月球粉尘的研究现状

随着我国探月工程的开展,面临着月球粉尘危害性的问题,急需开展月球粉尘的研究。文章在调研的基础上,阐述了目前国外在月球粉尘方面的研究现状,主要是美国"阿波罗"计划中对月尘的特性、危害性、探测和防护方面的研究。     

电帘除尘技术的研究现状

微尘作为影响探月工程和火星计划成败的一个因素,已经越来越多地引起人们的重视。而电帘除尘技术作为月球和火星探测有效的除尘技术之一,也得到广泛的关注。文章在调研相关文献的基础上,阐述了目前国外电帘除尘技术的研究现状,提出了开展研究工作的建议,对发展我国电帘除尘技术具有一定的参考意义。     

基于压缩感知的多基地无源雷达成像算法

由于成像场景可稀疏表示（场景中仅有少数强散射点）,针对外辐射源信号波长长,带宽窄的特点,本文提出了基于压缩感知的多发单收无源雷达成像算法,该算法由符合图像统计特性的先验信息构造合理的傅里叶基矩阵,利用lp范数法将带约束条件强散射点增强问题转换为最优化问题,并通过迭代算法快速获得最优解。实验仿真结果表明小转角情况下,本文算法无需充足站点数目,并且能获得较好成像效果。
     

The dust content of clusters of galaxies

We have statistically investigated the infrared luminosity of clusters of galaxies in comparison with the known tracers of the cluster mass like the X-ray luminosity and the cluster richness (e.g. the number of member galaxies). Our results show that there is a clear positive correlation of the infrared luminosity with the cluster mass. Quantitatively speaking, the infrared luminosity is on average 20 times higher than the X-ray luminosity. Moreover, the infrared luminosity increases with the redshift. This probably shows that a major part of this infrared luminosity is due to star formation in the member galaxies. Another possible contribution would be the thermal emission from dust particles in the diffuse intracluster medium. However our method does not allow us to infer conclusions about this second hypothesis. Depending on their size and abundance, such particles would contribute to the infrared luminosity of galaxy cluster and have an impact on the cooling function of the baryons and thus on the formation of the large scale structures. This is an important cosmological question which still remains open.     

赤泥堆起尘风洞实验研究

通过对不同粒径、不同湿度的赤泥起尘风速及起尘强度的风洞实验发现,对各种湿度的赤泥,都存在一临界粒径。当赤泥粒径小于该值时,起尘风速随粒径的减小而增大,而当粒径大于该值时,起尘风速随粒径的增大而增大。临界粒径大约为0.2mm,随湿度略有变化。临界粒径对应的起尘风速最小,它随湿度的增大而升高,其变化范围为2.5～3.0m/5,对应的起动摩擦速度介于0.17～0.20m/s。此外,当粒径小于0.1mm时,起尘风速随湿度的增大而减小,而当粒径大于0.2mm 以后,起尘风速随湿度的增大而增大。起尘强度实验表明,风速一定且大于4.7m/s,湿度小于15%时,起尘强度随湿度增大而减小,湿度大于15%时,起尘强度随湿度变化甚微。风速小于4.7m/s时,起尘强度基本不随湿度而变。湿度一定时,起尘强度随风速的增大而增大。文章还讨论了模拟实验的相似准则和定量换算问题。     

Dust Environment Modelling of Comet 67P/Churyumov-Gerasimenko

Dust is an important constituent of cometary emission; its analysis is one of the major objectives of ESA’s Rosetta mission to comet 67P/Churyumov-Gerasimenko (C–G). Several instruments aboard Rosetta are dedicated to studying various aspects of dust in the cometary coma, all of which require a certain level of exposure to dust to achieve their goals. At the same time, impacts of dust particles can constitute a hazard to the spacecraft. To conciliate the demands of dust collection instruments and spacecraft safety, it is desirable to assess the dust environment in the coma even before the arrival of Rosetta. We describe the present status of modelling the dust coma of 67P/C–G and predict the speed and flux of dust in the coma, the dust fluence on a spacecraft along sample trajectories, and the radiation environment in the coma. The model will need to be refined when more details of the coma are revealed by observations. An overview of astronomical observations of 67P/C–G is given, because model parameters are derived from this data if possible. For quantities not yet measured for 67P/C–G, we use values obtained for other comets, e.g. concerning the optical and compositional properties of the dust grains. One of the most important and most controversial parameters is the dust mass distribution. We summarise the mass distribution functions derived from the in-situ measurements at comet 1P/Halley in 1986. For 67P/C–G, constraining the mass distribution is currently only possible by the analysis of astronomical images. We find that both the dust mass distribution and the time dependence of the dust production rate of 67P/C–G are those of a fairly typical comet.     

A synchrotron-based facility for the in-situ location,chemical and mineralogical characterization of ∼10 μm particles captured in aerogel

NASA’s Stardust mission collected dust from the coma of Comet Wild-2 on January 2nd, 2004, by direct capture into aerogel cells that flew through the dust coma at ∼6 km/s. Stardust collected several hundred comet particles >10 μm in size. These comet samples were delivered to Earth on January 15th, 2006. We developed a facility at the National Synchrotron Light Source at Brookhaven National Laboratory (Upton, NY, USA) for the in-situ characterization of ∼10 μm particles collected in aerogel. These analytical instruments allow us to perform extensive chemical, mineralogical, and size-frequency characterization of particles captured in aerogel. These analyses are conducted without any invasive extraction, minimizing the possibility of contamination or particle loss during preparation. This facility was used to determine the chemical composition, the oxidation state, the mineralogy and to provide an indication of the grain size of the Wild-2 particles before they were removed from the aerogel. This information provides a catalog of particle types, allowing a more reasoned allocation of the particles to subsequent investigators based on a relatively detailed knowledge of the chemical composition and mineralogy of each particle. These measurements allowed a comparison of the chemical and mineralogical properties of the Wild-2 particles with other types of extraterrestrial materials, including interplanetary dust particles and meteorites. The success of in-situ analysis for Wild 2 particles demonstrates that synchrotron-based facilities will be important for the analysis of particles collected in aerogel on future earth-orbiting satellites and spacecraft.     

空间粉尘高速撞击对光学玻璃透过率影响的研究

航天器在轨服役期间会遭受到大量的微陨石及空间微小碎片撞击作用.这些微陨石和空间微小碎片可能吸附在航天器光学玻璃表面,也可能与光学玻璃表面碰撞产生陷坑等缺陷.文章采用爆炸式粉尘加速器加速微米级铝粉末撞击K8光学玻璃,在玻璃表面产生大量碰撞陷坑形成砂蚀磨损现象,利用СФ-46型分光计测量光学玻璃的透过率.结果表明,光学玻璃磨损区域的透过率明显下降.透过率下降程度与陷坑数量成比例.通过对单个陷坑的计算,当陷坑深度大于或等于一个粒子直径时,光线衰减程度达到最大.     

Response of a pentagonal PZT element as a component of a 4π-real-time detector

The detector characteristics of a pentagonal element were studied by colliding it with hypervelocity micro-particles. A charge-sensitive amplifier was developed for the element of its capacitance ∼10 nF. The output amplitudes were expressed as a linear function of the momentum at collision. Empirical formulas obtained from on-ground experiments could be used for the calibration of the detector. The pentagonal element was potential to measure the momentum during collision from the output amplitude. A set of electrodes on the surface was used to confirm the measurement of the coordinates at collision. A possible application of this pentagonal element on a real-time dust detector was discussed.     

1-D dusty photo-ionization models of WR planetary nebulae NGC 2452 and IC 2003

We report dusty photo-ionization models for two Planetary Nebulae NGC 2452 and IC 2003, which have [WR] type central stars, using 1D photo-ionization code Cloudy17.02. We used the medium resolution optical spectra and archival IRAS photometry to constrain our models. The physical size of the ionized nebula derived using accurate distance measurements and absolute H$\beta$ flux available in the literature were used as additional constrains. We examine the importance of photo-electric heating and found that models with and without considering photo-electric heating do not make significant difference for both PNe for the MRN grain size distribution considered in this study. We derive the nebular elemental abundances of these PNe by the empirical method as well as by making dusty photo-ionization models. The values of N/O ratios for both PNe obtained from our models are lower than their respective values arrived using empirical methods. The central stars are assumed to be black bodies and the photospheric temperatures derived respectively for NGC 2452 and IC 2003 from their best fit models are 182 kK and 155 kK and their respective luminosities are 630$L_{\odot }$ and 1015$L_{\odot }$. We propose that both the PNe were resulted from low-mass progenitors of mass $?$2.8 M_⊙.