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℃.     

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.     

体表电位标测系统中关键技术——心电信号数据高速采集

心电信号的数据采集是体表标测系统中关键技术之一。文中提出了128通道高性能体表标测系统中心电信号数据采集的VxD算法，在Wind9x系统下利用VxD技术、锁定内存和临界资源互斥访问算法相结合，实现了心电数据高速实时采集。该软件充分利用了硬件的等待时间，具有实时性高，运行速度快占内存少的特点。该软件在VtoolsD开发平台上用VisualC＋＋开发。     

GaInP2外延膜中施主—受主对复合发光带的能量关量

通过变温与变激发强度的近红外光致发光研究了用ＭＯＣＶＤ方法、生长在ＧａＡｓ衬底上的Ｇａ０．５Ｉｎ０．５Ｐ（ＧａＩｎＰ２）外延薄膜的１．１７ｅＶ发射带的发光特性。１．１７ｅＶ发光带性质与０．９９ｅＶ及０．８５ｅＶ发光带的性质有着明显的差别。１．１７ｅＶ发光带的机理可用施主－受主对的复合发光来解释，其中施主－受主对系白处在Ｇａ格位上的Ｓｉ（ＳｉＧａ）及其最邻近的Ｇａ空位（ＶＧａ）所组成，记作ＳｉＧａ－ＶＧａ。考虑到ＧａＩｎＰ２中存在着很强的电子－格子耦合作用及其Ⅲ族子格子为部分有序，所以在施主－受主对复合发光中应计及Ｆｒａｎｃｋ－Ｃｏｎｄｏｎ位移△ＦＣ及该对在等效的部分有序势场中的相互作用能Ｅｓ（ＤＡＰ）。Ｘ—射线衍射实验表明，部分有序结构相当于成分调制，因而可用Ｋｒｏｎｉｇ－Ｐｅｎｎｅｙ模型来计算Ｅｓ（ＤＡＰ）值。这样，我们就导出了施主－受主对复合发光的新的能量表示式。     

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。     

发动机某型号节流圈的切削加工

某型号节流圈,其结构特点是壁薄,壁厚仅2.5mm,轴向尺寸小,精度高,刚性差;加工难点为装夹时容易变形,尺寸精度难以保证。通过设计、制作专用夹具,优化加工参数,解决了这一加工难题。这样既保证了产品质量,降低了加工难度又显著提高了生产效率。     

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.     

基于正弦基础激励的航天器结构模型修正方法

正弦振动试验是航天器系统级和单机产品需要开展的常规试验,充分利用工程中积累的正弦试验数据进行结构模型修正具有重要的工程意义。文章首先介绍了基础激励下结构模型修正方法,通过矩阵分块、待修正参数归一化、参与修正的频率点选择等步骤,推导出基于基础激励的模型修正公式;然后对国际通用算例GARTEUR桁架结构的有限元模型进行修正,分析修正后模型在修正频段内和修正频段外计算所得模态频率,验证修正后模型对模态频率的复现和预示能力,通过对比试验模型、分析模型和修正后模型中4个典型节点的响应曲线,检验修正后模型精度。结果表明:修正后模型的模态频率和响应曲线均与试验模型趋于一致,证实了该修正方法对GARTEUR结构修正的有效性。