铝颗粒云燃烧研究进展

为探究铝颗粒云燃烧特性,把握其研究进展,并为后续研究工作提供参考,本文首先简述了铝颗粒点火、燃烧过程,总结了铝颗粒燃烧机理;其次,综述了铝颗粒云燃烧的实验、理论和模拟研究进展,从不同维度分析了影响颗粒云火焰速度的关键参数,并提出颗粒云燃烧的研究方向,包括提升颗粒云燃烧实验颗粒分散均匀性与表征精度、降低火焰传播速度等实验结果散差、改善颗粒云燃烧理论预测模型精度及构建实用的颗粒云燃烧模拟CFD模型。     

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。     

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。     

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 .     

太阳电池月尘遮蔽模型分析及试验研究

扬起的月尘颗粒沉积在月球探测器的太阳电池表面,可导致其性能下降。文章基于层叠遮挡理论,建立了一种月尘遮蔽光线透射的理论模型,利用该模型开展了模拟月尘颗粒形状与粒径对遮蔽效果影响的分析和计算,并与NASA的同类模型进行了对比分析。分析结果显示:2种模型给出的相对透过率随沉积月尘面密度的变化趋势相同,均呈指数型衰减关系;在随月尘形状、粒径、透过率的变化方面,2种模型存在差异。利用月尘沉积与吸附试验装置实施了模拟月尘沉积试验,验证了所建立模型的正确性,其预测准确度优于NASA模型。     

聚碳硅烷粉尘火灾爆炸特性参数测试及安全性分析

为确保聚碳硅烷粉尘作业安全,避免发生火灾爆炸事故,本文按照相应国家测试标准,采用标准测试仪器,对聚碳硅烷粉尘的最小点火能、最低着火温度、爆炸下限浓度3个火灾爆炸特性参数进行了测试。结果表明:聚碳硅烷粉尘最小点火能1. 5 mJEmin2 mJ,最低着火温度MIT=320℃,爆炸下限浓度12 g/m3Cmin13 g/m3。结合常见涉爆粉尘火灾爆炸特性参数范围比对分析,结果表明:聚碳硅烷粉尘最低着火温度和最小点火能均较低、爆炸下限浓度也小,说明该粉尘极易被引爆,安全风险较高。