线性回归模型的贝叶斯决策方法

决策影响图分析法是决策问题一种新的图示表征求解方法，它用无有向回路的有向图来表征决策信息的关系，运用这一决策分析的新方法，对一类线性回归模型，从决策的角度进行探讨和求解，并将结果推广到更加一般的情形。     

飞机机翼表面水滴撞击特性计算

根据飞机防冰系统的研制需要，以机翼为对象，对水滴撞击特性的数值计算进行研究，建立了计算模型，研究了计算方法，用相应的计算程序，在广泛的飞行，气象及多种翼型条件下，对水滴撞击特性作了计算，计算结果与国外权威机构公布的数据相比吻合性好，给出了部分计算结果，并对水滴撞击特性计算的应用作了简要分析。     

高速可编程PCM遥测帧同步器

依据国际最新测地面站的发展方向，给出了一种新型高码率可编程ＰＣＭ遥测帧同步器的方案设计，既采用了高速可编程全数字化相关检测技术及新颖的滑动窗口技术，又采用了状态机变量设计和微程序设计，并基于ＰＬＤ技术，完成了整个高速可编程ＰＣＭ遥测帧同步器的软、硬件设计、实验表明，该方案切实可行。     

图形点阵式液晶显示器MGLS-160128在智能化仪表中的应用

本文介绍了图形点阵式液晶显示器MGLS－160128在实际测量中硬件连接和软件设计思想。具有较强的实用价值。     

基于MATLAB的自动控制系统仿真与分析

本文在给出机器人行走系统的数学模型的基础上，利用 MATLAB对控制系统进行仿真，同时详细地分析了控制系统，给出了系统的时域性能指标、开环频率特性及根轨迹，说明了系统设计的有效性。     

精密车削细长轴的几点措施

本文针对长径比大于80：1的细长轴精密加工问题，从车刀角度、车削方法、车床尾座、跟刀架等方面提出了改进措施，从而满足了加工要求，提高了生产效率。     

“Oblique” Bernstein modes in solar preflare plasma: Generation of second harmonics

Process of second harmonics generation due to development of corresponding instability has been investigated for pure electron weakly oblique Bernstein mode. This mode was supposed to be modified by taking into account the influence of pair Coulomb collisions and weak large-scale electric field in flare loop. Investigated area was located near the loop foot-point in the “lower–middle” chromosphere of active region. It has been shown, that for the Fontenla–Avrett–Loeser model of solar atmosphere the investigated process of second harmonics generation starts at the extremely low threshold values of subdreicer electric field, well before the beginning of “preheating” phase of flare process.     

Space and velocity distributions of neutron stars in the Milky Way

We study the long term dynamics of isolated neutron stars (NSs) for different initial conditions. From the resulting phase-space distributions, we estimate the fraction of NSs bound to the Milky Way. We also estimate the surface and spatial density of NSs in the solar neighborhood and the mean velocity of NSs in the Galactic disk. Estimates of the sky density of NSs towards specific lines of sight, i.e. the Galactic center and the Magellanic Clouds, are also given.     

Three-dimensional global simulation of multiple ICMEs’ interaction and propagation from the Sun to the heliosphere following the 25–28 October 2003 solar events

This study performs simulations of interplanetary coronal mass ejection (ICME) propagation in a realistic three-dimensional (3D) solar wind structure from the Sun to the Earth by using the newly developed hybrid code, HAFv.2+3DMHD. This model combines two simulation codes, Hakamada–Akasofu–Fry code version 2 (HAFv.2) and a fully 3D, time-dependent MHD simulation code. The solar wind structure is simulated out to 0.08 AU (18 Rs) from source surface maps using the HAFv.2 code. The outputs at 0.08 AU are then used to provide inputs for the lower boundary, at that location, of the 3D MHD code to calculate solar wind and its evolution to 1 AU and beyond. A dynamic disturbance, mimicking a particular flare’s energy output, is delivered to this non-uniform structure to model the evolution and interplanetary propagation of ICMEs (including their shocks). We then show the interaction between two ICMEs and the dynamic process during the overtaking of one shock by the other. The results show that both CMEs and heliosphere current sheet/plasma sheet were deformed by interacting with each other.