空间微小颗粒对卫星光学器件的污染研究

空间微小颗粒以低于临界黏附速度撞击卫星光学镜头时会附着在其表面,当大量的微粒黏附在卫星镜头上时会影响镜头的探测性能。精确计算临界黏附速度及找出影响临界黏附速度的因素对研究空间污染效率有着重要意义。在简化的EA模型的基础上,文章仿真分析了铜和石墨微粒撞击卫星镜头过程中的黏附力和临界黏附速度。结果表明:镜头表面粗糙度修正系数CR是影响黏附力和临界黏附速度的重要参数;在相同条件下,虽然石墨微粒受到的最大黏附力比铜微粒的小,但石墨微粒的临界黏附速度比铜微粒的高,说明石墨微粒更有可能黏附于镜头表面。     

浮子组件密封空间微环境污染特征 对马达性能的影响分析

本文重点关注和探讨了高精度惯性仪表制造技术特征引发的浮子组件微环境体系中污染形成的机理和进入的途径,提出了控制、清除的方法.首次提出了多余物控制技术本质上是污染物跟踪控制技术,在高精度、高可靠性航天密封产品设计和制造中重视内部空间微环境和微动态环境污染体系对产品性能和可靠性的持久性影响作用,要有效识别零部组件在产品制造各阶段清洁的目的和方法,才能真正消除各种工艺污染对产品性能与可靠性的影响,这也是动压马达多余物控制的有效措施.     

A novel wireless light sensing device for planetary and astronomical observations

A novel and versatile wireless light sensing device has been designed and tested for stellar and planetary photometric observations. The device weighing few 10 s of grams finds a number of potential applications in the fields of astronomy and in situ planetary exploration. A Wireless Sensor Network (WSN) using a number of these devices has been deployed to successfully carry out simultaneous photometric observations under different conditions viz. sunlight, twilight, moonlight etc. Observation of a star of known magnitude for flux calibration at low intensity has been carried out by coupling the device to a 1.2 m telescope which demonstrates its sensitivity. A WSN using these devices is further capable of spatio-temporal investigations of sky background intensities. Such a network can also be used to effectively monitor certain astronomical events (lunar eclipse, asteroid occultation etc.) simultaneously from several locations. The capability of the device, level of miniaturization and its versatility makes it a potential tool for many photometric applications.     

液压传动系统综合污染分析与控制方法研究

详细分析了工作油液中的固体颗粒、水、气、氯污染物的特征及其对系统的影响.通过多年污染控制实践,以及在汲取国内外先进的污染控制技术的基础上,阐述了各种污染物的控制方法及测试技术,提出了全面污染控制的设想.     

The Composition of Cosmic Rays and the Mixing of the Interstellar Medium

The differences between the composition of Galactic cosmic rays and that of the interstellar medium are manifold, and they contain a wealth of information about the varying processes that created them. These differences reveal much about the initial mixing of freshly synthesized matter, the chemistry and differentiation of the interstellar medium, and the mechanisms and environment of ion injection and acceleration. Here we briefly explore these processes and show how they combine to create the peculiar, but potentially universal, composition of the cosmic rays and how measurements of the composition can provide a unique measure of the mixing ratio of the fresh supernova ejecta and the old interstellar medium in this initial phase of interstellar mixing. In particular, we show that the major abundance differences between the cosmic rays and the average interstellar medium can all result from cosmic ray ion injection by sputtering and scattering from fast refractory oxide grains in a mix of fresh supernova ejecta and old interstellar material. Since the bulk of the Galactic supernovae occur in the cores of superbubbles, the bulk of the cosmic rays are accelerated there out of such a mix. We show that the major abundance differences all imply a mixing ratio of the total masses of fresh supernova ejecta and old interstellar material in such cores is roughly 1 to 4. That means that the metallicity of ∼3 times solar, since the ejecta has a metallicity of ∼8 times that of the present interstellar medium.     

Interstellar Dust in the Solar System

The Ulysses spacecraft has been orbiting the Sun on a highly inclined ellipse almost perpendicular to the ecliptic plane (inclination 79°, perihelion distance 1.3 AU, aphelion distance 5.4 AU) since it encountered Jupiter in 1992. The in situ dust detector on board continuously measured interstellar dust grains with masses up to 10⁻¹³ kg, penetrating deep into the solar system. The flow direction is close to the mean apex of the Sun’s motion through the solar system and the grains act as tracers of the physical conditions in the local interstellar cloud (LIC). While Ulysses monitored the interstellar dust stream at high ecliptic latitudes between 3 and 5 AU, interstellar impactors were also measured with the in situ dust detectors on board Cassini, Galileo and Helios, covering a heliocentric distance range between 0.3 and 3 AU in the ecliptic plane. The interstellar dust stream in the inner solar system is altered by the solar radiation pressure force, gravitational focussing and interaction of charged grains with the time varying interplanetary magnetic field. We review the results from in situ interstellar dust measurements in the solar system and present Ulysses’ latest interstellar dust data. These data indicate a 30° shift in the impact direction of interstellar grains w.r.t. the interstellar helium flow direction, the reason of which is presently unknown.     

The heart-shaped supernova remnant 3C 391 viewed in multi-bands

Using Chandra X-ray, Spitzer mid-IR, and 1.5 GHz radio data, we examine the spatial structure of SNR 3C 391. The X-ray surface brightness is generally anti-correlative with the IR and radio brightness. The multiband data clearly exhibit a heart-shaped morphology and show the multi-shell structure of the remnant. A previously unseen thin brace-like shell on the south detected at 24 μm is projected outside the radio border and confines the southern faint X-ray emission. The leading 24 μm knot on the SE boundary appears to be partly surrounded by soft X-ray emitting gas. The mid-IR emission is dominated by the contribution of the shocked dust grains, which may have been partly destroyed by sputtering.     

含水率对电动修复Cr（Ⅵ）污染高岭土的影响

实验选用重铬酸钾作为污染物，配制高岭土中Cr（Ⅵ）初始质量分数为500mg·kg^-1。实验研究了不同含水率对电动修复效率的影响程度。实验结果表明：含水率极低时，由于电迁移和电渗流作用都很小，去除效率很低，需要其它的方式提高去除效率；在达到饱和状态时，含水率对去除效率影响很小，几乎为零。在一般含水率情况下，含水率对去除效率影响很大，在以后的中试或现场试验中，建议通过改变含水率的大小来提高去除效率，还需进一步研究。     

浅谈机务维护中液压系统的污染控制

液压系统污染是液压故障的一个主要原因,为了确保液压系统能够安全、可靠运行,针对外场机务工作提出一系列具体措施,以达到机务维护过程中的污染控制。     

Atmospheric electrical conductivity measurements and modeling for application to air pollution studies

The experimentally measured ground level atmospheric electrical conductivity is validated from a simplified ion–aerosol model for which the inputs are ionization rate from surface radioactivity, aerosol density and meteorological parameters. Also estimated from the model is the reduction in conductivity for assumed aerosol levels. It is seen that for an increase of ambient aerosols by threefold the percent reduction in conductivity is 7% and it is 10% for an increase by sixfold. Thus, the variations in the measured ground level conductivity can be used to examine the atmospheric pollution, if any.