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。     

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。     

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.     

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     

Measurements of the 12C/13C Ratio in Planetary Nebulae and Implications for Stellar Evolution

We present the results of a study aimed at determining the 12C/13C ratio in two samples of planetary nebulae (PNe) by means of mm-wave observations of 12CO and 13CO. The first group includes six PNe which have been observed in the 3He+ hyperfine transition; the other group consists of 23 nebulae with rich molecular envelopes. We have determined the isotopic ratio in 14 objects and the results indicate a range of values between 9 and 23. In particular, three PNe have ratios well below the value predicted by standard evolutionary models ( 20), indicating that some extra-mixing process has occurred in these stars. We briefly discuss the implications of our results for standard and nonstandard stellar nucleosynthesis.     

Impact Cratering Theory and Modeling for the Deep Impact Mission: From Mission Planning to Data Analysis

The cratering event produced by the Deep Impact mission is a unique experimental opportunity, beyond the capability of Earth-based laboratories with regard to the impacting energy, target material, space environment, and extremely low-gravity field. Consequently, impact cratering theory and modeling play an important role in this mission, from initial inception to final data analysis. Experimentally derived impact cratering scaling laws provide us with our best estimates for the crater diameter, depth, and formation time: critical in the mission planning stage for producing the flight plan and instrument specifications. Cratering theory has strongly influenced the impactor design, producing a probe that should produce the largest possible crater on the surface of Tempel 1 under a wide range of scenarios. Numerical hydrocode modeling allows us to estimate the volume and thermodynamic characteristics of the material vaporized in the early stages of the impact. Hydrocode modeling will also aid us in understanding the observed crater excavation process, especially in the area of impacts into porous materials. Finally, experimentally derived ejecta scaling laws and modeling provide us with a means to predict and analyze the observed behavior of the material launched from the comet during crater excavation, and may provide us with a unique means of estimating the magnitude of the comet’s gravity field and by extension the mass and density of comet Tempel 1.     

Large scale structure of the universe

The current situation with the cosmological model and fundamental constants is briefly reviewed. Here, we concentrate on evolutionary effects of large-scale structure formation, in particular, the relationship with the quasar distribution and dynamics is discussed. We argue that groups of bright quasars with few or more than dozen of members within regions l _LS(100–150)h ^–1 Mpc found atz<2 may belong to concentrations of young rich clusters of galaxies, and thus be distant Great Attractors like the local GA or the Shapley concentration. These early large-scale galactic structures (i) provide a natural way to bias the distribution of Abell clusters, and (ii) suggest that the spectrum of primordial density perturbations is nearly flat on scales encompassing both the cluster and GAs,l=k ^–1(10,100)h ^–1 Mpc: _k ² k ³ P(k) k , =1 _–0.4 ^+0.6 , whereP(k) is the power spectrum of density perturbations.     

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。