system. Besides, the effect of shock waves in cascade channel on the stability prediction is also considered in the stall inception model. Finally, some numerical analysis and experimental investigation are also conducted with emphasis on the mutual comparison.     

Multi-Wavelength Observations of CMEs and Associated Phenomena

This chapter reviews how our knowledge of CMEs and CME-associated phenomena has been improved, since the launch of the SOHO mission, thanks to multi-wavelength analysis. The combination of data obtained from space-based experiments and ground based instruments allows us to follow the space-time development of an event from the bottom of the corona to large distances in the interplanetary medium. Since CMEs originate in the low solar corona, understanding the physical processes that generate them is strongly dependant on coordinated multi-wavelength observations. CMEs display a large diversity in morphology and kinematic properties, but there is presently no statistical evidence that those properties may serve to group them into different classes. When a CME takes place, the coronal magnetic field undergoes restructuring. Much of the current research is focused on understanding how the corona sustains the stresses that allow the magnetic energy to build up and how, later on, this magnetic energy is released during eruptive flares and CMEs. Multi-wavelength observations have confirmed that reconnection plays a key role during the development of CMEs. Frequently, CMEs display a rather simple shape, exhibiting a well known three-part structure (bright leading edge, dark cavity and bright knot). These types of events have led to the proposal of the ‘`standard model’' of the development of a CME, a model which predicts the formation of current sheets. A few recent coronal observations provide some evidence for such sheets. Other more complex events correspond to multiple eruptions taking place on a time scale much shorter than the cadence of coronagraph instruments. They are often associated with large-scale dimming and coronal waves. The exact nature of these waves and the physical link between these different manifestations are not yet elucidated. We also discuss what kind of shocks are produced during a flare or a CME. Several questions remain unanswered. What is the nature of the shocks in the corona (blast-wave or piston-driven?) How they are related to Moreton waves seen in Hα? How they are related to interplanetary shocks? The last section discusses the origin of energetic electrons detected in the corona and in the interplanetary medium. “Complex type III-like events,”which are detected at hectometric wavelengths, high in the corona, and are associated with CMEs, appear to originate from electrons that have been accelerated lower in the corona and not at the bow shock of CMEs. Similarly, impulsive energetic electrons observed in the interplanetary medium are not the exclusive result of electron acceleration at the bow shocks of CMEs; rather they have a coronal origin.     

Half-bridge neutral point diode clamped rectifier for power factor correction

A high power factor rectifier based on neutral point clamped scheme is proposed. The voltage stress of each power semiconductor of the adopted rectifier is equal to the half dc bus voltage instead of full dc link voltage in the conventional switching mode rectifier. The control signals of the power switches are derived from the dc link voltage balance compensator, line current controller, and dc link voltage regulator. The hysteresis current control scheme is employed to draw a clean sinusoidal line current, high input power factor, regulated dc link voltage, and balance capacitor voltages. Three voltage levels are generated on the ac terminal of the adopted rectifier. To verify the proposed operation scheme, performance characteristics are given by the experimental results.     

Effect of system response on partial surge initiated instability in a transonic axial flow compressor

Partial surge is a type of instability inception in transonic compressors and occurs in the form of axisymmetric low-frequency disturbances localized in the hub region. Previous studies illustrate that the frequency of partial surge is set by the Helmholtz frequency of the entire system,which motivates to propose a hypothesis that the system response performs an important role in the formation of partial surge. For further verification, a series of experiments are conducted to explore the link b...     

轴流压气机近失速及旋转失速全通道数值模拟

为研究轴流压气机失速起始的动态过程,对某两级低速轴流压气机的第1级进行整环全通道模拟.结果表明:在近失速点流场中存在周向大尺度的速度波动,该波动与静子叶排首先出现的周向不均匀分布的叶背附面层分离密切相关,并且随着压气机进一步节流,波动幅值逐渐增大,最终诱发转子若干通道出现严重附面层分离,堵塞流道,压气机进入旋转失速.失速团完全发展后的转动频率与试验结果吻合较好.      

单级轴流压气机失速起始的数值模拟

基于某亚声单级轴流压气机试验台孤立转子环境下预失速行为的研究成果,进一步数值研究了该试验台单级环境下的失速起始过程.数值探针的监测结果表明,失速起始过程中单级轴流压气机的流动失稳始于转子叶尖部位,这与前期针对该试验台流动失稳的测量结果是一致的.对数值模拟的瞬态流场进行分析表明,先兆波的型式已从孤立转子环境下的“突尖”型转变为单级环境下的“多个小失速团”型,说明静叶的存在改变了近叶尖载荷的周向分布规律.然而,“叶尖二次涡”的形成与运动依然是“多个小失速团”型先兆波浮现的流体动力学机理.      

Novel single-phase AC/DC converter with two PWM control schemes

A novel single-phase AC/DC converter with two pulsewidth modulation (PWM) schemes is proposed to draw a sinusoidal line current with nearly unity power factor, achieve balanced neutral point voltage and regulate the DC bus voltage. With the aid of neutral point clamped scheme, a three-level voltage pattern is generated on the AC side of the proposed rectifier. To track the tine current command derived from a voltage controller and a phase-locked loop circuit, a hysteresis current control scheme is used in the inner loop control. A capacitor voltage compensator is employed to achieve the balanced neutral point voltage. To investigate the effectiveness of the proposed control scheme, the simulation and experimental results based on a laboratory prototype circuit are performed.     

The Solar Magnetic Field as a Coronal Hole Extension Forms: Effects of Magnetic Helicity and Boundary Conditions

An analytical solution is presented for linear force fields within a spherical shell, representing the solar corona. Allowing for a global magnetic helicity, we find magnetic fields over the entire corona with realistic inner boundary conditions obtained from transformation and extrapolation of photospheric magnetograms and considering alternative outer boundary conditions. Such fields are found for the well known coronal hole extension event of August 1996. This revised version was published online in June 2006 with corrections to the Cover Date.     

Plasma-physical aspects of the solar cycle

Mass motions below the photosphere drive the solar cycle which is associated with variations in the magnetic field structure and accompanying phenomena. In addition to semi-empirical models, dynamo theories have been used to explain the solar cycle. The emergence of magnetic field generated by these mechanisms and its expansion into the corona involves many plasma physical processes. Magnetic buoyancy aids the expulsion of magnetic flux. The corona may respond dynamically or by continually adjusting to a quasi-static force-free or pressure-balanced equilibrium. The formation and disruption of current sheets is significant for the overall structure of the coronal magnetic field and the physics of quiescent prominences. The corona has a fine structure consisting of magnetic loops. The structure and stability of these are important as they are one of the underlying elements which make up the corona.     

The heating of the solar corona

In this paper a discussion is given of the present state of the theory of the heating of the solar corona by shock waves. Arguments are presented why the main contribution to the mechanical energy flux is of acoustic origin, while estimates for the amount of acoustic energy generated in the convection zone as well as the deviations from isotropy are given. During propagation through the atmosphere acoustic waves develop into shock waves after a distance of a few scale heights in the chromosphere. The heating of the outer layers by dissipation of shock waves is found to be sufficient to account for the observed radiative and corpuscular energy losses.Much emphasis is laid on the competitive role played by the four fundamental processes of energy transfer: mechanical heating, radiation, heat conduction and convection of energy in establishing the equilibrium structure of the corona. The atmosphere may be divided in several regions according to the predominance of one of the energy processes mentioned above.The physical properties of the chromosphere and the solar wind are discussed only where they are intimately connected with the problem of the heating of the corona.The most important aspects of the influence of a magnetic field on the structure and the heating of the corona in magnetically active regions are briefly mentioned. Special attention is paid to the strong channelling of heat flow along the field lines and its consequences for the structure and dynamics of the chromosphere-corona transition layer.