Viewing radiation signatures of solar energetic particles in interplanetary space

A current serious limitation on the studies of solar energetic particle (SEP) events is that their properties in the inner heliosphere are studied only through in situ spacecraft observations. Our understanding of spatial distributions and temporal variations of SEP events has come through statistical studies of many such events over several solar cycles. In contrast, flare SEPs in the solar corona can be imaged through their radiative and collisional interactions with solar fields and particles. We suggest that the heliospheric SEPs may also interact with heliospheric particles and fields to produce signatures which can be remotely observed and imaged. A challenge with any such candidate signature is to separate it from that of flare SEPs. The optimum case for imaging high-energy (E > 100 MeV) heliospheric protons may be the emission of π⁰-decay γ-rays following proton collisions with solar wind (SW) ions. In the case of E > 1 MeV electrons, gyrosynchrotron radio emission may be the most readily detectible remote signal. In both cases we may already have observed one or two such events. Another radiative signature from nonthermal particles may be resonant transition radiation, which has likely already been observed from solar flare electrons. We discuss energetic neutrons as another possible remote signature, but we rule out γ-ray line and 0.511 MeV positron annihilation emission as observable signatures of heliospheric energetic ions. We are already acquiring global signatures of large inner-heliospheric SW density features and of heliosheath interactions between the SW and interstellar neutral ions. By finding an appropriate observable signature of remote heliospheric SEPs, we could supplement the in situ observations with global maps of energetic SEP events to provide a comprehensive view of SEP events.     

超高温度梯度定向凝固NiMnFeGa磁致形状记忆合金

利用超高温度梯度定向凝固装置制备出定向Ni51.2Mn20.0Fe13.0Ga15.8磁致形状记忆合金.沿晶体生长方向凝固组织由等轴晶逐渐过渡为柱状晶,马氏体变体取向性明显,γ相愈加细小,分布愈加均匀.Ni51.2Mn20.0-Fe13.0Ga15.8合金在加热和冷却过程中发生热致马氏体相变及逆相变,马氏体相变温度Ms＝121.3℃,Mf＝99.3℃,As＝118℃,Af＝147℃.     

俯仰轴飞行品质中频域准则的计算与模拟

简要介绍了军用飞机飞行品质MIL—STD—1797A中有关俯仰轴频域难则的要求和原由。提出了对这些难则的理论计算和模拟试验方法。并以某飞机为例，利用所提出的方法，对其飞行品质进行了计算和模拟。结果表明，所提出的计算和模拟方法是合理的。最后，讨论了驾驶员模型形式对俯仰轴飞行品质的影响。     

The Origin of Mercury’s Internal Magnetic Field

Mariner 10 measurements proved the existence of a large-scale internal magnetic field on Mercury. The observed field amplitude, however, is too weak to be compatible with typical convective planetary dynamos. The Lorentz force based on an extrapolation of Mariner 10 data to the dynamo region is 10⁻⁴ times smaller than the Coriolis force. This is at odds with the idea that planetary dynamos are thought to work in the so-called magnetostrophic regime, where Coriolis force and Lorentz force should be of comparable magnitude. Recent convective dynamo simulations reviewed here seem to resolve this caveat. We show that the available convective power indeed suffices to drive a magnetostrophic dynamo even when the heat flow though Mercury’s core–mantle boundary is subadiabatic, as suggested by thermal evolution models. Two possible causes are analyzed that could explain why the observations do not reflect a stronger internal field. First, toroidal magnetic fields can be strong but are confined to the conductive core, and second, the observations do not resolve potentially strong small-scale contributions. We review different dynamo simulations that promote either or both effects by (1) strongly driving convection, (2) assuming a particularly small inner core, or (3) assuming a very large inner core. These models still fall somewhat short of explaining the low amplitude of Mariner 10 observations, but the incorporation of an additional effect helps to reach this goal: The subadiabatic heat flow through Mercury’s core–mantle boundary may cause the outer part of the core to be stably stratified, which would largely exclude convective motions in this region. The magnetic field, which is small scale, strong, and very time dependent in the lower convective part of the core, must diffuse through the stagnant layer. Here, the electromagnetic skin effect filters out the more rapidly varying high-order contributions and mainly leaves behind the weaker and slower varying dipole and quadrupole components (Christensen in Nature 444:1056–1058, 2006). Messenger and BepiColombo data will allow us to discriminate between the various models in terms of the magnetic fields spatial structure, its degree of axisymmetry, and its secular variation.     

新型磁性液体材料的研究与探讨

磁性液体，是由固体的磁性粒子分散到载体（液体）中形成的一种胶体溶液，此种深夜既有液体的流动性，又具有磁性，是一种新型的磁性材料，本文对磁性液体的制造方法，及其存在的条件，进行了研究与探讨，并简单介绍了磁性液体的性质及其应用前景。     

三维Euler方程组隐式LU分解的高性能并行计算

许多非定常无粘流体力学问题的数值模拟都需要利用Euler方程组来进行计算,而由于在隐格式下,所选取的时间步长可以比在显格式下时大得多,所以隐格式越来越受到重视,其中隐式LU分解是最常用的方法之一。对三维Euler方程组,采用隐式LU分解进行计算时,网格点所在的各个对角阵面之间存在数据依赖关系,本文分析了采用区域分解且边界上用显格式代替隐格式进行计算的高效性,在长方体建筑物内的爆炸模拟表明,在有112个CPU的某MPP巨型机上,并行计算效率超过60%。本文还分析了计算结果与串行计算时的差异,以及利用区域重叠减小这种差异的方法,同时考虑了对处理器进行合理的逻辑组织,将计算网格映射到处理器网格,以最大限度减少通信开销的方法。文中最后以一个爆炸毁伤的例子实际说明了所述方法的可行性与高效性。     

Thermal cyclotron radiation from a hot coronal loop with helical magnetic field

The spectral and polarization properties of thermal cyclotron radio emission from a hot coronal loop with a current along the axis are computed. The magnetic field is supposed to have a component along the loop axis as well as a poloidal part due to the current, both components being of comparable magnitude. In this specific configuration a helical magnetic field is present with a remarkable minimum of its absolute value along the loop axis and a maximum at its periphery. The presence of one or two maxima of magnetic field value along the line of sight results in increasing optical thickness of the gyroresonance layers at appropriate frequencies in the microwave band and, therefore, in enhanced radio emission at those harmonics which are optically thin (for example,s=4). These cannot be observed in models with the commonly employed magnetic field configuration (longitudinal along the loop axis).We show that the frequency spectrum of thermal cyclotron radiation from a hot coronal loop with a helical magnetic field differs from that of the standards-component source (with smooth frequency characteristics and polarization corresponding toe-mode) in that plenty of fine structures (line-like features and cut-offs) are present and theo-mode is prevalent in some frequency intervals. The enhanced radio emission at high harmonics and the complicated form of frequency spectrum in the model considered imply that some microwave sources, which are poorly explained in traditional models of solar active regions, may be associated with helical magnetic fields in hot coronal loops. Computations allow one to indicate spectral and polarizational peculiarities of local sources testifying to the presence of a helical magnetic field.     

基于CompactPCI总线的红外目标跟踪系统

红外目标跟踪方法的理论研究较多,而通用的实时跟踪系统较少。给出了具有CompactPCI总线、并行分布式结构的系统方案,核心是基于标准总线的实时系统,上位机实现卡尔曼预测,DSP并行完成频域转换与相关,CPLD实现总线接口控制。所实现的系统具有运算能力强、通信带宽大、可扩展性和通用性强的特点,实用表明了它的可行性。     

基于CFD/CSD耦合的叶轮机叶片失速颤振计算

为了研究叶轮机叶片的失速颤振特性,发展了一种计算流体力学与计算结构力学(CFD/CSD)时域耦合方法。该方法通过每一物理时刻CFD和CSD的循环迭代实现了耦合计算。在CFD分析中,采用鲁棒性较好的空间离散格式AUSM+-UP,并基于延迟脱体涡模型(DDES)模拟了带分离流动。在结构分析中,通过模态法构建了旋转叶片动力学方程并运用杂交多步方法进行求解。以孤立转子Rotor37为例,计算了不同工况下流场总体与细节参数,与实验结果的对比验证了CFD算法的精度。对某转子叶片进行了颤振特性研究,计算所得的广义位移时间响应曲线表明该叶片在近失速工况下会发生失速颤振,其表现形式为一阶弯曲模态发散且各阶模态之间不耦合。分析表明,流场不稳定和非定常效应是引起失速颤振的关键因素,同时折合频率的降低也会导致原本气动弹性稳定的叶片发生失速颤振。