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61.
塞式喷管三维流场的数值模拟 总被引:2,自引:0,他引:2
从曲线坐标下的三维平均雷诺的N-S方程出发,并用k-ε两方程湍流模型封闭方程组,采用二阶精度的精度无波动、无自由参数的耗散差分格式(NND格式),发展了模拟塞式喷管三维流场的数值程序,并对线性塞式喷管和瓦状塞式喷管在不同落压比下的三维流场进行了数值模拟研究.结果较好地预示了塞式喷管的三维流场特征,并且显示瓦状塞式喷管除了圆柱形结构比平板更能承载外,其塞锥压强分布可以进一步改善其受力情况. 相似文献
62.
In this paper we review the possible mechanisms for production of non-thermal electrons which are responsible for the observed
non-thermal radiation in clusters of galaxies. Our primary focus is on non-thermal Bremsstrahlung and inverse Compton scattering,
that produce hard X-ray emission. We first give a brief review of acceleration mechanisms and point out that in most astrophysical
situations, and in particular for the intracluster medium, shocks, turbulence and plasma waves play a crucial role. We also
outline how the effects of the turbulence can be accounted for. Using a generic model for turbulence and acceleration, we
then consider two scenarios for production of non-thermal radiation. The first is motivated by the possibility that hard X-ray
emission is due to non-thermal Bremsstrahlung by nonrelativistic particles and attempts to produce non-thermal tails by accelerating
the electrons from the background plasma with an initial Maxwellian distribution. For acceleration rates smaller than the
Coulomb energy loss rate, the effect of energising the plasma is to primarily heat the plasma with little sign of a distinct
non-thermal tail. Such tails are discernible only for acceleration rates comparable or larger than the Coulomb loss rate.
However, these tails are accompanied by significant heating and they are present for a short time of <106 years, which is also the time that the tail will be thermalised. A longer period of acceleration at such rates will result
in a runaway situation with most particles being accelerated to very high energies. These more exact treatments confirm the
difficulty with this model, first pointed out by Petrosian (Astrophys. J. 557:560, 2001). Such non-thermal tails, even if possible, can only explain the hard X-ray but not the radio emission which needs GeV or
higher energy electrons. For these and for production of hard X-rays by the inverse Compton model, we need the second scenario
where there is injection and subsequent acceleration of relativistic electrons. It is shown that a steady state situation,
for example arising from secondary electrons produced from cosmic ray proton scattering by background protons, will most likely
lead to flatter than required electron spectra or it requires a short escape time of the electrons from the cluster. An episodic
injection of relativistic electrons, presumably from galaxies or AGN, and/or episodic generation of turbulence and shocks
by mergers can result in an electron spectrum consistent with observations but for only a short period of less than one billion
years. 相似文献
63.
平均轨道要素在卫星轨道设计及星座仿真中具有非常重要的作用。在综合国内外现有研究成果的基础上,给出了一整套简单实用、没有奇点的密切要素与平均要素间的相互转化方法,用此法进行的星座设计及仿真工作表明该方法非常有用。同时给出了利用平均轨道要素得以的关于赤道平面圆轨道的一个有意义的结论。 相似文献
64.
S.V. Chalov H.J. Fahr 《Advances in Space Research (includes Cospar's Information Bulletin, Space Research Today)》2011
In this paper we start from the most recently observed fact that the solar wind plasma after passage over the termination shock is still supersonic with a Mach number of about 2. To explain this unexpected phenomenon and to predict the evolution of properties of the downstream plasma flow we here consider a two-fluid proton plasma with pick-up protons as a separate suprathermal, second proton fluid. We then formulate a self-consistent system of hydrodynamical conservation equations coupling the two fluids by dynamical and thermodynamical coupling terms and taking into account the effects of newly incorporated protons due to charge exchange with the H-atoms in the heliosheath. This then allows us to predict that in the most probable case the solar wind protons will become subsonic over a distance of about 30 AU downstream of the shock. As we can also show, it may, however, happen that the plasma mixture later again reconverts to a supersonic signature and has to undergo a second shock before meeting the heliopause. 相似文献
65.
针对多星对地观测系统联合任务规划问题,考虑卫星载荷具备连续侧摆能力和多种数据压缩模式的新特点,构建了多星联合任务规划模型,在此基础上设计多星联合任务规划和数传调度算法框架,实现了卫星连续侧摆成像规划算法和基于任务优先级的数传任务调度算法,最后采用实际算例进行试验,结果表明文章提出的多星联合任务规划方法能在提高完成任务数量的同时降低卫星资源消耗,满足实际应用需求。 相似文献
66.
M. Ishiguro Y. Sarugaku S. Nishihara Y. Nakada S. Nishiura T. Soyano K. Tarusawa T. Mukai S.M. Kwon S. Hasegawa F. Usui M. Ueno 《Advances in Space Research (includes Cospar's Information Bulletin, Space Research Today)》2009
Cometary dust trails were first observed by IRAS; they are widely known to be the origins of meteoric showers. A new window has been opened for the study of dust trails, using ground-based observations. We succeeded in obtaining direct images of the 22P/Kopff dust trail with the Kiso 1.05-m Schmidt telescope. Following this initial success, we have continued to perform a dust trail survey at Kiso. As a result of this survey, we have detected dust trails along the orbit of six periodic comets, between February 2002 and March 2004. The optical depth of these dust trails are 10−9 to 10−8, which is consistent with IRAS measurements. In this paper, we describe the observations and data reduction procedures, and report the brief result obtained between February 2002 and March 2004. 相似文献
67.
针对全尺寸飞机结构疲劳(耐久性)试验过程中更改载荷谱情况下对全尺寸结构疲劳试验机(单机)进行耐久性评定的需求,基于耐久性分析的概率断裂力学方法和改进的裂纹萌生方法,提出了综合不同谱下耐久性试验数据集确定描述结构细节原始疲劳质量的当量初始缺陷尺寸分布的方法,给出了载荷谱变更情况下计算各应力区裂纹超越概率的损伤累加方法,从而建立了能够准确预测载荷谱变更情况下结构经济寿命的耐久性评定方法.这种方法已成功应用于某型飞机结构全尺寸试验中更改载荷谱情况的耐久性评定,有着重要的工程应用价值. 相似文献
68.
研究了空间平台发射拦截器的两体耦合动力学,以及拦截器拦截目标星的最优脉冲控制问题。平台首先与目标星形成绕飞关系,保持其发射筒轴线始终瞄准目标星。接到发射指令后,拦截器从发射筒中射出,本文采用拉格朗日第二类方程建立了发射过程平台-拦截器两体动力学模型。因为两体耦合影响,平台姿态偏转,拦截器出筒时的速度已经不能瞄准目标星。通过小型火箭发动机给其施加速度脉冲,使其进入拦截轨道,保证拦截的同时,将脉冲速度最小化以节省燃料,本文将其归结为一个非线性规划问题,采用三级优化的策略来求解。在拦截飞行时间相较于平台绕飞目标星的周期是小量的条件下,可以视绕飞平均角速度为小参数,采用正则摄动方法求出非线性规划的一阶近似解,然后以此为迭代初值,寻找最优真解。最后进行了数值仿真验证。 相似文献
69.
70.