On the Origin of the Strong Intermittent Nature of Interplanetary Magnetic Field

We briefly discuss the strong intermittent nature of the interplanetary magnetic field, observing that similarity between its statistical properties and the passive scalar ones exists, and may arise from different dynamical mechanisms.     

PIP 法制备SiBN 纤维增强氮化物陶瓷基复合材料Ⅰ———纤维和先驱体性能分析

利用先驱体聚合物浸渍-裂解(PIP)技术制备SiBN纤维增强氮化物陶瓷基复合材料,对SiBN纤维、聚硅硼氮烷有机先驱体裂解以及SiBN纤维增强氮化物陶瓷基复合材料性能进行了分析。研究表明:聚硅硼氮烷先驱体在氨气气氛下裂解得到的陶瓷产物碳含量较低,其裂解产物介电常数在3.0左右,介电损耗小于0.01;SiBN纤维中C和O元素含量均较高,碳的存在对材料介电性能影响明显;制备的氮化物陶瓷基复合材料弯曲强度为88.52 MPa,弹性模量为20.03 GPa。     

石墨烯基吸波材料研究新进展

吸波材料的性能是影响雷达隐身的关键因素,其研究对军用和民用都具有非常重要的意义。石墨烯由于其独特的吸波性能,成为吸波材料研究的一大热点。本文综述了石墨烯/铁氧体、石墨烯/金属微粉、石墨烯/磁性金属、石墨烯/导电聚合物和石墨烯/磁性材料/导电聚合物等复合吸波材料在吸波领域的最新研究应用现状,并展望了吸波材料未来发展趋势。     

SiC尺寸和含量对MB2/SiC复合材料超塑性的影响

在应变速率为 2 .0 8× 10 - 3 s- 1 ～ 5 .2 1× 10 - 1 s- 1 的范围内 ,测试了四种镁基复合材料的超塑性。结果表明 ,颗粒百分含量增加 ,复合材料的延伸率和应变速率敏感性指数增加 ,颗粒尺寸增大则导致复合材料超塑性能的下降。     

Synthesis of Iron-containing Carbon Microparticles from Deoiled Asphalt and Ferrocene

The deoiled asphalt as the carbon source and the ferrocene as the metal source and the catalyst precursor were chosen to synthesize iron-containing carbon microparticles through co-carbonization at the temperature of about 450℃ for 3 h. The resulting products were treated at 2 000 ℃ for 2 h. All samples were examined by high resolution transmission electron microscopy （HRTEM） and X-ray diffraction （XRD）. The results show that the iron particles in the heat-treated material are completely coated by carbon. In addition to the fully filled carbon microparticles as well as hollow carbon ones, also form carbon fibers with hollow centers. The formation mechanism of the as-prepared products was discussed briefly.     

VXI数字示波器仪器驱动器与软面板设计

简述了５００ＭＨｚ四通道数字存示波器ＨＰＥ１４２６Ａ的工作原理，详细介绍了在ＬａｂＷｉｎｄｏｗｓ／ＣＶＩ编程环境下，满足ＶＸＩ即插即用规范的仪器驱动器和软面板的设计步骤，方法与编程技术。     

基于MATLAB下的磁性测量新方法

在简单介绍磁性测量冲击法基本原理的基础上,提出了一种将多元回归分析应用于磁性测量中的新方法。着重讲述了如何实现基于多元回归分析法下的磁性测量新方法,借助于MATLAB语言编辑可实现多元回归算法及磁测新方法的多个可嵌套调用的GUI界面。实践证明,使用MATLAB可实现磁性测量新方法,该方法大大缩短了测量周期,所编辑的GUI界面充分利用了MATLAB函数库,可快速精确的处理磁测数据,建立回归模型,保存并显示计算结果,且操作方便。     

Solar Wind Control of the Magnetospheric and Auroral Dynamics

A dependence of the polar cap magnetic flux on the interplanetary magnetic field and on the solar wind dynamic pressure is studied. The model calculations of the polar cap and auroral oval magnetic fluxes at the ionospheric level are presented. The obtained functions are based on the paraboloid magnetospheric model calculations. The scaling law for the polar cap diameter changing for different subsolar distances is demonstrated. Quiet conditions are used to compare theoretical results with the UV images of the Earth’s polar region obtained onboard the Polar and IMAGE spacecrafts. The model calculations enable finding not only the average polar cap magnetic flux but also the extreme values of the polar cap and auroral oval magnetic fluxes. These values can be attained in the course of the severe magnetic storm. Spectacular aurora often can be seen at midlatitude during severe magnetic storm. In particularly, the Bastille Day storm of July 15–16, 2000, was a severe magnetic storm when auroral displays were reported at midlatitudes. Enhancement of global magnetospheric current systems (ring current and tail current) and corresponding reconstruction of the magnetospheric structure is a reason for the equatorward displacement of the auroral zone. But at the start of the studied event the contracted polar cap and auroral oval were observed. In this case, the sudden solar wind pressure pulse was associated with a simultaneous northward IMF turning. Such IMF and solar wind pressure behavior is a cause of the observed aurora dynamics.     

The solar wind control of the equatorial ionosphere dynamics during geomagnetic storms

The interplanetary magnetic field, geomagnetic variations, virtual ionosphere height h′F, and the critical frequency foF2 data during the geomagnetic storms are studied to demonstrate relationships between these phenomena. We study 5-min ionospheric variations using the first Western Pacific Ionosphere Campaign (1998–1999) observations, 5-min interplanetary magnetic field (IMF) and 5-min auroral electrojets data during a moderate geomagnetic storm. These data allowed us to demonstrate that the auroral and the equatorial ionospheric phenomena are developed practically simultaneously. Hourly average of the ionospheric foF2 and h′F variations at near equatorial stations during a similar storm show the same behavior. We suppose this is due to interaction between electric fields of the auroral and the equatorial ionosphere during geomagnetic storms. It is shown that the low-latitude ionosphere dynamics during these moderate storms was defined by the southward direction of the B_z-component of the interplanetary magnetic field. A southward IMF produces the Region I and Region II field-aligned currents (FAC) and polar electrojet current systems. We assume that the short-term ionospheric variations during geomagnetic storms can be explained mainly by the electric field of the FAC. The electric fields of the field-aligned currents can penetrate throughout the mid-latitude ionosphere to the equator and may serve as a coupling agent between the auroral and the equatorial ionosphere.     

Mode selection mechanism and magnetic diffusivity in a non-axisymmetric solar dynamo model

The generation of solar non-axisymmetric magnetic fields is studied based on a linear α²–Ω dynamo model in a rotating spherical frame. The model consists of a solar-like differential rotation, a magnetic diffusivity varied with depth, and three types of α-effects with different locations, i.e. the tachocline, the whole convective zone and the sub-surface. Some comparisons of the critical α-values of axisymmetric (m = 0) and longitude-dependent modes (m = 1,2,3) are presented to show the roles of the magnetic diffusivity in the problem of modes selection. With the changing of diffusivity intensity for the given solar differential rotation system, the dominant mode possibly changes likewise and the stronger the diffusivity is, the easier the non-axisymmetric modes are excited. The influence of the diffusivity and differential rotation on the configurations of the dominant modes are also presented.