行星际MHD激波的速度

本文导出了ＭＨＤ激波相对子上游介质传播速度的一般公式，指出ＭＨＤ激波的相对速度由激波上下游密度比、上游激波角、上游等离子体β值和温度决定．在低β高温等离子体中激波相对速度较大，密度比和激波角越大相对速度也越大．在不同流速的太阳风中激波相对速度均随日心距下降，但都比气体爆炸激波预言的慢．     

行星际日冕物质抛射中的磁流体波动观测

日冕物质抛射（CME）是最大尺度的太阳活动现象,灾害性空间天气的主要驱动源．行星际日冕物质抛射（ICME）中的等离子体波动性质与ICME的演化密切相关．由于ICME中的平均磁场较大,其中的Alfven低频扰动研究较少．前人的研究只分析了0．3AU和0．68AU处的个别ICME中的Alfven波动．ICME在1AU处的Alfven波观测较少．本文对第23太阳周1995—2006年期间所有引起大磁暴（Dst≤－100nT）的单个ICME事件进行统计分析,结果表明：（1）大约30％的ICME中长时间存在Alfven波（超过ICME持续时间的30％）;（2）约一半的ICME的鞘层中存在快磁声波;（3）所有ICME中都存在短时间段的慢磁声波．这些观测结果为研究CME在行星际传播过程时其中的Alfven波演化机制及其动力学演化提供了观测基础．     

一类等熵欧拉方程组的流近似

研究了一类带有流扰动的一般压力等熵欧拉方程组的黎曼问题，获得了包含5种不同结构的黎曼解.证明了当包含压力的3-参数流扰动消失时，任何包含2个激波的黎曼解收敛于零压流系统的狄拉克激波解；任何包含2个稀疏波的黎曼解收敛于零压流系统的真空解.还证明了当包含压力的2-参数流扰动消失时，任何满足一定初值条件的2-激波黎曼解收敛于一类Chaplygin型气体方程组的狄拉克激波解.最后，对狄拉克激波和真空状态的形成过程进行了数值模拟.     

Richtmyer-Meshkov不稳定性的格子Boltzmann数值模拟

为了探寻研究Richtmyer-Meshkov(RM)不稳定性的新方法,采用耦合双分布函数格子Boltzmann方法(LBM),对激波作用下两种不同密度流体交界面的演化过程进行了数值模拟研究,着重讨论了RM不稳定性的行程和演化特征,给出了交界面的扰动增长率的变化规律,同时还研究了激波强度对扰动振幅的影响.结果表明:由于受RM不稳定性的影响,两种不同密度流体的交界面上,重流体演化成尖顶结构,而轻流体演化成气泡结构,最终由于斜压效应重流体的尖顶转变成蘑菇头形状;交界面扰动增长率与Zhang-Sohn模型较吻合;激波强度越大,扰动振幅增长率越高.研究表明所提的方法可以用于RM不稳定性的研究,有望成为两相流研究的新途径.     

沸腾液体扩展蒸汽爆炸初期演化过程的数值模拟

对沸腾液体扩展蒸汽爆炸发生初期,容器顶部突然出现开口,压力快速泄放导致容器内介质过热沸腾的过程进行了模拟研究。选取过热水及饱和水蒸气为容器内介质,分析了该过程中气液两相的变化过程。探讨了初始温度（初始压力）、初始充装量及开口大小等因素对前述物理过程及容器内压力、温度的影响。结果表明：容器内过热沸腾的过程中,温度逐渐下降,压力响应会出现两次压力峰和一个压力平台期,两个压力峰值都会随初始温度的增加而增加,压力平台持续时间随初始温度先增大后减小;第一个压力峰值随初始充装量的增加先增大后减小,第二个压力峰值则随初始充装量的增加而增大,压力平台的持续时间和液体充装量成正比关系;开口越大两个压力峰值也越大,压力平台持续时间越短。     

RFT-2000型透平式热分离机原理及其应用

1,工作原理 RFT-2000型透平式热分离机是由高速旋转的喷嘴和配置在旋转喷嘴四周的接受管组成(见图1).带压气体经转子中心孔进入喷嘴发生膨胀,压力与温度降低,在近喷嘴出口截面处气流速度达到音速,并以一定方向流出喷嘴,进入接受管。 气流对喷嘴产生的推力使喷嘴旋转,依次对每根接受管射气。接受管的一端正对喷嘴出口气流方向,另一端封闭。高速气流进入接受管后压力与温度一般要继续降低,冲击着管内原气体,在接触面前方形成激波,激波以更高的速度向封闭端传播。由于激波压缩使激波和接触而之间的气体压力、温度和密度升高。RFT—2000型热…     

纯音脉冲强度JND测试值与SPIN理论严重背离

对不同持续时间１ｋＨｚ纯音的强度ＪＮＤ的测量表明，Ｗｅｂｅｒ比随信号持续时间的增加而减小，减小的速度信号持续时间的增加而减缓，到信号持续时间增另到５ｓ时Ｗｅｂｅｒ比不再随信号持续时间的增加而减小，此时Ｗｅｂｅｒ比随强度的变化与Ｗｅｂｅｒ定律极为接拉，而与内部泊松内部噪声（ＰＩＮ）理论，以及饱和内部泊松内部噪声（ＳＰＩＮ）理论的预期严重背离。     

激波反射对扰动界面湍流混合区影响的数值分析

发展三维可压缩多介质黏性流动和湍流流动的大涡数值模拟方法MVFT3D,对Poggi等人进行的重流体冲击加载轻流体激波管界面不稳定性实验进行数值模拟,通过Vreman SGS应力模型模拟小尺度运动对大尺度运动的影响,运用统计方法分析湍动能特征。计算结果显示,激波多次加载下扰动界面不稳定性及其诱发的湍流混合是一个非常复杂的发展演化过程,在反射激波第一次加载前湍流混合区宽度增长缓慢,湍动能按时间和空间的1.3次幂指数规律衰减,再加载后湍流混合区宽度非线性增长加快,湍动能强度迅速增强后再逐渐递减,而后期的流场则出现明显的气泡竞争现象。计算给出两次再加载的湍流混合区宽度与实验测试结果吻合,第一次再加载前湍动能随时间和空间1.3次幂指数衰减规律与Mohamed和Larue的研究结论一致。数值模拟再现了实验观察到的激波多次加载过程并描述了湍流混合区发展演化的基本物理特征,检验了数值方法和计算程序。     

多孔颗粒床阴燃着火实验研究与数值分析

对发生在多孔颗粒床的阴燃着火过程进行了实验研究，针对最常见的加热方式热接触，设计了平板加热的实验模型，实验表明，长时间的缓慢升温后突然出现温度的跃升是阴燃着火的基本特征，采用有限区域临界着火理论进行了数值模拟计算，得出了发生阴燃着火的临界现象的规律，主要包括：（1）燃料床尺寸不变时，如果临界热流密度增加，则临界环境温度降低，临界点燃温度增高；（2）环境温度不变时，如果临界热流密度增加，则燃料床的临界尺寸减小，临界点燃温度增高；（3）热流密度不变时，如果环境温度较高，则点燃的临界尺寸较小，同时临界点燃温度较高，以上结论与实验结果一致。     

纤锌矿结构的GaAlN/GaN量子阱中电子激发态极化的压力效应

研究了GaN／GaAlN量子阱内电子的激发态极化（EESP）的压力效应，计算中考虑了纤锌矿结构材料的晶格常数、形变势的各向异性。以及内建电场（IEF）的作用．结果表明：电子势垒高度随压力下降；电子基态有效质量随压力下降而电子的第一激发态有效质量随压力上升；EESP强度随压力缓慢上升；电子极化的偶极矩随Al浓度非线性下降．一般情况下，EESP对IEF的影响可忽略，但当掺杂浓度n足够大（n〉10^19／cm^3）时，EESP可屏蔽IEF．     

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.     

An interplanetary shock traced by planetary auroral storms from the Sun to Saturn

A relationship between solar activity and aurorae on Earth was postulated long before space probes directly detected plasma propagating outwards from the Sun. Violent solar eruption events trigger interplanetary shocks that compress Earth's magnetosphere, leading to increased energetic particle precipitation into the ionosphere and subsequent auroral storms. Monitoring shocks is now part of the 'Space Weather' forecast programme aimed at predicting solar-activity-related environmental hazards. The outer planets also experience aurorae, and here we report the discovery of a strong transient polar emission on Saturn, tentatively attributed to the passage of an interplanetary shock--and ultimately to a series of solar coronal mass ejection (CME) events. We could trace the shock-triggered events from Earth, where auroral storms were recorded, to Jupiter, where the auroral activity was strongly enhanced, and to Saturn, where it activated the unusual polar source. This establishes that shocks retain their properties and their ability to trigger planetary auroral activity throughout the Solar System. Our results also reveal differences in the planetary auroral responses on the passing shock, especially in their latitudinal and local time dependences.     

Responses of the magnetotail plasma sheet to two interplanetary shocks: TC-1 observations

Two interplanetary shocks are examined to determine the responses of the magnetic field and plasma in the plasma sheet upon the shock impacts by using TC-1 observational data.The two shocks are observed by WIND on November 7,2004.Prior to and after the shock,the IMF is either weakly southward or northward.The responses of the plasma sheet to the two shocks are intense and much similar.When the shock interacts with the magnetosphere,the magnetic field impulsively increases 1-2 min after the geomagnetic field...     

两弹性接触粗糙低速滑动表面温升的分形模型

采用球形微凸体的赫兹接触理论和MB模型,对微接触点的稳态温升、瞬态温升进行了分析,得到了低速滑动区域内的分形区域实际接触面积温升概率分布密度的封闭形式表达式.分析结果说明:摩擦副表面粗糙度、最大弹性微接触点的面积、域扩展系数均随分形维数增加而减小,域分开系数随分形维数增加而线性增加.最大温升随分形维数增加而减小,总体上随实际接触面积增加而线性增加,还随分形粗糙度参数增加而增加.当温升增加时,受给定温升的微接触点数减小会导致实际接触面积的温升概率分布密度下降.考虑了各接触微凸体之间相互作用的瞬态温升效应,但计算表明在低速滑动区域可以不考虑其影响.     

Optimal disturbances rejection control for singularly perturbed systems with time-delay

The optimal control design for singularly perturbed time-delay systems affected by external disturbances is considered. Based on the decomposition theory of singular perturbation, the system is decomposed into a fast subsystem without time-delay and a slow time-delay subsystem with disturbances. The optimal disturbances rejection control law of the slow subsystem is obtained by using the successive approximation approach (SAA) and feedforward compensation method. Further, the feedforward and feedback composite control (FFCC) law for the original problem is developed. The FFCC law consists of linear analytic terms and a time-delay compensation term which is the limit of the solution sequence of the adjoint vector equations. A disturbance observer is introduced to make the FFCC law physically realizable. Numerical examples show that the proposed algorithm is effective.     

空间灾害性扰动事件数值预报初探——行星际激波动力学问题6步求解法

空间灾害性天气的预报是日地物理学界及高科技领域的热门话题.未来预测太阳剧烈扰动所造成的行星际风暴到达地球空间的状态势必借助于数值方法.浅析了空间灾害性扰动事件数值预报存在的问题及未来设想, 针对这一目的对一维球对称问题提出了处理行星际激波的 6步求解方法,指出未来空间灾害性扰动事件预报模式应是一个基于三维的以真实太阳风为背景自洽建立起来的、以太阳等离子体输出及磁场全球结构为初边值、太阳、行星际、地磁因果耦合模式.     

林火干扰对广东马尾松林土壤有机碳密度及其活性有机碳的影响

【目的】森林在全球碳循环中发挥着重要作用。林火干扰是全球生物地球化学循环的关键驱动因子,影响植被结构变化及森林演替方向,从而对森林生态系统土壤有机碳密度及碳周转产生重要作用,进而影响森林碳循环与碳平衡。笔者定量研究林火干扰对森林生态系统土壤有机碳密度及其活性有机碳的影响,科学阐明林火干扰对森林生态系统土壤有机碳的影响机制,为火烧迹地恢复与森林碳减排增汇提供参考。【方法】以广东省佛冈马尾松林为研究对象,采用相邻样地比较法、化学分析法,在森林生态系统水平上,定量测定不同林火干扰强度对土壤有机碳密度、土壤活性有机碳含量和细根生物量的影响,对林火干扰后土壤有机碳密度的变化进行定量研究,探讨林火干扰对土壤有机碳密度以及活性有机碳的影响机制,深入分析森林生态系统土壤有机碳的循环与分配过程。【结果】林火干扰对马尾松林的土壤有机碳密度、活性有机碳含量和细根生物量均有影响,不同林火干扰强度下土壤有机碳密度与土壤活性有机碳含量变化趋势均表现为对照>轻度林火干扰>中度林火干扰>重度林火干扰。轻度林火干扰对土壤有机碳密度的影响差异不显著(P>0.05),而中度和重度林火干扰则显著降低土壤有机碳密度(P<0.05)。林火干扰的马尾松林土壤细根生物量均低于对照样地,变化趋势为重度林火干扰>中度林火干扰>轻度林火干扰,轻度林火干扰只显著降低土壤表层细根生物量(P<0.05),而中度和重度林火干扰显著降低了土壤表层和浅层细根生物量(P<0.05)。【结论】林火干扰减小了土壤有机碳密度,减少幅度随土壤剖面深度增加而逐渐变小。轻度林火干扰仅显著降低了表层土壤有机碳密度,而中度和重度林火干扰显著降低了土壤表层和浅层土壤有机碳密度,进而导致土壤有机碳密度显著变化。林火干扰对土壤活性有机碳含量产生了影响。林火干扰后马尾松林4种土壤活性有机碳含量均呈下降趋势,但仅中度和重度林火干扰差异显著。活性有机碳含量各组分随林火干扰强度增加沿土壤剖面递减的幅度呈现一定差异,重度林火干扰后的递减趋势最强。此外,林火干扰还降低了马尾松林土壤细根生物量。     

两弹性接触粗糙快速滑动表面温升的分形模型

采用球形微凸体的赫兹接触理论和MB模型,对微接触点的温升进行了分析,得到了快速滑动区域内的分形区域实际接触面积的温升概率分布密度、温升补充累积概率分布函数的封闭式表达式.分析结果说明:量纲一特定滑动区域的实际接触面积随量纲一最大Jaeger参数增加而单调减小.量纲一最大温升随分形维数增加而减小,但随分形粗糙度参数增加而增加.量纲一温升随分形维数增加而增加.当分形维数为1.5时,实际接触面积的温升概率分布密度等于在一个弹性微接触点面积上的温升概率分布密度,基于正八边形面积的近似解适当接近精确解.温升的补充累积概率分布函数随分形维数、滑动速度和量纲一分形粗糙度参数增加而增加.     

Response of the magnetic field and plasmas at the geosynchronous orbit to interplanetary shock

Interplanetary shock can greatly disturb the Earth＇s magnetosphere and ionosphere, causing the temporal and spatial changes of the magnetic field and plasmas at the geosynchronous orbit. In this paper, we use the magnetic field data of GOES satellites from 1997 to 2007 and the plasma data of MPA on the LANL satellites from 1997 to 2004 to study the properties of magnetic field and plasma （0.03-45 keV） at the geosynchronous orbit （6.6 RE） within 3 hours before and after the arrival of shock front at the geosynchronous orbit through both case study and superposed epoch analysis. It is found that following the arrival of shock front at the geosynchronous orbit, the magnetic field magnitude, as well as GSM Bzcomponent increases significantly on the dayside （8-16 LT）, while the By component has almost no change before and after shock impacts. In response to the interplanetary shock, the proton becomes much denser with a peak number density of 1.2 cm^-3, compared to the typical number density of 0.7 cm^-3. The proton temperature increases sharply, predominantly on the dusk and night side. The electron, density increases dramatically on the night side with a peak number density of 2.0 cm^-3. The inferred ionospheric O^＋ density after the interplanetary shock impact reaches the maximum value of 1.2 cm^-3 on the dusk side and exhibits the clear dawn-dusk asymmetry. The peak of the anisotropy of proton＇s temperature is located at the noon sector, and the anisotropy decreases towards the dawn and dusk side. The minimum of temperature anisotropy is on the night side. It is suggested that the electromagnetic ion cyclotron （EMIC） wave and whistler wave can be stimulated by the proton and electron temperature anisotropy respectively. The computed electromagnetic ion cyclotron wave （EMIC） intense on the day side （8--16 LT） with a frequency value of 0.8 Hz, and the wave intensity decreases towards the dawn and dusk side, the minimum value can be found on the night side. The computed electron whistler wave locates on the day side （8--16 LT） with a value of 2 kHz.     

TC11钛合金与5CrMnMo模具钢间接触换热实验研究

基于稳态热流法,利用自制的接触换热系数测量装置对TC11钛合金与5CrMnMo模具钢间的接触换热进行测试,探讨了界面荷载、界面温度、接触面粗糙度和玻璃润滑剂对接触换热系数的影响.实验结果表明:接触换热系数随界面荷载的增加而增大,且与界面荷载的幂指数函数近似成正比关系;接触换热系数随界面温度的升高总体上呈增大趋势;在相对较小的粗糙度范围内,产生接触换热系数随接触面粗糙度增加而增大的反常现象;玻璃润滑剂的存在使接触换热系数降低了1～2个数量级,厚度的影响尤其明显.