基于单神经元算法的内嵌式永磁同步电机智能驱动控制

基于人工神经网络的内嵌式永磁同步电机(IPMSM)智能驱动控制性能要明显优于传统控制方法,但是存在计算量大和离线训练时间长的问题。针对该问题,提出了一种基于单神经元算法的IPMSM智能驱动控制策略。阐述了永磁同步电机的数学模型及电流转矩控制规律;并基于单神经元的控制原理,推导了驱动控制律,由于采用的是单神经元结构并设置了迭代算法的边界,因此达到了计算量减小和训练较少的效果。最后,搭建了小功率电机驱动试验平台开展了试验研究,并通过与传统PID控制的对比试验,验证了新型控制器的性能。     

超燃冲压发动机隔离段流动特性研究

隔离段是双模态超燃冲压发动机实现双模态和模态转换的一个重要部件,同时它把进气道和燃烧室隔离开,以防止燃烧室工作对进气道干扰,引起进气道不启动。由于隔离段内流场的复杂性及其广泛的工程应用前景,隔离段内的流动特性引起了人们广泛的关注。本文利用计算流体力学软件Fluent,采用k-ε湍流模型,近壁面采用非平衡壁面函数方法处理,控制方程的离散采用二阶迎风格式,对隔离段的流场进行了数值模拟,并分析了出口反压、来流马赫数等参数对隔离段内流场的影响。     

Phobos regolith simulants PGI-1 and PCA-1

The Martian moon Phobos is the target of the upcoming JAXA Martian Moons eXploration (MMX) mission. There are currently no known samples of Phobos, so spacecraft hardware testing and scientific studies require Phobos regolith simulants. Here, we present two new Phobos regolith simulants: Phobos Captured Asteroid-1 (PCA-1) and Phobos Giant Impact (PGI-1). These two simulants reflect the two hypotheses for Phobos’s formation, and thus the two broad possibilities for composition. This work follows previous efforts to document the development of mineralogically accurate simulants, in an effort to overcome past pitfalls with inappropriate uses of simulants. We report physical and geotechnical properties of PCA-1 and PGI-1, including their reflectance spectra, grain size distributions, abrasivity, cohesion, strength, and hardness. Our intent is for PCA-1 and PGI-1 to be open standards for Phobos simulants, and we present the simulant recipes and production methodology for use and modification by the community.     

Longitudinal MLT wind structure at higher mid-latitudes as seen by meteor radars at central and Eastern Europe (13°E/49°E)

The mid-latitude mesosphere and lower thermosphere (MLT) wind speeds measured by two SKiYMET meteor radars (MRs) at Collm (51°N, 13°E) and Kazan (56°N, 49°E) during 2016–2017 were analyzed to study longitudinal wind structures. The differences between monthly mean prevailing wind speeds and tidal amplitudes were compared with the corresponding differences obtained from TIMED/TIDI satellite winds and gradient wind speeds from the AURA/MLS instrument. It is shown that the MR wind difference between the two sites is statistically significant. The difference of the horizontal prevailing winds can be explained by a superposition of the background zonal flow, which is different at the two latitudes, with stationary planetary waves of different origin. Non-migrating tides contribute significantly to the difference of the semidiurnal tidal winds between the two sites.     

非对称超声速来流下矩形转圆隔离段研究

为了适应超燃冲压发动机模块化设计及圆形燃烧室的需求,隔离段必须设计成矩形截面渐变为圆形出口的形状。发展了一种基于超椭圆曲线的截面渐变方法,以此设计了矩形转圆隔离段,开展了数值模拟研究并进行了在Ma=2.1且来流条件非对称下的矩形转圆隔离段吹风实验。研究结果表明:在反压相同时,两种不同来流条件下矩形转圆隔离段的出口总压恢复系数较等直矩形隔离段分别提高了4%和5%;在非对称来流实验条件下,矩形转圆隔离段壁面沿程压力分布规律与等直矩形隔离段压力分布规律趋势一致,上壁面沿程压力曲线前部呈波动式上升,后半部上升平缓,而下壁面沿程压力曲线整体上升较为平缓,随着出口反压的增大,总压恢复系数随之减小,矩形转圆隔离段最大能够承受4.1倍的来流静压,极限反压状态下出口总压恢复系数为0.505。     

一种带抽吸狭缝的新型短隔离段数值研究

为了缩短超燃冲压发动机隔离段长度以及提高它的耐反压能力,采用数值模拟方法研究了一种带抽吸狭缝的新型短隔离段,获得了隔离段的缩短程度以及耐反压能力提高的程度。结果表明,通过流向狭缝抽吸隔离段角流区内的低能附面层,可不降低隔离段耐反压能力而将其长度缩短30%左右。同一隔离段采用狭缝抽吸后,能够承受的最大反压从来流静压的3.46倍上升到3.74倍,提高了8%左右。合理的狭缝位置应在厚附面层一侧的隔离段前部角流区内,前倾角对隔离段性能的影响呈非线性特征,抽吸背压在亚临界范围时对隔离段性能的影响较明显,而在超临界范围时的影响则不明显。     

教师的创造性素质与学生创造能力的培养

培养创造能力是高等教育的重要任务，是时代的要求，要开展创造教育，培养学生的创造力就必须建设一支具有创造性素质的教师队伍。     

基于波叠加法高速列车单车通过隧道诱发压力波计算方法

通过分析列车通过隧道过程中压力波的产生机理,并根据近年来国外学者提出的基于经验计算特征波的简单隧道内压力波计算方法,得出了隧道内和列车上任意时刻压力可以看作是多个特征波的叠加的结论,把压力波的计算问题就转化为特征波的叠加问题,建立了隧道压力波的波叠加计算方法。计算与国外实车试验结果吻合良好,通过与试验数据和特征线法计算结果的对比,证明了本文所建的叠加法计算压力波的方法的正确性和可行性。随后研究了阻塞比、车速和隧道长度的影响特性,验证了本文所建方法具有良好的预测结果。     

The James Webb Space Telescope

The James Webb Space Telescope (JWST) is a large (6.6 m), cold (<50 K), infrared (IR)-optimized space observatory that will be launched early in the next decade into orbit around the second Earth–Sun Lagrange point. The observatory will have four instruments: a near-IR camera, a near-IR multiobject spectrograph, and a tunable filter imager will cover the wavelength range, 0.6 < ; < 5.0 μ m, while the mid-IR instrument will do both imaging and spectroscopy from 5.0 < ; < 29 μ m.The JWST science goals are divided into four themes. The key objective of The End of the Dark Ages: First Light and Reionization theme is to identify the first luminous sources to form and to determine the ionization history of the early universe. The key objective of The Assembly of Galaxies theme is to determine how galaxies and the dark matter, gas, stars, metals, morphological structures, and active nuclei within them evolved from the epoch of reionization to the present day. The key objective of The Birth of Stars and Protoplanetary Systems theme is to unravel the birth and early evolution of stars, from infall on to dust-enshrouded protostars to the genesis of planetary systems. The key objective of the Planetary Systems and the Origins of Life theme is to determine the physical and chemical properties of planetary systems including our own, and investigate the potential for the origins of life in those systems. Within these themes and objectives, we have derived representative astronomical observations.To enable these observations, JWST consists of a telescope, an instrument package, a spacecraft, and a sunshield. The telescope consists of 18 beryllium segments, some of which are deployed. The segments will be brought into optical alignment on-orbit through a process of periodic wavefront sensing and control. The instrument package contains the four science instruments and a fine guidance sensor. The spacecraft provides pointing, orbit maintenance, and communications. The sunshield provides passive thermal control. The JWST operations plan is based on that used for previous space observatories, and the majority of JWST observing time will be allocated to the international astronomical community through annual peer-reviewed proposal opportunities.