串联磁路混合励磁爪极发电机的研究(英文)

针对电励磁爪极发电机效率低、永磁爪极发电机磁场调节困难的问题,提出了一种串联磁路混合励磁爪极同步发电机,利用磁路计算方法和三维有限元的分析研究了这种新型电机各部分的磁密大小,确定了合适的极对数和合理的磁钢厚度,探讨了这种新型电机的空载特性、外特性和调节特性.研究表明:串联磁路混合励磁爪极发电机合适的极对数为2,且磁钢厚度存在一个较为合理的优化值.相对于电励磁爪极发电机,它实现了励磁电流的双向控制;相对于永磁爪极发电机它使得输出电压可调,在更宽的负载范围内实现了输出电压的恒定.在参数相同的情况下,与电励磁爪极发电机相比,该电机具有更高的气隙磁密和功率密度.     

石墨-熔盐反应堆堆芯中子通量与钍铀转换比

作为获国际认可的第四代核电站反应堆堆型之一的熔盐堆(Molten salt reactor,MSR),具有固有安全性高、经济性好、核资源可持续发展以及易于防止核扩散等优点。针对石墨-熔盐零功率堆的几何参数,利用蒙特卡罗计算程序MCNP5建立了物理计算模型,计算临界情况下堆芯径向、轴向中子通量及增殖区厚度与Th-U转换比(Conversion ratio,CR)的关系。结果表明,(1)石墨-熔盐零功率堆堆芯中子通量密度分布较为平坦;(2)石墨-熔盐零功率堆反射层厚度和增殖区厚度在一定范围内,CR随反射层厚度或增殖区厚度的增加而增加,当超出该范围,CR不再随反射层厚度或增殖区厚度的增加而明显增加。     

纳米硫化物半导体颜料的制备及其红外发射率研究

为了制备出在8～14μm红外波段具有较低红外发射率的颜料粉体，本文以醋酸镉Cd(AC)2．2H2O，醋酸锌Zn(AC)2．2H2O，硫化钠Na2S．2H2O为原料，采用化学均匀沉淀法在水浴中制备了平均粒径40nm左右的CdZnS固溶体纳米粒子。分析了实验反应过程中反应时间、反应温度和搅拌速度对CdZnS纳米粒子半径尺寸的影响。通过XRD，BET(ASAT2010)比表面仪和TEM表征，研究了粉体的粒度、结构和表面形貌等特征；通过IR-1红外发射率测量仪器测试了粉体在8～14μm波段的红外发射率。作者着重讨论了粉体粒径和8～14μm波段红外发射率之间的关系。并对此给出了一定的解释。     

基于Bancroft算法的GPS动态定位非线性滤波法

由于系统线性化时存在忽略项,扩展卡尔曼滤波成为一种次优的梯度下降算法.当滤波方程病态时,求解存在发散倾向,且估计量为有偏的,而非最优估计.即使动态系统噪声为高斯噪声时,残差也不是高斯噪声.在伪距定位中,由于线性化后的伪距方程是局部解,这有可能丢失正确解值.针对GPS动态导航扩展卡尔曼滤波定位问题,基于美国Bancroft的全局性非线性"闭合式求解"最小二乘算法(Bancroft算法),本文提出一种闭合式GPS非线性代数解的卡尔曼滤波法(两步算法).该方法将GPS滤波问题中的空间与时间分离,较好地解决了非线性GPS动态定位求解问题,且获得稳定可靠的动态定位解.     

一种磁载光催化剂的制备及光催化活性的研究

采用溶胶-凝胶法,在磁性颗粒表面包覆T iO2,制备了易于固液分离的纳米级磁载光催化剂T iO2/S iO2/F e3O4,并通过TEM,IR,XRD等对样品进行表征。以有机污水为降解对象,研究了磁载光催化剂的光催化活性。研究结果表明,包覆S iO2有利于提高磁载光催化剂的光催化活性,光催化剂能使有机污水快速降解,5次循环使用后降解率达90%以上,且光催化剂能快速地从液相中分离回收。同时磁载光催化剂具有较高的光催化活性,对高盐污水、含酚污水的降解率分别可达到99%,86.8%,对染料污水也有良好的降解效果,并具有磁性回收的特点,应用前景广泛。     

模型机匣的包容性试验和数值模拟

为了解叶片断开撞击机匣的过程,研究航空发动机机匣包容性设计方法,在旋转试验器上进行了不同模型机匣的包容性试验,得到了叶片断开甩出时的转速、断叶撞击机匣的应变响应和断叶撞击机匣过程的高速摄影照片。试验结果表明:断叶与机匣碰撞两次,机匣破坏发生在第2次撞击,机匣的失效模式为剪切和拉伸失效。采用基于冲击动力学理论的有限元数值分析方法模拟了试验过程,反映了撞击过程中断叶的能量变化历程,较好地模拟了试验结果。     

导管螺旋桨内流场的PIV测量

内流场对于导管螺旋桨的设计和性能分析是至关重要的,利用随车式PIV在中国船舶科学研究中心拖曳水池进行了导管螺旋桨的内流场测量.使用标靶技术建立了物像对应关系,从而修正导管曲率和厚度产生的图象畸变.使用同步控制器实现螺旋桨相位、CCD摄像和激光器的精确同步控制.试验分别在三个不同进速系数J=1.2,1.0 和0.8下进行.试验结果很好地反映了螺旋桨梢涡、毂部涡、以及螺旋桨上下表面脱落的旋向相反的尾涡,以及近导管内壁、桨毂壁面涡层等流动特征.试验表明,涡强都随着进速系数的减小而增加.与螺旋桨前流动相比,导管内螺旋桨后轴向速度沿径向分布的不均匀性明显增强.试验结果表明,对于导管厚度与曲率都空间变化的导管螺旋桨,应用PIV技术进行内流场测量在技术上是可行的.     

Slow Solar Wind: Observations and Modeling

While it is certain that the fast solar wind originates from coronal holes, where and how the slow solar wind (SSW) is formed remains an outstanding question in solar physics even in the post-SOHO era. The quest for the SSW origin forms a major objective for the planned future missions such as the Solar Orbiter and Solar Probe Plus. Nonetheless, results from spacecraft data, combined with theoretical modeling, have helped to investigate many aspects of the SSW. Fundamental physical properties of the coronal plasma have been derived from spectroscopic and imaging remote-sensing data and in situ data, and these results have provided crucial insights for a deeper understanding of the origin and acceleration of the SSW. Advanced models of the SSW in coronal streamers and other structures have been developed using 3D MHD and multi-fluid equations.However, the following questions remain open: What are the source regions and their contributions to the SSW? What is the role of the magnetic topology in the corona for the origin, acceleration and energy deposition of the SSW? What are the possible acceleration and heating mechanisms for the SSW? The aim of this review is to present insights on the SSW origin and formation gathered from the discussions at the International Space Science Institute (ISSI) by the Team entitled “Slow solar wind sources and acceleration mechanisms in the corona” held in Bern (Switzerland) in March 2014 and 2015.     

Book reviews

The general significance of streamers of the solar corona is discussed in the frame of our knowledge of the solar wind phenomenon and the large-scale solar magnetic structure. Thermodynamical and geometric parameters of streamers observed and measured at total solar eclipses are reviewed. Both the low part (in the form of a helmet with a cusp) and the external part (in the form of a stalk extended at many solar radii) are considered. The modelling of streamers starts with the analysis of effects produced by the solar wind flow on a magnetic structure. Facts and arguments are presented in favor of a model with a current sheet and reconnection processes going on along the axis of the streamer, especially in the non-collisional part of the radially extended streamer. Further development of the Pneuman and Kopp (1971) model is discussed, including difficulties occurring in the interpretation of a stationary solution. An empirical model satisfying observations is presented. Future researchs on streamers were discussed with emphasis on observations to be done with the space-borne coronagraphs on the SOHO spacecraft.