月球巡视器太阳电池阵电性能仿真模型

建立精准的太阳电池阵电性能仿真模型,可为月球巡视器电源设计方案以及在轨任务规划的验证和优化提供保障。文章依据巡视器设计及月面环境的特殊性,建立了考虑遮挡、月尘等因素的太阳电池阵电性能仿真模型。该模型包括布阵文件编写及导入模块,光强、温度、老化影响计算模块,月尘影响计算模块,以及部分遮挡影响计算模块。对仿真模型进行了仿真分析,并将仿真结果与硬件实测值进行比较,结果表明:两者之间的误差可控制在5%以内,证明了模型的正确性和精准度。     

NbV 替代 NiMo 生产球铁钆辊

本文采用正交试验方法寻找Ｎｂ、Ｖ合金元素与变质剂的最佳组合以获得性能良好的球铁轧辊材料，比较ＮｂＶ球铁与ＮｉＭｏ球铁的铸造性能、常规力学性能及断裂韧性，结果表明，ＮｂＶ球铁不亚于ＮｉＭｏ球铁，可替代ＮｉＭｏ球铁生产轧辊。     

Field emission characteristics of gold dust grains

The space plasma environment usually contains charged dust grains. The grain charge is an important parameter determining its migration through the space, coagulation, formation of dust clouds and so on. The knowledge of its charge is thus one of the basic information we want to know. There are several emission processes leading to both positive and negative charges, among others photoemission, all kinds of secondary emissions, field emissions, etc. The present study is focused on a laboratory simulation of emissions caused by impacts by energetic ions. Our experiment is based on the Paul trap which gives us an opportunity to catch a single dust grain for several days inside the vacuum vessel and exposed it by electron/ion beams. This experimental approach allows us to separate an individual charging process. We have chosen spherically shaped gold grains and discussed the processes leading to the limitation of the grain charge. We suggested that the implantation of charging ions leads to deformations of the grain surface. The deformations enhance the local electric field strength that becomes sufficient for the field ionization.     

The Cool Interstellar Medium

Infrared spectroscopy and photometry with ISO covering most of the emission range of the interstellar medium has led to important progress in the understanding of the physics and chemistry of the gas, the nature and evolution of the dust grains and also the coupling between the gas and the grains. We review here the ISO results on the cool and low-excitation regions of the interstellar medium, where T _gas≲ 500 K, n _H∼ 100–10⁵ cm⁻³ and the electron density is a few 10⁻⁴. JEL codes: D24, L60, 047 Based on observations with ISO, an ESA project with instruments funded by ESA Member States (especially the PI countries: France, Germany, The Netherlands, and the United Kingdom), and with the participation of ISAS and NASA.     

An ISO View on Interstellar and Cometary Ice Chemistry

The ISO-SWS instrument offering a large wavelength coverage and a resolution well adapted to the solid phase has changed our knowledge of the physical-chemical properties of ices in space. The discovery of many new ice features was reported and the comparison with dedicated laboratory experiments allowed the determination of more accurate abundances of major ice components. The presence of CO₂ ice has recently been confirmed with the SWS (Short Wavelength Spectrometer) as a dominant ice component of interstellar grain mantles. The bending mode of CO₂ ice shows a particular triple-peak structure which provides first evidence for extensive ice segregation in the line-of-sight toward massive protostars. A comparison of interstellar and cometary ices using recent ISO data and ground-based measurements has revealed important similarities but also indicated that comets contain, beside pristine interstellar material, admixtures of processed material. The investigation of molecules in interstellar clouds is essential to reveal the link between dust in the interstellar medium and in the Solar System. This revised version was published online in June 2006 with corrections to the Cover Date.     

Interplanetary medium – A dusty plasma

The average mass of dust per volume in space equals that of the solar wind so that the interplanetary medium should provide an obvious region to study dust plasma interactions. While dust collective behavior is typically not observed in the interplanetary medium, the dust component rather consists of isolated grains screened by and interacting with the plasma. Space measurements have revealed several phenomena possibly resulting from dust plasma interactions, but most of the dust plasma interactions are at present not quantified. Examples are the production of neutrals and pick-up ions from the dust, dust impact generated field variations at spacecraft and magnetic field variations possibly caused by solar wind interacting with dust trails. Since dust particles carry a surface charge, they are exposed to the Lorentz force in the interplanetary magnetic field and for grains of sub-micrometer sizes acceleration can be substantial.     

韧性材料的冲蚀损伤数值仿真综述

砂尘造成韧性材料的冲蚀损伤现象和损伤演化规律是冲蚀机理研究的重要内容，基于相应冲蚀试验和数值仿真的分析 方法是揭示冲蚀机理的重要手段。回顾了砂尘冲蚀损伤研究的缘起和发展经历，在介绍砂尘冲蚀损伤机理的基础上，总结了当前 数值仿真研究的3种主流方法：有限元方法、无网格方法和计算流体动力学方法。从数值仿真角度针对砂尘对韧性材料造成的破 坏模式、砂尘冲击姿态、砂尘冲击速度和形状、砂尘破碎对材料去除机制的影响等4个方面综述了影响冲蚀损伤机理的主要因素 和当前研究进展。砂尘对韧性材料造成的破坏模式通常分为材料凹陷、滑动、犁削、切削等4种不同机制；砂尘的冲击姿态决定了 材料的损伤模式；砂尘的冲击速度和砂尘的形状决定了材料的损伤严重程度；砂尘破碎现象对材料的去除机制有一定影响。     

上海大中型钢铁企业营销管理研究

总结了 2 0 0 0年～ 2 0 0 1年对上海大中型钢铁企业的营销系统所作的市场调查 ,结合我国钢铁市场的竞争态势、钢铁市场基本情况等钢铁企业营销环境变量 ,对上海大中型钢铁企业的营销管理现状进行了实证分析和诊断。     

方向舵纸基蜂窝芯零件夹持方法研究

采用基于磁场和摩擦吸附原理的纸基蜂窝芯零件夹持方法,以某型号飞机方向舵蜂窝芯零件为对象,研究了区域划分单元的形式以及在确定的铣削条件下Z向变形与蜂窝芯高度的关系,利用实验测试和有限元方法对专用装夹平台进行了设计分析,确定了夹持点的位置以及夹持点的反力,最后给出了设计方案。     

The Coma of Comet 9P/Tempel 1

As comet 9P/Tempel 1 approaches the Sun in 2004–2005, a temporary atmosphere, or “coma,” will form, composed of molecules and dust expelled from the nucleus as its component icy volatiles sublimate. Driven mainly by water ice sublimation at surface temperatures T > 200 K, this coma is a gravitationally unbound atmosphere in free adiabatic expansion. Near the nucleus (≤ 10² km), it is in collisional equilibrium, at larger distances (≥10⁴ km) it is in free molecular flow. Ultimately the coma components are swept into the comet’s plasma and dust tails or simply dissipate into interplanetary space. Clues to the nature of the cometary nucleus are contained in the chemistry and physics of the coma, as well as with its variability with time, orbital position, and heliocentric distance. The DI instrument payload includes CCD cameras with broadband filters covering the optical spectrum, allowing for sensitive measurement of dust in the comet’s coma, and a number of narrowband filters for studying the spatial distribution of several gas species. DI also carries the first near-infrared spectrometer to a comet flyby since the VEGA mission to Halley in 1986. This spectrograph will allow detection of gas emission lines from the coma in unprecedented detail. Here we discuss the current state of understanding of the 9P/Tempel 1 coma, our expectations for the measurements DI will obtain, and the predicted hazards that the coma presents for the spacecraft. An erratum to this article is available at .