Particle Acceleration Mechanisms

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.     

Alfvénic Electron Acceleration in Aurora Occurs in Global Alfvén Resonosphere Region

Auroral emission caused by electron precipitation (Hardy et al., 1987, J. Geophys. Res. 92, 12275–12294) is powered by magnetospheric driving processes. It is not yet fully understood how the energy transfer mechanisms are responsible for the electron precipitation. It has been proposed (Hasegawa, 1976, J. Geophys. Res. 81, 5083–5090) that Alfvén waves coming from the magnetosphere play some role in powering the aurora (Wygant et al., 2000, J. Geophys. Res. 105, 18675–18692, Keiling et al., 2003, Science 299, 383–386). Alfvén-wave-induced electron acceleration is shown to be confined in a rather narrow radial distance range of 4–5 R _E (Earth radii) and its importance, relative to other electron acceleration mechanisms, depends strongly on the magnetic disturbance level so that it represents 10% of all electron precipitation power during quiet conditions and increased to 40% during disturbed conditions. Our observations suggest that an electron Landau resonance mechanism operating in the “Alfvén resonosphere” is responsible for the energy transfer.     

遥测接收站火焰衰减计算模型及应用

火焰衰减是运载火箭遥测系统设计及地面测站布站须重点考虑的问题.以火焰衰减对遥测地面站接收信号的影响为出发点,推导了火焰夹角与测站位置及火箭俯仰角之间的数学关系式,在此基础上依据已有的火焰夹角与火焰衰减关系模型,设计了理论弹道全程中地面测站火焰衰减量的计算程序.以某型遥测设备的接收信道链路为依据,在实际任务中对火焰衰减模型进行验证,结果证实模型具有一定的准确性,并在此基础上分析火焰衰减对遥测地面站某型变频器参数设置的影响,确定了实际任务中更加合理的变频器参数.     

基于离心加速度信息的单站无源测距定位方法

针对只测向（B0）方法具有收敛速度慢、定位误差大等缺点，提出了一种利用角度及其变化率、离心加速度等信息进行单站无源测距定位的新方法。对该方法的单次测距误差进行了分析，经多次测量定位计算机仿真结果表明，该方法比只测角定位方法、角度及其变化率定位方法具有更高的定位精度和更快的收敛速度，并且具有更广的应用范围。     

The role of radial perpendicular diffusion and latitude dependent acceleration along the solar wind termination shock

A numerical model, based on Parker’s transport equation, describing the modulation of anomalous cosmic rays and containing diffusive shock acceleration is applied. The role of radial perpendicular diffusion at the solar wind termination shock, and as the dominant diffusion coefficient in the outer heliosphere, is studied, in particular the role it plays in the effectiveness of the acceleration of anomalous protons and helium when its latitude dependence is changed. It is found that the latitudinal enhancement of radial perpendicular diffusion towards the heliospheric poles and along the termination shock has a prominent effect on the acceleration of these particles. It results in a ‘break’ in the energy spectrum for anomalous protons at ∼6.0 MeV, causing the spectral index to change from E^−1.38 to E^−2.23, but for anomalous helium at ∼3.0 MeV, changing the spectral index from E^−1.38 to E^−2.30. When approaching the simulated TS, the changes in the modulated spectra as they unfold to a ‘steady’ power law shape at energies below 50 MeV are much less prominent as a function of radial distances when radial perpendicular diffusion is increased with heliolatitude.     

Distribution and variability of accelerated electrons at Mars

We investigate accelerated electrons observed by Mars Global Surveyor (MGS), using data from the Electron Reflectometer (ER) instrument. We find three different types of accelerated electron events. Current sheet events occur over regions with weak or no crustal fields, have the highest electron energy fluxes, and are likely located on draped magnetotail fields. Extended events occur over regions with moderate crustal magnetic fields, and are most often observed on closed magnetic field lines. Localized events have the lowest energy fluxes, occur in strong magnetic cusp regions, and are the most likely kind of event to be found on open magnetic field lines. Some localized events have clear signatures of field-aligned currents; these events have much higher electron fluxes, and are preferentially observed on radially oriented open magnetic field lines. Electron acceleration events, especially localized events, are similar in many ways to events observed in the terrestrial auroral zone. However, physical processes related to those found in the terrestrial cusp and/or plasmasheet could also be responsible for accelerating electrons at Mars.     

A combined turbulent combustion model in studying a lean flameout process

A modification of the Zimont turbulent combustion model is presented; the modification makes it possible to describe processes in diffusion and homogeneous flame fronts as well as to take into account the influence of different factors that cause flame destabilization. The model is based on the equation for a reaction completeness extent (completeness of combustion). The model realization to simulate the premixed combustion is described and the modification of the turbulent combustion model is applied to simulate a process of flameout downstream of the flameholder.     

基于退化模型的失效机理一致性检验方法

有效的加速试验必须保证产品的失效机理不变。针对加速退化试验(ADT)可靠性建模的特点,提出了一种基于退化模型的失效机理一致性检验方法。以基于随机过程和基于退化轨迹拟合的退化模型为例,通过加速系数的2种等效定义分别建立了模型参数与失效机理不变的内在联系,进一步推导出其参数在不同应力下须满足的关系。在合理假定检验样本服从正态分布的基础上,利用t统计量对样本的一致性进行检验。通过2个ADT实例验证了所提检验方法的合理性与可行性。     

弯曲通道模拟离心条件下的主燃级和预燃级联焰试验

冲压转子发动机是冲压发动机和燃气涡轮发动机的有机结合,其结构简单。冲压转子发动机燃烧室由于其内部受到强离心力场的作用,燃烧室火焰的稳定燃烧以及传播都会受其影响。为了得到离心力场对分级燃烧中两级联焰的影响规律,本文进行了试验研究工作。针对燃烧室在强离心条件下的燃烧特点,采用弯曲通道模拟气流的离心效应。在弯曲试验段上对预燃级和主燃级进行了联焰研究,试验在常温常压条件下进行,进口气流速度范围为10~70m/s。试验中考察了离心力、燃油分级比例以及主燃级燃油喷射初始角度对联焰的影响,试验结果初步验证了燃烧方案的可行性,为冲压转子发动机燃烧室的研究奠定了基础。     

乙醇-空气稀液雾值班火焰的大涡模拟研究

为加深对气液两相湍流燃烧现象的认知,检测火焰面模型在液雾燃烧中的适用性,本文在欧拉-拉格朗日架构下使用火焰面/反应进度变量模型(FPV)数值模拟了乙醇-空气稀液雾值班火焰。欧拉坐标系下的气相湍流场使用大涡模拟方法模拟,离散液相则使用拉格朗日颗粒轨道模型进行描述,考虑了相间质量、动量、能量交换。燃烧模型中采用碳元素定义混合物分数,在混合物分数方程源项中体现液相对燃烧模型的影响。模拟得到的气相温度分布和液相统计值均和实验数据较好吻合,验证了该燃烧模型对稀液雾扩散类型火焰的适用性。分析瞬时图发现,该稀液雾火焰的最高燃烧温度往往位于当量混合物分数附近,在出口下游20倍直径处火焰完全点着,此处上游FPV模型能给出局部点火熄火现象。蒸发作用在剪切层和点火区域较强,而液滴和火焰作用较弱,单一液滴很少被火焰包围。