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。     

The dynamics of the solar radiative zone

The picture of the solar radiative zone is evolving quickly. This review is separated in two parts. We first recall how the two powerful probes of the solar interior, namely the neutrinos and helioseismology have scrutinized the microscopic properties of the solar radiative plasma. Recent observations stimulate today complementary activities beyond the standard stellar model through theoretical modeling of angular momentum transport by rotation, internal waves or (and) by magnetic fields to get access to the dynamical motions of this important region of the Sun. So in the second part, we summarize the first impact of such processes on the radiative zone.     

Active Region Dynamics

New methods of local helioseismology and uninterrupted time series of solar oscillation data from the Solar and Heliospheric Observatory (SOHO) have led to a major advance in our understanding of the structure and dynamics of active regions in the subsurface layers. The initial results show that large active regions are formed by repeated magnetic flux emergence from the deep interior, and that their roots are at least 50 Mm deep. The active regions change the temperature structure and flow dynamics of the upper convection zone, forming large circulation cells of converging flows. The helioseismic observations also indicate that the processes of magnetic energy release, flares and coronal mass ejections, might be associated with strong (1–2 km/s) shearing flows, 4–6 Mm below the surface.     

Recent progress in time–distance helioseismology

Time–distance helioseismology is one of the local helioseismology techniques that are used to derive the interior properties of the Sun. It has been used to study the structures and flow fields beneath sunspots on local scales, as well as used to derive interior rotational rates and meridional flow velocities on global scales. In addition to the efforts in improving time–distance measurements and inversions, theoretical modeling is also carried out to enhance the accuracy of sensitivity kernels. Recently, by use of realistic numerical simulation on solar convection, we have also started to investigate the validity of time–distance studies.     

The Progress of the Taiwan Oscillation Network Project

We describe the present status of the project of the Taiwan Oscillation Network (TON) and discuss a scientific result using the TON data. The TON is a ground-based network to measure solar intensity oscillations for the study of the solar interior. Four telescopes have been installed in appropriate longitudes around the world. The TON telescopes take K-line full-disk solar images of diameter 1000 pixels at a rate of one image per minute. The data has been collected since October of 1993. The TON high-spatial-resolution data are specially suitable for the study of local properties of the Sun. In 1997 we developed a new method, acoustic imaging, to construct the acoustic signals inside the Sun with the acoustic signals measured at the solar surface. From the constructed signals, we can form intensity map and phase-shift map of an active region at various depths. The direct link between these maps and the subsurface wave-speed perturbation suffers from the poor vertical resolution of acoustic imaging. Recently an inversion method has been developed to invert the measured phase travel time perturbation to estimate the distribution of wave-speed perturbation based on the ray approximation. This technique of acoustic imaging has been used to image the far-side of the Sun that could provides information on space weather prediction. The TON Team includes: Antonio Jimenez (Instituto Astrofisica de Canarias, Spain); Guoxiang Ai and Honqi Zhang (Huairou Solar Observing Station, P.R.C.); Philip Goode and William Marquette (Big Bear Solar Observatory, U.S.A.); Shuhrat Ehgamberdiev and Oleg Ladenkov (Ulugh Beg Astronomical Institute, Uzbekistan) This revised version was published online in August 2006 with corrections to the Cover Date.     

固体燃气发生器动力模拟水下发射试验研究

通过模拟水下试验,对导弹发射管充水工况下的固体燃气发生器动力发射技术进行了研究。结果表明,在发射管充水工况下燃气动力发射方式可行。与干式发射相比,该发射动力装置需要的装药量大,但发射管内的温度较低,热防护问题容易解决。在此基础上总结出发射深度、弹后空间、挡流板和装药量对发射内弹道的影响规律。试验表明,弹后空间越小,导弹出管速度越大;加装挡流板,可使导弹出管速度明显提高。通过试验对发射方案进行了优选。     

旋转发动机内弹道计算初探

提出了一种旋转固体火箭发动机的内弹道计算方法。在推导出旋转条件下的燃面变化规律的基础上,采用龙格库塔法求解了内弹道计算基本方程,并编制了计算程序。旋转和不旋转情况下的计算结果对比表明,旋转使发动机内压强增高,工作时间缩短,拖尾段加长。最后还就实验研究方法和实验结果处理进行了探讨。     

固体火箭发动机性能分析及预示

根据固体火箭发动机地面及高空模拟试验,提出了内弹道性能分析及预示方法,并编制了程序.通过算例给出了某发动机内弹道性能P-t、F-t、q_m-t、I_s-t、m_p-t曲线及试验修正系数k_1、ξ_(C_*)和ξ_(CF).计算表明,理论预示推力与测试推力基本一致,平均推力偏差不大于0.4%,平均比冲偏差不大于0.35%.由该程序计算的内弹道性能可提供导弹总体设计使用.     

SOHO: The Solar and Heliospheric Observatory

The Solar and Heliospheric Observatory (SOHO), together with the Cluster mission, constitutes ESA's Solar Terrestrial Science Programme (STSP), the first Cornerstone of the Agency's long-term programme Space Science — Horizon 2000. STSP, which is being developed in a strong collaborative effort with NASA, will allow comprehensive studies to be made of the both the Sun's interior and its outer atmosphere, the acceleration and propagation of the solar wind and its interaction with the Earth. This paper gives a brief overview of one part of STSP, the SOHO mission.     

基于IPDG方法的嵌套网格技术

在内罚间断伽辽金（IPDG）方法框架内应用嵌套网格技术求解了二维可压缩Navier-Stokes方程。通过把黏性通量作为辅助变量实现了Navier-Stokes方程的降阶,继而用间断有限元方法进行离散得到空间半离散方程。时间推进采用Newton-Krylov隐式方法。利用库埃特流动精确解验证了该方法的精度。在此基础上,对包括有黏NACA0012翼型绕流、定常和非定常的圆柱绕流在内的若干典型测试算例开展数值模拟,进一步验证了该方法的鲁棒性和可靠性。在嵌套网格中应用了h型网格自适应技术用于提高激波分辨率,对NACA0012翼型无黏跨声速绕流开展数值模拟,结果表明：自适应之后的单元数相比无自适应时只增加了8.4%,但是激波分辨率得到了显著提高,激波附近的计算结果也与实验值符合得更好,从而验证了该方法的有效性。