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851.
单晶铝纳米级硬度试验研究 总被引:1,自引:0,他引:1
使用纳米硬度计对单晶铝进行了纳米压痕试验,利用原子力显微镜对压痕形貌进行扫描并计算硬度值,重点观察和分析了纳米级条件下单晶铝的硬度性质,结果表明,当压痕深度小于2000nm时,单晶铝纳米硬度存在尺寸效应现象;从材料性质的角度分析了纳米硬度尺寸效应现象;探讨了纳米硬度和传统硬度本质上的区别,指出其根本原因在于不同尺度下人们对材料性质的关注点不同。 相似文献
852.
Examination of the spatial distribution of CO intensity of Comet Halley indicates that a large fraction of CO originates from
the refractory organic component in the coma, rather than directly from the volatiles in the nucleus. Based on the fluffy
aggregate interstellar dust comet model, we have estimated the upper limits of the total amount of CO provided by coma dust.
The implications from the comparison of the predicted results with the observed value have been discussed.
This revised version was published online in June 2006 with corrections to the Cover Date. 相似文献
853.
航空发动机用金属橡胶隔振器动静态性能的研究 总被引:14,自引:1,他引:14
以某型号航空发动机阻尼减振需求为背景,对开发研制的金属橡胶隔振器与现用的橡胶隔振器进行了动、静态实验研究。研究结果表明:金属橡胶隔振器的能量耗散性能、静态承载能力、过临界的能力及提供振动防护的区域都远远大于橡胶隔振器,而且通过改变金属橡胶隔振器的结构参数和预压缩量可以优化其隔振效果。研究结果为利用金属橡胶隔振器来改善航空发动机的振动状况提供了依据。 相似文献
854.
R. H. Brown K. H. Baines G. Bellucci J.-P. Bibring B. J. Buratti F. Capaccioni P. Cerroni R. N. Clark A. Coradini D. P. Cruikshank P. Drossart V. Formisano R. Jaumann Y. Langevin D. L. Matson T. B. Mccord V. Mennella E. Miller R. M. Nelson P. D. Nicholson B. Sicardy C. Sotin 《Space Science Reviews》2004,115(1-4):111-168
The Cassini visual and infrared mapping spectrometer (VIMS) investigation is a multidisciplinary study of the Saturnian system. Visual and near-infrared imaging spectroscopy and high-speed spectrophotometry are the observational techniques. The scope of the investigation includes the rings, the surfaces of the icy satellites and Titan, and the atmospheres of Saturn and Titan. In this paper, we will elucidate the major scientific and measurement goals of the investigation, the major characteristics of the Cassini VIMS instrument, the instrument calibration, and operation, and the results of the recent Cassini flybys of Venus and the Earth–Moon system.This revised version was published online in July 2005 with a corrected cover date. 相似文献
855.
R. Srama T. J. Ahrens N. Altobelli S. Auer J. G. Bradley M. Burton V. V. Dikarev T. Economou H. Fechtig M. Görlich M. Grande A. Graps E. Grün O. Havnes S. Helfert M. Horanyi E. Igenbergs E. K. Jessberger T. V. Johnson S. Kempf A. V. Krivov H. Krüger A. Mocker-Ahlreep G. Moragas-Klostermeyer P. Lamy M. Landgraf D. Linkert G. Linkert F. Lura J. A. M. McDonnell D. Möhlmann G. E. Morfill M. Müller M. Roy G. Schäfer G. Schlotzhauer G. H. Schwehm F. Spahn M. Stübig J. Svestka V. Tschernjawski A. J. Tuzzolino R. Wäsch H. A. Zook 《Space Science Reviews》2004,114(1-4):465-518
The Cassini-Huygens Cosmic Dust Analyzer (CDA) is intended to provide direct observations of dust grains with masses between 10−19 and 10−9 kg in interplanetary space and in the jovian and saturnian systems, to investigate their physical, chemical and dynamical properties as functions of the distances to the Sun, to Jupiter and to Saturn and its satellites and rings, to study their interaction with the saturnian rings, satellites and magnetosphere. Chemical composition of interplanetary meteoroids will be compared with asteroidal and cometary dust, as well as with Saturn dust, ejecta from rings and satellites. Ring and satellites phenomena which might be effects of meteoroid impacts will be compared with the interplanetary dust environment. Electrical charges of particulate matter in the magnetosphere and its consequences will be studied, e.g. the effects of the ambient plasma and the magnetic field on the trajectories of dust particles as well as fragmentation of particles due to electrostatic disruption.The investigation will be performed with an instrument that measures the mass, composition, electric charge, speed, and flight direction of individual dust particles. It is a highly reliable and versatile instrument with a mass sensitivity 106 times higher than that of the Pioneer 10 and 11 dust detectors which measured dust in the saturnian system. The Cosmic Dust Analyzer has significant inheritance from former space instrumentation developed for the VEGA, Giotto, Galileo, and Ulysses missions. It will reliably measure impacts from as low as 1 impact per month up to 104 impacts per second. The instrument weighs 17 kg and consumes 12 W, the integrated time-of-flight mass spectrometer has a mass resolution of up to 50. The nominal data transmission rate is 524 bits/s and varies between 50 and 4192 bps.This revised version was published online in July 2005 with a corrected cover date. 相似文献
856.
Ground penetrating radar VIY-2 总被引:2,自引:0,他引:2
Prokhorenko V.P. Ivashchuk V.E. Korsun S.V. 《Aerospace and Electronic Systems Magazine, IEEE》2005,20(7):16-18
VIY-2 ground penetrating radar (GPR) with unique sounding possibilities and use simplicity is presented at this paper. VIY-2 GPR combines all units (synchronizer, transmitting and receiving modules, powering, and antenna system) into single case. The VIY-2 GPR communicates with computer via standard interface RS232 or USB1.0. Technical solutions utilized by the VIY-2 GPR reduce deployment time and simplify surveying process. The VIY-2 GPR design features and its components interaction are considered at this paper. Some field results are also presented here. The VIY-2 GPR design concept allows reducing the data acquisition time,, optimizing the time-varying gain control function, applying depth-stacking dependence, controlling the surveying window position and interference reducing by pulse repetition frequency randomizing. 相似文献
857.
Until pristine samples can be returned from cometary nuclei, primitive meteorites represent our best source of information
about organic chemistry in the early solar system. However, this material has been affected by secondary processing on asteroidal
parent bodies which probably did not affect the material now present in cometary nuclei. Production of meteoritic organic
matter apparently involved the following sequence of events: Molecule formation by a variety of reaction pathways in dense
interstellar clouds; Condensation of those molecules onto refractory interstellar grains; Irradiation of organic-rich interstellar-grain
mantles producing a range of molecular fragments and free radicals; Inclusion of those interstellar grains into the protosolar
nebula with probable heating of at least some grain mantles during passage through the shock wave bounding the solar accretion
disc; Agglomeration of residual interstellar grains and locally produced nebular condensates into asteroid-sized planetesimals;
Heating of planetesimals by decay of extinct radionuclides; Melting of ice to produce liquid water within asteroidal bodies;
Reaction of interstellar molecules, fragments and radicals with each other and with the aqueous environment, possibly catalysed
by mineral grains; Loss of water and other volatiles to space yielding a partially hydrated lithology containing a complex
suite of organic molecules; Heating of some of this organic matter to generate a kerogen-like complex; Mixing of heated and
unheated material to yield the meteoritic material now observed. Properties of meteoritic organic matter believed to be consistent
with this scenario include: Systematic decrease of abundance with increasing C number in homologous series of characterisable
molecules; Complete structural diversity within homologous series; Predominance of branched-chain isomers; Considerable isotopic
variability among characterisable molecules and within kerogen-like material; Substantial deuterium enrichment in all organic
fractions; Some fractions significantly enriched in nitrogen-15; Modest excesses of L-enantiomers in some racemisation-resistant
molecules but no general enantiomeric preference. Despite much speculation about the possible role of Fischer-Tropsch catalytic
hydrogenation of CO in production of organic molecules in the solar nebula, no convincing evidence for such material has been
found in meteorites. A similarity between some meteoritic organics and those produced by Miller-Urey discharge synthesis may
reflect involvement of common intermediates rather than the operation of electric discharges in the early solar system. Meteoritic
organic matter constitutes a useful, but not exact, guide to what we shall find with in situ analytical and sample-return
missions to cometary nuclei.
This revised version was published online in June 2006 with corrections to the Cover Date. 相似文献
858.
859.
Streamer evaporation is the consequence of heating in ideal MHD models because plasma is weakly contained by the magnetic
field. Heating causes inflation, opening of field lines, and release of solar wind. It was discovered in simulations and,
due to the absence of loss mechanisms, the ultimate end point is the complete evaporation of the streamer. Of course streamers
do not behave in this way because of losses by thermal conduction and radiation. Heating is also expected to depend on ambient
conditions. We use a global MHD model with thermal conduction to examine the effect of changing the heating scale height.
We also extend an analytic model of streamers developed by Pneuman (1968) to show that steady streamers are unable to contain
plasma for temperatures near the cusp greater than ∼ 2 × 106 K.
This revised version was published online in June 2006 with corrections to the Cover Date. 相似文献
860.
2001 Mars Odyssey Mission Summary 总被引:1,自引:0,他引:1
Saunders R.S. Arvidson R.E. Badhwar G.D. Boynton W.V. Christensen P.R. Cucinotta F.A. Feldman W.C. Gibbs R.G. Kloss C. Landano M.R. Mase R.A. McSmith G.W. Meyer M.A. Mitrofanov I.G. Pace G.D. Plaut J.J. Sidney W.P. Spencer D.A. Thompson T.W. Zeitlin C.J. 《Space Science Reviews》2004,110(1-2):1-36
The 2001 Mars Odyssey spacecraft, now in orbit at Mars, will observe the Martian surface at infrared and visible wavelengths to determine surface mineralogy and morphology, acquire global gamma ray and neutron observations for a full Martian year, and study the Mars radiation environment from orbit. The science objectives of this mission are to: (1) globally map the elemental composition of the surface, (2) determine the abundance of hydrogen in the shallow subsurface, (3) acquire high spatial and spectral resolution images of the surface mineralogy, (4) provide information on the morphology of the surface, and (5) characterize the Martian near-space radiation environment as related to radiation-induced risk to human explorers. To accomplish these objectives, the 2001 Mars Odyssey science payload includes a Gamma Ray Spectrometer (GRS), a multi-spectral Thermal Emission Imaging System (THEMIS), and a radiation detector, the Martian Radiation Environment Experiment (MARIE). THEMIS and MARIE are mounted on the spacecraft with THEMIS pointed at nadir. GRS is a suite of three instruments: a Gamma Subsystem (GSS), a Neutron Spectrometer (NS) and a High-Energy Neutron Detector (HEND). The HEND and NS instruments are mounted on the spacecraft body while the GSS is on a 6-m boom. Some science data were collected during the cruise and aerobraking phases of the mission before the prime mission started. THEMIS acquired infrared and visible images of the Earth-Moon system and of the southern hemisphere of Mars. MARIE monitored the radiation environment during cruise. The GRS collected calibration data during cruise and aerobraking. Early GRS observations in Mars orbit indicated a hydrogen-rich layer in the upper meter of the subsurface in the Southern Hemisphere. Also, atmospheric densities, scale heights, temperatures, and pressures were observed by spacecraft accelerometers during aerobraking as the spacecraft skimmed the upper portions of the Martian atmosphere. This provided the first in-situ evidence of winter polar warming in the Mars upper atmosphere. The prime mission for 2001 Mars Odyssey began in February 2002 and will continue until August 2004. During this prime mission, the 2001 Mars Odyssey spacecraft will also provide radio relays for the National Aeronautics and Space Administration (NASA) and European landers in early 2004. Science data from 2001 Mars Odyssey instruments will be provided to the science community via NASA’s Planetary Data System (PDS). The first PDS release of Odyssey data was in October 2002; subsequent releases occur every 3 months. 相似文献