基于LabVIEW的通信系统的构建

本设计基于LabVIEW仿真软件完成了基本通信系统和通信综合系统的构建。该系统涵盖了模拟调制,数字调制,模拟信号数字传输,信道编码,最佳接收系统几部分内容。通过系统仿真,实现了系统输入输出波形的直观显示,解决了教学中实验效果不理想,理论内容不好理解的问题。同时通过内置的Web Server进行网页发布后,用户可以在客户...     

数字多媒体音频新技术的发展研究——MPEG标准音频编码系统

声音信号的存储与传输,从模拟信号到数字信号经历了迅速的发展。随着多媒体处理技术的发展,数字音频压缩编码技术得到了广泛的应用。运动图像专家组—MPEG（Moving Picture Expert Group）,该组织自1988年以来制定了一系列国际标准,其中MPEG-1、MPEG-2已为人们所熟知。从1999年开始,他们...     

廊坊市体育健身娱乐市场现状调查与对策分析

本文采用问卷调查、文献资料、观察、数理统计、逻辑分析等研究方法,对廊坊市体育健身娱乐经营单位的基本情况、经营状况和居民体育健身娱乐消费情况进行了调查研究,揭示了市场供求的现状特征及存在的问题,并据此提出了拓展廊坊市体育健身娱乐市场的若干对策.     

Determination of station positions and velocities from laser ranging observations to Ajisai,Starlette and Stella satellites

The positions and velocities of the four Satellite Laser Ranging (SLR) stations: Yarragadee (7090), Greenbelt (7105), Graz (7839) and Herstmonceux (7840) from 5-year (2001–2005) SLR data of low orbiting satellites (LEO): Ajisai, Starlette and Stella were determined. The orbits of these satellites were computed from the data provided by 20 SLR stations. All orbital computations were performed by means of NASA Goddard’s GEODYN-II program. The geocentric coordinates were transformed to the topocentric North–South, East–West and Vertical components in reference to ITRF2005. The influence of the number of normal points per orbital arc and the empirical acceleration coefficients on the quality of station coordinates was studied. To get standard deviation of the coordinates determination lower than 1 cm, the number of the normal points per site had to be greater than 50. The computed positions and velocities were compared to those derived from LAGEOS-1/LAGEOS-2 data. Three parameters were used for this comparison: station coordinates stability, differences from ITRF2005 positions and velocities. The stability of coordinates of LEO satellites is significantly worse (17.8 mm) than those of LAGEOS (7.6 mm), the better results are for Ajisai (15.4 mm) than for Starlette/Stella (20.4 mm). The difference in positions between the computed values and ITRF2005 were little bit worse for Starlette/Stella (6.6 mm) than for LAGEOS (4.6 mm), the results for Ajisai were five times worse (29.7 mm) probably due to center of mass correction of this satellite. The station velocities with some exceptions were on the same level (≈1 mm/year) for all satellites. The results presented in this work show that results from Starlette/Stella are better than those from Ajisai for station coordinates determination. We can applied the data from LEO satellites, especially Starlette and Stella for determination of the SLR station coordinates but with two times lower accuracy than when using LAGEOS data.     

ASTROSAT

The ASTROSAT satellite is an Indian National Space Observatory under development in India. Due for launch in 2010, ASTROSAT will carry a complement of five scientific instruments enabling simultaneous observations from the optical through to the hard X-ray energy band. This capability will enable broad-band spectroscopy and high time-resolution monitoring of both galactic and extra-galactic targets, such as X-ray binaries and AGN. One of the instruments is being built in collaboration with the Canadian Space Agency and another in collaboration with the University of Leicester. ASTROSAT also carries a scanning sky monitor to observe the variable X-ray sky. After an initial period of science verification and guaranteed time, a certain fraction of ASTROSAT observing time will also be made available to the community via a call for proposals. Here I summarise the instrument complement and principle scientific objectives of the mission.     

Evolution of periodic orbits near the Lagrangian point L2

A study of the evolution of the periodic and the quasi-periodic orbits near the Lagrangian point L₂, which is located to the right of the smaller primary on the line joining the primaries and whose distance from the more massive primary is greater than the distance between the primaries, in the framework of restricted three-body problem for the Sun–Jupiter, Earth–Moon (relatively large mass ratio) and Saturn–Titan (relatively small mass ratio) systems is made. Two families of periodic orbits around the smaller primary are identified using the Poincaré surface of section method – family I (initially elliptical, gradually becomes egg-shaped with the increase in the Jacobi constant C and elongated towards the more massive primary) and family II (initially egg-shaped orbits elongated towards L₂ and gradually becomes elliptical with the increase in C). The family I in the Sun–Jupiter and Saturn–Titan systems contains two separatrix caused by third-order and fourth-order resonances, while the Earth–Moon system has only one separatrix which is caused by third-order resonances. Also in the Sun–Jupiter and the Saturn–Titan systems, family I merge with family II, around Jacobian constant 3.0393 and 3.0163, respectively, while in the Earth–Moon system, family II evolves separately from two different branches. The two branches merge at C = 3.184515. In the Earth–Moon system, the family II contains a separatrix due to third-order resonances which is absent in the other two systems.     

A null frame for spacetime positioning by means of pulsating sources

We introduce an operational approach to the use of pulsating sources, located at spatial infinity, for defining a relativistic positioning and navigation system, based on the use of four-dimensional bases of null four-vectors, in flat spacetime. As a prototypical case, we show how pulsars can be used to define such a positioning system. The reception of the pulses for a set of different sources whose positions in the sky and periods are assumed to be known allows the determination of the user’s coordinates and spacetime trajectory, in the reference frame where the sources are at rest. We describe our approach in flat Minkowski spacetime, and discuss the validity of this and other approximations we have considered.     

Comparison of peak characteristics of F2 ionospheric layer over Tehran region at a low solar activity period with IRI-2001 and IRI-2007 models predictions

In the present work values of peak electron density (NmF2) and height of F2 ionospheric layer (hmF2) over Tehran region at a low solar activity period are compared with the predictions of the International Reference Ionosphere models (IRI-2001 and IRI-2007). Data measured by a digital ionosonde at the ionospheric station of the Institute of Geophysics, University of Tehran from July 2006 to June 2007 are used to perform the calculations. Formulations proposed by  and  are utilized to calculate the hmF2. The International Union of Radio Science (URSI) and International Radio Consultative Committee (CCIR) options are employed to run the IRI-2001 and IRI-2007 models. Results show that both IRI-2007 and IRI-2001 can successfully predict the NmF2 and hmF2 over Tehran region. In addition, the study shows that predictions of IRI-2007 model with CCIR coefficient has closer values to the observations. Furthermore, it is found that the monthly average of the percentage deviation between the IRI models predictions and the values of hmF2 and NmF2 parameters are less than 10% and 21%, respectively.     

基于DSPN的航天测控系统任务可靠性仿真建模

提出了基于确定与随机Petri网（deterministic and stochastic Petri nets,DSPN）的航天测控系统（tracking,telemetry and command,TT&C）任务可靠性定量分析方法,旨在对相关航天测控方案进行可靠性预计.通过对TT&C系统任务剖面进行时序弧段划分,考虑实际系统中测控单元阶段依赖、单元故障可修以及各单元参与任务起止时间不同等其他建模方法难以处理的复杂因素,建立了“单元层-系统逻辑层-阶段层”3层相互关联的TT&C系统任务可靠性DSPN模型.通过对模型仿真运行,实现了对给定测控方案下TT&C系统任务可靠性定量化评估.分析表明:仿真结果随着仿真次数增加逐渐收敛,与Markov解析方法求得的精确值对比误差控制在1%以内.      

作为企业组织形式的信托

在信托作为企业组织形式的发展过程中,有两个问题值得关注：一是为什么信托能够作为企业的组织形式;二是信托作为企业组织形式经历了由盛而衰,然后再度崛起的过程,其背后的原因是什么？以法经济学的视角观察会发现,信托与公司在资产分割及其所导致的债权人模式上是没有区别的,这奠定了信托作为企业形式的基础;而以企业理论观察,就会发现信托与公司在企业所有权安排上的不同,即信托将控制权安排给了人力资本所有者,而公司则是将控制权安排给了非人力资本,这一不同导致了两者在治理结构与应用范围上的差别。