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991.
金属零件的一种快速成型制造方法 总被引:6,自引:0,他引:6
金属零件的快速制造是快速成型技术的最终目标之一,也是当今快速成型领域的一大研究热点。本文在介绍快速成型技术的一个重要分支-选区激光烧结的基础上,提出了一种基于小功率激光快速成型系统的金属零件成型工艺。这种方法首先烧结金属与有机粘结剂的混合粉末,生成“绿件”,而后除粘、熔渗金属,最终得到致密的金属件。最后,文中给出了加工实例,并对这种工艺的影响因素进行了详细的分析与讨论。 相似文献
992.
在应用模糊逻辑建模与辨识方法建立微下击暴流风切变模型的基础上,根据恒定俯仰姿态改出微下击暴流的飞行引导策略,提出了一种改出微下击暴流风切变的模糊反馈控制系统,并将遗传算法应用于该模糊逻辑控制器的设计。结果表明,本文提出的建模方法能够更真实地反映出飞机穿越微下击暴流风场的动态特性;采用模糊逻辑控制器,可使得飞机在穿越微下击暴流风场时具有较好的改出性能;另外,遗传算法的应用对已设计的模糊逻辑控制器进行了优化,进一步改善了飞机穿越微下击暴流的性能。 相似文献
993.
变化和重构是快速可重构信息系统 (RRIS)的两个核心概念 ,RRIS对变化的适应或演化能力使它优于传统信息系统。本文首先提出 RRIS的体系结构 ,然后以 RRIS框架为重点 ,讨论框架的定义、分类及设计 ,研究框架的构成、构成元素 (业务构件 )的设计及构件如何在构架的组织下协调地安插在 CORBA的软总线上 ,实现类似硬件IC的即插即用。构件在框架上即插即用的灵活机制及热点构件 (反映变化 )的灵活运用 ,提高了框架的可扩展性、可定制性 ,从而提高了 RRIS适应变化的可重构性。 相似文献
994.
T. Mukai K. Ogasawara Y. Saito 《Advances in Space Research (includes Cospar's Information Bulletin, Space Research Today)》2004,33(12):2166-2171
Since the flyby observations by Mariner 10 in 1974 and 1975, Mercury has been one of the most interesting objects for space physics and planetary exploration. The MESSENGER and BepiColombo missions now plan to revisit this planet. In order to design plasma instruments for the BepiColombo mission, we have estimated electron and ion fluxes around Mercury with an empirical model, which has been developed for the Earth’s magnetotail. The solar wind data needed as input parameters are derived from Helios observations. The result shows that our predicted electron fluxes at aphelion agree well with the Mariner-10 data. It is also noted that ion instruments must cover a very wide dynamic range of proton fluxes. However, the applicability of the Earth’s magnetospheric model to Mercury is, in itself, an important issue for comparative magnetospheric studies. 相似文献
995.
An analysis of the data from the Wind and IMP-8 spacecraft revealed that a slow solar wind, flowing in the heliospheric plasma sheet, represents a set of magnetic tubes with plasma of increased density (N > 10cm-3 at the Earth's orbit). They have a fine structure at several spatial scales (fractality), from 2°-3°(at the Earth's orbit, it is equivalent to 3.6-5.4h, or (5.4-8.0)×106km) to the minimum about 0.025°, i.e. the angular size of the nested tubes is changed nearly by two orders of magnitude. The magnetic tubes at each observed spatial scale are diamagnetic, i.e. their surface sustains a flow of diamagnetic (or drift) current that decreases the magnetic field within the tube itself and increases it outside the tube. Furthermore, the value of β= 8π[N(Te + Tp)]/B2 within the tube exceeds the value of βoutside the tube. In many cases total pressure P = N(Te + Tp) + B2/8πis almost constant within and outside the tubes at any one of the aforementioned scales. 相似文献
996.
997.
S.J. Wang D. Maia M. Pick G. Aulanier J.-M. Malherbe J.-P. Delaboudinire 《Advances in Space Research (includes Cospar's Information Bulletin, Space Research Today)》2005,36(12):2273
We present our research on a fast and decelerating partial halo coronal mass ejection (CME) event detected in multi-wavelengths in the chromosphere and the corona on 14 October, 1999. The event involved a whole complex active area which spanned more than 40° of heliolongitude. It included a strong solar flare (XI/1N) and a complex eruptive filament within an active region of the entire complex. Especially, several radio sources were detected in the decimetric range prior to the CME by the Nançay Radioheliograph (NRH). A linear force-free field extrapolation of the Michelson Doppler Imager (MDI) magnetogram was performed to calculate the magnetic topology of the complex prior to the triggering of the event. The presence of a coronal null point combined with the occurrence of two distant and nearly simultaneous radio sources put strong arguments in favor of the generalized breakout model for the triggering of the eruption. The analysis of the subsequent development of the event suggests that large interconnecting loops were ejected together with the CME. 相似文献
998.
Non-thermal components are key ingredients for understanding clusters of galaxies. In the hierarchical model of structure
formation, shocks and large-scale turbulence are unavoidable in the cluster formation processes. Understanding the amplification
and evolution of the magnetic field in galaxy clusters is necessary for modelling both the heat transport and the dissipative
processes in the hot intra-cluster plasma. The acceleration, transport and interactions of non-thermal energetic particles
are essential for modelling the observed emissions. Therefore, the inclusion of the non-thermal components will be mandatory
for simulating accurately the global dynamical processes in clusters. In this review, we summarise the results obtained with
the simulations of the formation of galaxy clusters which address the issues of shocks, magnetic field, cosmic ray particles
and turbulence. 相似文献
999.
1994年2月21日行星际激波引起的磁暴 总被引:2,自引:0,他引:2
利用Imp-8,Geotail和Goes-6等卫星资料,研究了1994年2月21日0900UT到达地球磁层的行星际激波引起的磁暴期间,从太阳风向磁层传输能量的有关问题.结果指出:(1)南向行星际磁场(IMF)的长持续时间不是太阳风向磁层输能的必要条件.南北振荡的,较强IMF也能产生显著的能量传输;(2)行星际扰动磁场通过弓激波和磁层顶后扰动磁能增加,增幅将近5倍;(3)在磁层内扰动磁场的Bz分量在1×10-4Hz附近显著被吸收.这一低频扰动磁场可能是磁暴期间导致氧离子和质子等环电流粒子向内扩散并被加速的原因之一. 相似文献
1000.
V. S. Makhmutov P. Kaufmann J. E. R. Costa P. R. Lagrotta A. Magun K. Arzner G. A. Bazilevskaya M. A. Shea 《Advances in Space Research (includes Cospar's Information Bulletin, Space Research Today)》2002,29(12):1186-2104
Itapetinga measurements at 48 GHz with the multibeam technique are used to determine the relative position of solar burst centroid of emission with high spatial accuracy and time resolution. For the Great Bursts of October 19,22, 1989, with a large production of relativistic particles, and October 23, it is suggested that, at 48 GHz, the bursts might have originated in more then one source in space and time. Additionally the October 19 and 22 Ground Level Events exhibited very unusual intensity-time profiles including double component structures for the onset phase. The Bern observatory spectral radio emission data show a strong spectral flattening typical for large source inhomogeneties. The interpretation for this is that large solar flares are a superposition of a few strong bursts (separated both in space and time) in the same flaring region. 相似文献