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。     

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。     

星载宽测绘带合成孔径雷达成象处理

波束扫描合成孔径雷达是为了满足星载合成孔径雷达宽测绘的要求而提出的，本文主要研究ＳＣＡＮＳＡＲ成象处理。ＳＣＡＮＳＡＲ的工作原理、信号格式、信号结构和信号参数限制的深入分析是成象处理研究的基础，成象处理算法包括块数据成象算法和块图象拼接算法两部分，频谱分析法和时域频域混合相关法被用于块数据成象，块图象的拼接是利用时间关系剪裁块图象再顺次拼接，完整的计算机仿真验证了本文提出的ＳＣＡＮＳＡＲ信号格式和     

1990年7月30日太阳射电大爆发中的脉动现象

本文讨论了1990年7月30日伴随日面2B级双带光学耀斑发生的3.2cm波微波大爆发事件的观测特征,它呈现为显著的脉动形态。并对它进行了数据处理,发现射电爆发流量S与脉动的特征参量:平均重复率R,调制度△S/S和能量△E之间有良好的统计相关性。对此作了讨论和初步的解释。     

What is the role of magnetic null points in large flares?

We have performed the analysis of the magnetic topology of active region NOAA 10486 before two large flares occurring on October 26 and 28, 2003. The 3D extrapolation of the photospheric magnetic field shows the existence of magnetic null points when using two different methods. We use TRACE 1600 Å and 195 Å brightenings as tracers of the energy release due to magnetic reconnections. We conclude on the three following points:

1. The small events observed before the flares are related to low lying null points. They are long lasting and associated with low energy release. They are not triggering the large flares.

2. On October 26, a high altitude null point is found. We look for bright patches that could correspond to the signatures of coronal reconnection at the null point in TRACE 1600 Å images. However, such bright patches are not observed before the main flare, they are only observed after it.

3. On October 28, four ribbons are observed in TRACE images before the X17 flare. We interpret them as due to a magnetic breakout reconnection in a quadrupolar configuration. There is no magnetic null point related to these four ribbons, and this reconnection rather occurs at quasi-separatrix layers (QSLs).

We conclude that the existence of a null point in the corona is neither a sufficient nor a necessary condition to give rise to large flares.     

From solar nanoflares to stellar giant flares: Scaling laws and non-implications for coronal heating

In this study we explore physical scaling laws applied to solar nanoflares, microflares, and large flares, as well as to stellar giant flares. Solar flare phenomena exhibit a fractal volume scaling, V(L)  L^1.9, with L being the flare loop length scale, which explains the observed correlation between the total emission measure EM_p and flare peak temperature T_p in both solar and stellar flares. However, the detected stellar flares have higher emission measures EM_p than solar flares at the same flare peak temperature T_p, which can be explained by a higher electron density that is caused by shorter heating scale height ratios s_H/L ≈ 0.04–0.1. Using these scaling laws we calculate the total radiated flare energies E_X and thermal flare energies E_T and find that the total counts C are a good proxy for both parameters. Comparing the energies of solar and stellar flares we find that even the smallest observed stellar flares exceed the largest solar flares, and thus their observed frequency distributions are hypothetically affected by an upper cutoff caused by the maximum active region size limit. The powerlaw slopes fitted near the upper cutoff can then not reliably be extrapolated to the microflare regime to evaluate their contribution to coronal heating.     

中心频率为175MHz复合布拉格声光器件的设计

介绍以钼酸铅为声光介质、中心频率为１７５ＭＨｚ复合声光器件的设计，计算了以铟为粘合层时换能器带宽并确定了镀层厚度，该器件带宽为１２０ＭＨｚ，时间带宽积达１２０７．５，初步满足声光信号处理的需要。     

对称矩阵反问题解的稳定性

考虑如下对称矩阵反问题：问题Ⅰ：给定Ｘ，Ｂ∈Ｒ（ｎ×ｎ），求Ａ∈ＳＲ（ｎ×ｎ）使得ＡＸ＝Ｂ，其中ＳＲ（ｎ×ｎ）＝｛｛Ａ｜Ａ∈Ｒ（ｎ×ｎ），ＡＴ＝Ａ｝。问题Ⅱ：给定，求使得其中是矩阵的Ｆｒｏｂｅｎｉｕｓ范数，ＳＡ表示问题Ⅰ的解集合。本文讨论问题Ⅰ解的稳定性，给出问题Ⅱ解的扰动界。     

一维波动方程的小波解法

利用具有紧文集的Datubechies正交小波基函数，构造出了一种新的计算一维波动方程的数值方法——小波解法。由于该方法充分利用了Daubechies小波函数良好的局部性质，并且巧妙地运用了Fourier变换，数值试验表明该方法不但精度高，而且计算量小。     

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。