用于JL—ZKR燃烧器的牛角锥体旋风除尘器的设计

这种除尘器是为了满足JL—ZKR燃烧器的需要而设计的。它的体积小,造价低。构造简单,使用方便。它的除尘效率可达80％左右。但其阻力比普通除尘器略高。     

Sunyaev-Zel'dovich effect and the dust emission in the galaxy clusters

It is shown that if the dust is present in the hot intergalactic gas, the galaxy cluster must be very bright source of far infrared emission. This emission can be observed by modern IR astronomy methods. At the same time, taking realistic assumptions about the intergalactic dust nature, it is impossible to explain negative results of the attempts made at observational detecting the Sunyaev-Zel'dovich effect in the centimeter wavelength region as the compensation of the expected decrements by the dust grains emission.     

煤粉热解的激波管测试法及其控制系统

本文主要介绍煤粉热解的激波管测试法及其系统的原理和软件、硬件系统组成。本系统的特点是控制与测试系统既相互独立又有数据传递。特别是控制系统采用模块化的设计方法,集控制与管理为一体。硬件布局合理可靠、软件丰富,且各软件模块间相互调用,克服了机器内存不够的缺陷。还具有手动操作和自动控制两种功能,可广泛应用于其它小型风洞及其它机械设备的控制。     

激波对管内壁堆积粉尘作用的实验研究

用水平激波管研究了激波对管内壁堆积粉尘的抛撒效应。试验粉尘为玉米粉(平均直径5μm),采用 YA-16高速摄影机观察了激波特性和粉尘云的发展。结果表明,在激波扫过堆积粉尘与粉尘被扬起存在一定时间滞后,粉尘云的高度也是有限的。     

行星际尘粒中锂同位素丰度与太阳星云演化的关系

1引言构成太阳系的大多数元素都经历过恒星演化过程，但3种轻元素Li，Be和B极为脆弱，在绝大多数恒星内部的高温、高密度和剧烈变动的条件下，很快就会分解．太阳系的早期阶段，太阳星云可能是由大爆炸产生的1H、2H、3He、4He和7Li及附近超新星爆发产生的C、N、O等构成[1]，而6Li、Be、B是以后由宇宙射线粒子轰击附近星际和行星际的C、N、O等的核产生[2]．因为Li的同位素丰度的一部分是由大爆炸生成，一部分是由宇宙射线与星际介质核反应产生，因此它的丰度与宇宙射线暴露时间有关．1991年，文献间报导过在行星际尘粒中发现Li、Be和…     

砂尘环境试验设备中颗粒浓度场的实验研究

利用中科院寒旱所沙漠研究所室内风沙环境风洞,采用激光粒子成像技术对砂尘环境试验设备中含砂气固两相射流在距喷嘴不同截面中心位置的颗粒浓度场进行了测量和分析研究,并与拍摄的颗粒空间分布数码照片进行对比.实验结果表明在距气固喷嘴约1?m处的截面上,砂粒颗粒还没有扩散到整个空间内,轴线附近的粒子较多,而且大粒子多数处于下部区域,只有在距喷嘴下游约3?m处粒子才基本扩散均匀,从而可确定砂尘环境试验中试件的安放位置.结论认为砂尘试验设备的加砂段应保持在3?m左右,这样才能满足国军标要求,从而为我国自行研制大型砂尘环境试验设备,确定加砂/尘方法、参数、加料和试验段尺寸等提供了依据.     

彗星环境中尘埃等离子体的电荷涨落和静电波动

本文分析了尘埃等离子体中尘埃颗粒的带电过程，给出了一套自洽的工流体方程组．运用这组方程研究了尘埃电荷的起伏涨落，得到了非磁化均匀尘埃等离子体中静电波动的色散关系．针对彗星空间环境中尘埃等离子体的特点，讨论了尘埃电荷的涨落对各种静电波动的影响．     

聚碳硅烷纤维的不熔化处理研究(Ⅱ)─-放大工艺的研究

采用熔融纺丝法纺出连续PCS纤维束,研究了升温制度、纤维装填量以及过热现象等因素对PCS纤维不熔化结果的影响,探讨了不熔化工艺的优化。结果表明,低温段慢速升温,中温段延长保温时间,高温段进一步强化的升温制度是比较合理的。纤维装填质量及密度增大到一定程度后,会因散热不利而引起急剧高温,导致纤维的熔并。急剧放热引起纤维结构的变化较大,而且内部纤维与表层纤维的反应程度不同。     

空间微小碎片对光学玻璃的污染效应研究

航天器在轨服役期间会遭受到大量空间微小碎片撞击作用。这些微陨石和空间微小碎片可能在光学玻璃表面碰撞产生陷坑,也可能吸附在航天器光学玻璃表面造成污染。文章介绍了采用静电式粉尘加速器使微米级铝粉末低速撞击K8光学玻璃,在玻璃表面吸附大量的粉尘粒子。研究结果表明,被铝粒子污染的光学玻璃透过率明显下降。透过率下降与污染程度成比例。对光学玻璃表面单个粒子陷坑计算分析表明,粒子吸附在玻璃表面时,比粒子陷入一定深度造成的光线衰减更大。     

MIDAS – The Micro-Imaging Dust Analysis System for the Rosetta Mission

The International Rosetta Mission is set for a rendezvous with Comet 67 P/Churyumov-Gerasimenko in 2014. On its 10 year journey to the comet, the spacecraft will also perform a fly-by of the two asteroids Stein and Lutetia in 2008 and 2010, respectively. The mission goal is to study the origin of comets, the relationship between cometary and interstellar material and its implications with regard to the origin of the Solar System. Measurements will be performed that shed light into the development of cometary activity and the processes in the surface layer of the nucleus and the inner coma. The Micro-Imaging Dust Analysis System (MIDAS) instrument is an essential element of Rosetta’s scientific payload. It will provide 3D images and statistical parameters of pristine cometary particles in the nm-μm range from Comet 67P/Churyumov-Gerasimenko. According to cometary dust models and experience gained from the Giotto and Vega missions to 1P/Halley, there appears to be an abundance of particles in this size range, which also covers the building blocks of pristine interplanetary dust particles. The dust collector of MIDAS will point at the comet and collect particles drifting outwards from the nucleus surface. MIDAS is based on an Atomic Force Microscope (AFM), a type of scanning microprobe able to image small structures in 3D. AFM images provide morphological and statistical information on the dust population, including texture, shape, size and flux. Although the AFM uses proven laboratory technology, MIDAS is its first such application in space. This paper describes the scientific objectives and background, the technical implementation and the capabilities of MIDAS as they stand after the commissioning of the flight instrument, and the implications for cometary measurements.