Spectroscopic Constraints on Models of Ion-cyclotron Resonance Heating in the Polar Solar Corona

Using empirical velocity distributions derived from UVCS and SUMER ultraviolet spectroscopy, we construct theoretical models of anisotropic ion temperatures in the polar solar corona. The primary energy deposition mechanism we investigate is the dissipation of high frequency (10-10000 Hz) ion-cyclotron resonant Alfvén waves which can heat and accelerate ions differently depending on their charge and mass. We find that it is possible to explain the observed high perpendicular temperatures and strong anisotropies with relatively small amplitudes for the resonant waves. There is suggestive evidence for steepening of the Alfvén wave spectrum between the coronal base and the largest heights observed spectroscopically. Because the ion-cyclotron wave dissipation is rapid, even for minor ions like O⁵⁺, the observed extended heating seems to demand a constantly replenished population of waves over several solar radii. This indicates that the waves are generated gradually throughout the wind rather than propagated up from the base of the corona. This revised version was published online in June 2006 with corrections to the Cover Date.     

用衰减全反射(ATR)研究金属薄膜的物理性质

本文作者所设计的实验是利用光学中全反射衰减特性方法测量在介质上蒸镀的金属薄膜的厚度和各种频率下的复介电常数等物理性质，它可以精确测定１００～１０００范围内金属膜层的厚度和ε（ω）值，以及一些其它性质，是研究固体表面物理的一种有效的方法和技术。     

Solar flare forecasting model supported with artificial neural network techniques

Nowadays operational models for solar activity forecasting are still based on the statistical relationship between solar activity and solar magnetic field evolution. In order to set up this relationship, many parameters have been proposed to be the measures. Conventional measures are based on the sunspot group classification which provides limited information from sunspots. For this reason, new measures based on solar magnetic field observations are proposed and a solar flare forecasting model supported with an artificial neural network is introduced. This model is equivalent to a person with a long period of solar flare forecasting experience.     

星敏感器低频误差与陀螺漂移离线校正方法

获取高精度事后姿态数据是提高遥感平台成像质量的必要条件之一,离线处理可有效降低敏感器测量误差,从而获得更高的姿态确定精度。基于滤波的校正方法中,星敏感器低频误差(LFE)与陀螺漂移将产生耦合影响导致校正精度低,本文针对该问题推导了耦合误差的数学模型,并设计了一种两步双向平滑事后处理算法,将陀螺漂移与低频误差分两步校正,通过反复滤波剥离陀螺漂移与低频误差。同时,针对低频误差参数收敛速度慢、噪声参数调节困难的问题,利用一种基于极大似然估计(MLE)的固定窗口自适应双向滤波算法进行处理以获得更好的噪声估计,提高了收敛速度和收敛精度。文中仿真工况下,离线姿态确定精度可达到0.8″(3σ),低频误差参数完全收敛时间不超过4个轨道周期。     

磁转速表指针摆动的故障分析

就磁转速表活动系统的动态特性以及在附加交变力矩的作用下，指针摆动随转速变化的规律，从理论上进行了分析，并结合实际探讨了指针摆动的故障原因。     

The evolution of mirror type magnetic fluctuations in the magnetosheath based on multipoint observations

Two orbits were selected in January–February 2006 when the separation between the Cluster spacecraft was large and mirror type magnetic field fluctuations were observed by all spacecraft in different regions of the terrestrial magnetosheath. Minimum variance analysis was applied to find the mirror type fluctuations, and the amplitude of the fluctuations was determined individually. Mirror mode structures are moving along the streamlines frozen in the plasma. A model was developed for the calculation of plasma flowtime from the bow shock to the observation point. The growth rate of the field strength perturbations was estimated by comparing the amplitudes of fluctuations observed simultaneously at distant locations (∼10,000 km) based on the assumption that δB ∼ exp(γt). The obtained growth rate values were about an order of magnitude smaller than those provided by linear models and they decreased in the inner regions of the magnetosheath, indicating some saturation in the growth of the waves when proceeding towards the magnetopause. The results of these two case studies suggest that mirror type fluctuations originate from the compression region downstream of the quasi-perpendicular bow shock, and the growth of the fluctuations cannot be described by linear approximations.     

一种新型正弦压力发生器

介绍了一种利用压电叠堆激励管道内液体介质发生谐振产生正弦压力的发生装置.与其它正弦压力发生器相比,本装置压力源的激励方式新颖,工作频率较高,所产生的正弦压力波的幅值较大,失真度较小.     

Alfvénic Electron Acceleration in Aurora Occurs in Global Alfvén Resonosphere Region

Auroral emission caused by electron precipitation (Hardy et al., 1987, J. Geophys. Res. 92, 12275–12294) is powered by magnetospheric driving processes. It is not yet fully understood how the energy transfer mechanisms are responsible for the electron precipitation. It has been proposed (Hasegawa, 1976, J. Geophys. Res. 81, 5083–5090) that Alfvén waves coming from the magnetosphere play some role in powering the aurora (Wygant et al., 2000, J. Geophys. Res. 105, 18675–18692, Keiling et al., 2003, Science 299, 383–386). Alfvén-wave-induced electron acceleration is shown to be confined in a rather narrow radial distance range of 4–5 R _E (Earth radii) and its importance, relative to other electron acceleration mechanisms, depends strongly on the magnetic disturbance level so that it represents 10% of all electron precipitation power during quiet conditions and increased to 40% during disturbed conditions. Our observations suggest that an electron Landau resonance mechanism operating in the “Alfvén resonosphere” is responsible for the energy transfer.     

人工辅助心脏用永磁轴承盘式无刷电机设计与研究

介绍了一种应用于人工辅助心脏的永磁轴承无位置传感器盘式无刷直流电动机的结构与电磁场仿真计算方法及结果,并对其温度场进行仿真计算。该电机体积重量小,无机械轴承,避免了对血液的破坏,且运行安全可靠。     

MSMA振动发电机的建模与仿真

振动发电就是利用电磁感应、压电技术、智能材料等将外部的机械振动能量通过一定装置转换成电能,实现机械振动能量和电能的转换.在分析磁控形状记忆合金（Magnetic Shape MemoryAlloy,简称MSMA）振动发电原理的基础上,利用MSMA智能材料的维拉利效应对振动能量进行收集,建立了MSMA振动发电机的数学模型,求出振动发电机感应电动势与压应力及外加磁场的数学关系.分析了振动应力幅值、频率的响应特性,仿真结果验证了MSMA振动发电的可行性.