EBT中的弱相对论哨声波不稳定性

讨论了在具有热电子环的ＥＢＴ装置中，弱相对论捕获电子对哨声波不稳定的影响。从 回旋动力论方程出发，用解析法求出了哨声模的实频和不稳定性增长率。发现在温度各向异性下的捕获电子共振效应会导致哨声波不稳定性；相对论效应会增大不稳定性最大增表率，同时使不稳定性最大值向低频段移动。     

哨声模合声波驱动同步轨道高能电子通量上升的事例分析

采用LANL同步轨道卫星和ClusterC4卫星的数据,研究了2004年9月13日和2001年10月21日两个磁暴事件期间,辐射带同步轨道附近高能电子通量的变化和哨声模合声波的活动之间的关系．通过观测对比发现,在相同的空间位置,两个事件均观测到高能电子通量的上升和明显的合声波对磁场的扰动;而且高能电子通量上升的程度与合...     

绝热放电现象和粒子碰撞对磁化尘埃等离子体中、低频静电波稳定性的影响

考虑到尘埃绝热放电现象、外磁场、碰撞、离子与尘埃温度之比、电子与离子数密度之比以及斜传播等因素对均匀尘埃等离子体中低频静电波的影响，其中包括高能离子和玻耳兹曼分布电子，运用简正模分析法，得出了低频波的色散关系．研究表明，以上诸因素对低频波有很大影响．研究中包括两种不同的低频波模式．在研究斜传播对低频波的影响时，发现当θ=π／2时，第一种模式是稳定的；而第二种模式存在一个稳定区域，即1.3≤θ≤1.7.     

载流等离子体中的修正双流不稳定性

本文研究载流等离子体中的修正双流不稳定性.我们从Braginskii 流体方程组出发,考虑了密度梯度和电子成分与离子成分之间的碰撞相互作用,导出了一般色散关系,本征频率和增长率的公式.结果表明,粒子的热效应使得本征频率增加,并且在一定的参范围内,它对该模起解稳作用.最后,我们给出了不稳定性增长率对于传播方向,粒子漂移速度,密度梯度以及温度的依赖关系和数值结果.     

钢板不等温拉深成形的影响因素研究

建立了高温下方盒形件不等温拉深成形的有限元模型.利用正交试验,研究热冲压过程中模具温度对22MnB5钢板的不等温拉深成形能力的影响,并分析零件几何参数对22MnB5钢板的不等温成形能力的影响.结果表明,模具温度越高,22MnB5钢板的成形能力越好;其中凹模温度对成形能力的影响最大,压边圈影响次之,凸模温度影响不大.方盒形件的凸、凹模圆角半径越大,22MnB5钢板在高温下不等温拉深成形能力越好;转角半径越大,转角区域越不易起皱.     

绝热放电现象和粒子碰撞对磁化尘埃等离子体中低频静电波稳定性的影响

考虑到尘埃绝热放电现象、外磁场、碰撞、离子与尘埃温度之比、电子与离子数密度之比以及斜传播等因素对均匀尘埃等离子体中低频静电波的影响,其中包括高能离子和玻耳兹曼分布电子,运用简正模分析法,得出了低频波的色散关系.研究表明,以上诸因素对低频波有很大影响.研究中包括两种不同的低频波模式.在研究斜传播对低频波的影响时,发现当θ=π/2时,第一种模式是稳定的;而第二种模式存在一个稳定区域,即1.3≤θ≤1.7.     

热价值理论及其在加热炉节能中的应用

给出了预热助燃空(煤)气和热装时的热价值计算公式,比较加热炉的热工指标,指出热价值可以合理评价热能在加热炉中的有效利用状况.建立了炉内逆流换热模型,主要利用热价值理论研究了预热空(煤)气和热装对热价值的影响.结果表明:提高预热温度,热价值升高,且随着预热温度的进一步提高,热价值的增长率变小;热装可以使热价值升高,且热装温度越高,其热价值的增长率越大;设计时,当装料温度较高时应选择小的炉长,预热温度较高时应选择大的炉长.     

轴向受压光热敏感凝胶杆屈曲失稳分析

当压缩载荷达到失稳临界值时轴向受压细长杆将发生屈曲失稳,从而影响系统的正常运作。为分析光热敏感细长凝胶直杆轴向受压的稳定性问题,通过光热敏感凝胶大变形理论和铁木辛柯弹性稳定理论研究了环境温度、光强对不同长细比凝胶杆屈曲行为的影响。结果表明:化学势、光强和温度对光热敏感凝胶压杆的增量模量具有显著影响;溶液化学势越低、辐射光光强越弱、温度越低,光热敏感凝胶压杆的增量模量越高;光热敏感凝胶杆轴向受压时存在临界长细比,只有当长细比大于该临界值时凝胶压杆才会发生屈曲失稳;临界长细比受光强和温度影响显著,光强越强、温度越高时,临界长细比越大;当长细比大于临界值时,光强越强、温度越高则使凝胶杆发生屈曲的临界应力越大。     

循环流化床床层与壁面间传热特性的模拟分析

利用已建立的数学模型，对循环流化床床层与壁面间的传热特性进行了预测．分析了床层密度、床层温度、流化速度、颗粒粒径以及壁面长度等设计和运行参数对传热系数的影响．结果表明，床层密度越大或温度越高，传热系数越大；而颗粒粒径越大或壁面长度越大，传热系数越小；流化速度对传热系数则影响不大．     

WAVE-CISK斜交型扰动不稳定谱点分布的半圆定理

对WAVE-CISK斜交型不稳定扰动的谱点分布作了理论分析,得出了有别于Howard半圆定理的该谱点分布的半圆定理;还对该不稳定扰动的增长率上界作了估计,发现对流凝结加热反馈越大,风速垂直切变越大,纬度越高,扰动水平尺度越小,模式顶越高,则该估值就越大;层结稳定度的减小则不利于不稳定能量的累积,故该估值反而减小.     

The unexpected origin of plasmaspheric hiss from discrete chorus emissions

Plasmaspheric hiss is a type of electromagnetic wave found ubiquitously in the dense plasma region that encircles the Earth, known as the plasmasphere. This important wave is known to remove the high-energy electrons that are trapped along the Earth's magnetic field lines, and therefore helps to reduce the radiation hazards to satellites and humans in space. Numerous theories to explain the origin of hiss have been proposed over the past four decades, but none have been able to account fully for its observed properties. Here we show that a different wave type called chorus, previously thought to be unrelated to hiss, can propagate into the plasmasphere from tens of thousands of kilometres away, and evolve into hiss. Our new model naturally accounts for the observed frequency band of hiss, its incoherent nature, its day-night asymmetry in intensity, its association with solar activity and its spatial distribution. The connection between chorus and hiss is very interesting because chorus is instrumental in the formation of high-energy electrons outside the plasmasphere, whereas hiss depletes these electrons at lower equatorial altitudes.     

Scattering by chorus waves as the dominant cause of diffuse auroral precipitation

Earth's diffuse aurora occurs over a broad latitude range and is primarily caused by the precipitation of low-energy (0.1-30-keV) electrons originating in the central plasma sheet, which is the source region for hot electrons in the nightside outer magnetosphere. Although generally not visible, the diffuse auroral precipitation provides the main source of energy for the high-latitude nightside upper atmosphere, leading to enhanced ionization and chemical changes. Previous theoretical studies have indicated that two distinct classes of magnetospheric plasma wave, electrostatic electron cyclotron harmonic waves and whistler-mode chorus waves, could be responsible for the electron scattering that leads to diffuse auroral precipitation, but it has hitherto not been possible to determine which is the more important. Here we report an analysis of satellite wave data and Fokker-Planck diffusion calculations which reveals that scattering by chorus is the dominant cause of the most intense diffuse auroral precipitation. This resolves a long-standing controversy. Furthermore, scattering by chorus can remove most electrons as they drift around Earth's magnetosphere, leading to the development of observed pancake distributions, and can account for the global morphology of the diffuse aurora.     

Electron acceleration from contracting magnetic islands during reconnection

A long-standing problem in the study of space and astrophysical plasmas is to explain the production of energetic electrons as magnetic fields 'reconnect' and release energy. In the Earth's magnetosphere, electron energies reach hundreds of thousands of electron volts (refs 1-3), whereas the typical electron energies associated with large-scale reconnection-driven flows are just a few electron volts. Recent observations further suggest that these energetic particles are produced in the region where the magnetic field reconnects. In solar flares, upwards of 50 per cent of the energy released can appear as energetic electrons. Here we show that electrons gain kinetic energy by reflecting from the ends of the contracting 'magnetic islands' that form as reconnection proceeds. The mechanism is analogous to the increase of energy of a ball reflecting between two converging walls--the ball gains energy with each bounce. The repetitive interaction of electrons with many islands allows large numbers to be efficiently accelerated to high energy. The back pressure of the energetic electrons throttles reconnection so that the electron energy gain is a large fraction of the released magnetic energy. The resultant energy spectra of electrons take the form of power laws with spectral indices that match the magnetospheric observations.     

自由电子激光器的渐近分析

对于波动器磁场纵向渐变的自由电子激光器,不仅渐变锥度对电子能量有累积影响,而且信号场的增长率对电子能量也有累积效应,这些高阶微量要以通过将运动方程和波动方程渐近展开后得到,由电子能量谐振的发生条件可以确定系统参数慢变和更慢变的２种特性以及系统信号场微速、低速和高速等３级不同的增长速率,这是一个有微摄动带慢变参数的强非线性振动系统。     

Fast acceleration of “killer” electrons and energetic ions by interplanetary shock stimulated ULF waves in the inner magnetosphere

Energetic electrons and ions in the Van Allen radiation belt are the number one space weather threat. Understanding how these energetic particles are accelerated within the Van Allen radiation belt is one of the major challenges in space physics. This paper reviews the recent progress on the fast acceleration of "killer" electrons and energetic ions by ultralow frequency (ULF) waves stimulated by the interplanetary shock in the inner magnetosphere. Very low frequency (VLF) wave-particle interaction is considered to be one of the primary electron acceleration mechanisms because electron cyclotron resonances can easily occur in the VLF frequency range. Recently, using four Cluster spacecraft observations, we have found that, after interplanetary shocks impact the Earth’s magnetosphere, energetic electrons in the radiation belt are accelerated almost immediately and continue to accelerate for a few hours. The time scale (a few days) for traditional acceleration mechanisms, based on VLF wave-particle interactions to accelerate electrons to relativistic energies, is too long to explain our observations. Furthermore, we have found that interplanetary shocks or solar wind pressure pulses, with even small dynamic pressure changes, can play a non-negligible role in radiation belt dynamics. Interplanetary shocks interaction with the Earth’s magnetosphere manifests many fundamental space physics phenomena including energetic particle acceleration. The mechanism of fast acceleration of energetic electrons in the radiation belt responding to interplanetary shock impacts consists of three contributing parts: (1) the initial adiabatic acceleration due to strong shock-related magnetic field compression; (2) followed by the drift-resonant acceleration with poloidal ULF waves excited at different L-shells; and (3) particle acceleration due to the quickly damping electric fields associated with ULF waves. Particles end up with a net acceleration because they gain more energy in the first half of this cycle than they lose in the second. The results reported in this paper cast a new light on understanding the acceleration of energetic particles in the Earth’s Van Allen radiation belt. The results of this study can likewise be applied to interplanetary shock interaction with other planets such as Mercury, Jupiter, Saturn, Uranus and Neptune, and other astrophysical objects with magnetic fields.     

SiH_4射频辉光放电等离子体特性的光发射研究

采用ＯＭＡ－４０００测量了ＳｉＨ_４射频辉光放电等离子体的光发射谱，研究了其谱线强度随放电射频功率和反应气体流量间的变化关系。结果表明：在放电射频功率增加和反应气体流量升高的过程中。其等离子体状态分别发生了性质不同的转变，这种转变联系到射频功率耗散机制的变化。当反应气体流量增加时，电子获得能量的机制由阴极暗区加速转变为等离子体内电场的加热效应；而在放电功率升高的过程中，离子轰击阴极产生的二次电子发射效应导致了光发射谱强度急剧增强的转变。     

旋拧射流的线性稳定性研究

用Chebyshev谱配置法求解柱坐标下线化不可压缩Navier-Stokes方程,分析喷管出口附近粘性旋摈射流的线性稳定性,为了研究离心不稳定对线性增长率的影响,本研究中基本流的周向速度可以是离心稳定的,也可以是离心不稳定的,结果表明在一定参数下旋摈能增强扰动的线性增长率,且对于离心不稳定的剖面增长率升高更大,对于离心稳定的速度型,有旋拧时轴对和我模态的增长率轻微下降,而负周向波数扰动的增长率明显上升,对于离心不稳定的速度型,可以观察到优势模态由低波数量的Kelvin-Helmholtz(K-H)不稳定波转换到高波数时的离心不稳定。     

平衡式Ku波段低噪声放大器ADS仿真

平衡放大技术具有驻波特性好,增益高,易级联等特点。这里把平衡放大技术应用到Ku波段低噪声放大器的设计当中,在保证低噪声和功率增益的同时,用以提高低噪放的驻波比和增益平坦度。ADS仿真结果显示,在10～12 GHz频带范围内,低噪声放大器绝对稳定,噪声系数≤0.7 dB,功率增益达到≤10 dB,通过采用平衡放大技术,输入输出驻波比≤1.12∶1,带内波动≤0.5 dB。提高了低噪声放大器的有效工作带宽。