磁阻尼对火星探测器降落过程的动力学效应

火星稀薄的大气使得探测器再入火星时难以获得足够的减速阻力,为此,文章提出利用磁阻尼增加阻力的概念。高速再入的探测器与火星大气剧烈摩擦产生等离子体,利用探测器上的磁偶极场将等离子体捕获,同时在火星大气中形成一个“磁泡”区域并跟随探测器。由“磁泡”束缚的等离子体与来流的中性气体发生碰撞获得动量,又通过磁场作用将动量传递给探测器,从而使探测器获得一定的减速阻力。在磁阻尼的作用下,在同样的开伞高度探测器速度可降至更低,而低速开伞又可提高阻力伞打开的可靠性。因此,磁阻尼不仅可加快降低再入速度,而且还有助于提高探测器着陆火星的安全性。     

Properties of Interplanetary Coronal Mass Ejections

Interplanetary coronal mass ejections (ICMEs) originating from closed field regions on the Sun are the most energetic phenomenon in the heliosphere. They cause intense geomagnetic storms and drive fast mode shocks that accelerate charged particles. ICMEs are the interplanetary manifestations of CMEs typically remote-sensed by coronagraphs. This paper summarizes the observational properties of ICMEs with reference to the ordinary solar wind and the progenitor CMEs.     

航磁补偿技术及补偿质量的评价方法

航磁补偿的目的是要消除飞机平台引入的干扰磁场,对于高精度航空磁探来说,磁补偿质量直接制约了探测效果。文章按照航磁补偿的执行步骤进行了飞机平台磁干扰建模、模型参数求解方法、补偿飞行方案。另外,为了对补偿飞行的质量进行有效控制,采用量化指标对磁补偿效果进行评价,判定补偿效果的优劣。最后,基于 MFC软件平台开发了航磁补偿系数求解及补偿质量评价软件。     

Solar flare forecasting model supported with artificial neural network techniques

Nowadays operational models for solar activity forecasting are still based on the statistical relationship between solar activity and solar magnetic field evolution. In order to set up this relationship, many parameters have been proposed to be the measures. Conventional measures are based on the sunspot group classification which provides limited information from sunspots. For this reason, new measures based on solar magnetic field observations are proposed and a solar flare forecasting model supported with an artificial neural network is introduced. This model is equivalent to a person with a long period of solar flare forecasting experience.     

The evolution of mirror type magnetic fluctuations in the magnetosheath based on multipoint observations

Two orbits were selected in January–February 2006 when the separation between the Cluster spacecraft was large and mirror type magnetic field fluctuations were observed by all spacecraft in different regions of the terrestrial magnetosheath. Minimum variance analysis was applied to find the mirror type fluctuations, and the amplitude of the fluctuations was determined individually. Mirror mode structures are moving along the streamlines frozen in the plasma. A model was developed for the calculation of plasma flowtime from the bow shock to the observation point. The growth rate of the field strength perturbations was estimated by comparing the amplitudes of fluctuations observed simultaneously at distant locations (∼10,000 km) based on the assumption that δB ∼ exp(γt). The obtained growth rate values were about an order of magnitude smaller than those provided by linear models and they decreased in the inner regions of the magnetosheath, indicating some saturation in the growth of the waves when proceeding towards the magnetopause. The results of these two case studies suggest that mirror type fluctuations originate from the compression region downstream of the quasi-perpendicular bow shock, and the growth of the fluctuations cannot be described by linear approximations.     

基于低频磁信标的全天时自主定位方法

由于以GPS、北斗为代表的GNSS信号容易受到天气和位置的影响,单纯使用GNSS在某些条件下会有较大的定位误差,甚至无法提供定位服务。针对这种情况研究了基于低频磁信标的自主定位方法,分析了电磁学中的毕奥-萨伐尔定律等原理,建立了基于低频磁信标定位的系统模型,给出了分离式双信标定位方法。通过实验分析了信标安装的误差特性,最后通过仿真和实际实验验证了该定位方法的有效性,对于室内机器人导航、地下生物探索、水下跟踪定位等单独采用GNSS定位影响较大的场景下的自主定位与导航具有重要的工程应用价值。     

飞机风挡玻璃在电磁脉冲环境下的屏蔽效能测试

飞机作为高电子集成度平台,在飞行过程中,必将面临着复杂的电磁环境,研究复杂电磁环境,尤其是电磁脉冲环境对飞机性能的影响。设计了一种基于试验件结构的电磁脉冲环境屏蔽效能测试方法,以飞机电磁防护中的主要薄弱环节风挡玻璃的屏蔽为例,分别从时域、频域和能域的角度出发,评估不同姿态下的风挡玻璃屏蔽效能。经屏蔽效能试验验证,测试方法可行、有效,风挡玻璃在水平和垂直方向的屏蔽效能相差5dB,说明结构件的形状对屏蔽效能有较大影响。     

Materials selection for electronic enclosures in space environment considering electromagnetic interference effect

Using low power electronic devices for space applications to reduce the mass and energy consumption has lead to electromagnetic interference (EMI) problem. Electronic enclosures are used to shield electronic devices against EMI. In the past, electromagnetic shielding has been mainly the only criteria considered in electronic enclosure design. However, there are several structural and thermal requirements for selection of shielding materials which should also be taken into account. In this research work, three quantitative materials selection methods, i.e. Digital Logic (DL), Modified Digital Logic (MDL), and Z-transformation, are employed to select the best material from among a list of candidate materials. Composite and metallic electronic enclosures are explored and the best material is selected. Z-transformation method is applicable to both of the considered case studies while DL and MDL can only be used for solving one of them. Z-transformation method ranks aluminum as the first choice among various metallic materials. The wide range of Z-transformation application and its practical results confirm the superiority of Z-transformation method over DL and MDL methods.     

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.