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91.
92.
智能微尘是一种关于微型无线传感器的新兴技术.本文着重介绍了智能微尘技术的应用情况,并对目前存在的问题和发展趋势做了简要的叙述. 相似文献
93.
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。 相似文献
94.
95.
Kamel A.K. Gadallah Abdallah A.M. Ali 《Advances in Space Research (includes Cospar's Information Bulletin, Space Research Today)》2021,67(12):4222-4237
Interstellar dust grains are illuminated in the reflection nebulae. Under conditions of the PAH size and the intensity of the interstellar radiation field, we follow their impact on the PAH aromatic infrared bands using the numerical DustEM code. For a dust model consisting of PAH, amorphous C and amorphous silicate, the PAH size varies in a range from 0.31 to 4.9 nm while the radiation intensity varies by a scale factor from 0.1 to 104. Various trends of the results show the effect of varying both the PAH size and the radiation intensity on the strength of the aromatic mid-IR bands. Through small PAH sizes less than 0.7 nm, the grain temperature distribution of PAHs shows a small variation within 2–3 K at low radiation intensity while it increases to 15 and 8 K for PAH0 and PAH+, respectively, at higher radiation intensity. In final the variability in these results reveals the evolution of the dust grains under the physical space conditions of the reflection nebulae. In the mid-IR region, the contributions of PAH0 and PAH+ in the total SED intensity agree with the proportions of these PAHs observed in some reflection nebulae having higher radiation intensities. 相似文献
96.
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. 相似文献
97.
A.M. Soltan M.J. Freyberg 《Advances in Space Research (includes Cospar's Information Bulletin, Space Research Today)》2004,34(12):2535-2539
The X-ray background intensity around galaxies and rich clusters of galaxies is investigated in three energy bands using the ROSAT All-Sky Survey maps. It is found that an amplitude of the XRB enhancements surrounding the Abell clusters and high density areas in the Lick galaxy counts depends on photon energy. Excess flux generated in the surrounding of the galaxy concentrations is consistent with the thermal emission by hot gas postulated by hydrodynamic simulations. 相似文献
98.
The combination of recent observational and theoretical work has completed the catalog of the sources of heliospheric Pickup
Ions (PUIs). These PUIs are the seed population for Anomalous Cosmic Rays (ACRs), which are accelerated to high energies at
or beyond the Termination Shock (TS). For elements with high First Ionization Potentials (high-FIP atoms: e.g., H, He, Ne,
etc.), the dominant source of PUIs and ACRs is from neutral atoms that drift into the heliosphere from the Local Interstellar
Medium (LISM) and, prior to ionization, are influenced primarily by solar gravitation and radiation pressure (for H). After
ionization, these interstellar ions are pickup up by the solar wind, swept out, and are either accelerated near the TS or
beyond it. Elements with low first ionization potentials (low-FIP atoms: e.g., C, Si, Mg, Fe, etc.) are also observed as PUIs
by Ulysses and as ACRs by Wind and Voyager. But the low-FIP composition of this additional component reveals a very different
origin. Low-FIP interstellar atoms are predominantly ionized in the LISM and therefore excluded from the heliosphere by the
solar wind. Remarkably, a low-FIP component of PUIs was hypothesized by Banks (J. Geophys. Res. 76, 4341, 1971) over twenty years prior to its direct detection by Ulysses/SWICS (Geiss et al., J. Geophys. Res. 100(23), 373, 1995) The leading concept for the generation of Inner Source PUIs involves an effective recycling of solar wind on grains near
the Sun, as originally suggested by Banks. Voyager and Wind also observe low-FIP ACRs, and a grain-related source appears
likely and necessary. Two concepts have been proposed to explain these low-FIP ACRs: the first concept involves the acceleration
of the Inner Source of PUIs, and the second involves a so-called Outer Source of PUIs generated from solar wind interaction
with the large population of grains in the Kuiper Belt. We review here the observational and theoretical work over the last
decade that shows how solar wind and heliospheric grains interact to produce pickup ions, and, in turn, anomalous cosmic rays.
The inner and outer sources of pickup ions and anomalous cosmic rays exemplify dusty plasma interactions that are fundamental
throughout the cosmos for the production of energetic particles and the formation of stellar systems. 相似文献
99.
Maren Rehders Bianka B. Grosshäuser Anita Smarandache Annapurna Sadhukhan Ursula Mirastschijski Jürgen Kempf Matthias Dünne Klaus Slenzka Klaudia Brix 《Advances in Space Research (includes Cospar's Information Bulletin, Space Research Today)》2011
Exposure to lunar dust during Apollo missions resulted in occasional reports of ocular, respiratory and dermal irritations which showed that lunar dust has a risk potential for human health. This is caused by its high reactivity as well as its small size, leading to a wide distribution also inside habitats. Hence, detailed information regarding effects of extraterrestrial lunar dusts on human health is required to best support future missions to moon, mars or other destinations. In this study, we used several methods to assess the specific effects of extraterrestrial dusts onto mammalian skin by exposing HaCaT keratinocytes and CHO-K1 fibroblasts to dusts simulating lunar or mars soils. These particular cell types were chosen because the skin protects the human body from potentially harmful substances and because a well orchestrated program ensures proper wound healing. Keratinocytes and fibroblasts were exposed to the dusts for different durations of time and their effects on morphology and viability of the cells were determined. Cytotoxicity was measured using the MTT assay and by monitoring culture impedance, while phalloidin staining of the actin cytoskeleton was performed to address structural integrity of the cells which was also investigated by propidium iodide intake. It was found that the effects of the two types of dust simulants on the different features of both cell lines varied to a considerable extent. Moreover, proliferation of HaCaT keratinocytes, as analyzed by Ki67 labeling, was suppressed in sub-confluent cultures exposed to lunar dust simulant. Furthermore, experimental evidence is provided for a delay in regeneration of keratinocyte monolayers from scratch-wounding when exposed to lunar dust simulant. The obtained results will facilitate further investigations of dust exposure during wound healing and will ease risk assessment studies e.g., for lunar lander approaches. The investigations will help to determine safety measures to be taken during extraterrestrial expeditions in order to minimize risks to human health associated with exposure of human skin to dust contaminants. 相似文献
100.
Nima Afshar-Mohajer Brian Damit Chang-Yu Wu Nicoleta Sorloaica-Hickman 《Advances in Space Research (includes Cospar's Information Bulletin, Space Research Today)》2011
Lunar grains accumulate charges due to solar-based ionizing radiations, and the repelling action of like-charged particles causes the levitation of lunar dust. The lunar dust deposit on sensitive and costly surfaces of investigative equipment is a serious concern in lunar explorations. Inspired by electrostatic precipitators (ESPs), the Electrostatic Lunar Dust Collector (ELDC) was proposed for collecting already charged lunar dust particles to prevent the lunar dust threat. As the conditions for terrestrial counterparts are not valid in the lunar environment, equations developed for terrestrial devices yield incorrect predictions in lunar application. Hence, a mathematical model was developed for the ELDC operating in vacuum to determine its collection efficiency. The ratios of electrical energy over potential energy, kinetic energy over potential energy and the ratio of ELDC dimensions were identified to be the key dimensionless parameters. Sensitivity analyses of the relevant parameters showed that depending on ELDC orientation, smaller particles would be collected more easily at vertical orientation, whereas larger particles were easier to collect in a horizontal ELDC configuration. In the worst case scenario, the electrostatic field needed to be 10 times stronger in the vertical mode in order to adequately collect larger particles. The collection efficiency was very sensitive to surface potential of lunar dust and it reached the maximum when surface potential was between 30 and 120 V. 相似文献