CC—高阶通信系统的并发演算

并发演算CC(Concurrent Calculus)是高阶并发通信系统的数学模型,它把λ-演算作为子理论并包含一阶通信系统演算CCS、活动进程演算CMP、和高阶通信系统演算CHOCS的主要特征。在CC中,通信端口可为任意表达式并且进程和通信端口都可以作为在通信中传递的一等对象(First-class Objects)。从而CC不仅可以描述一阶通信行为而且可以刻划通信网络的动态自修改行为。另外,由于CC把λ-演算和进程演算纳入同一形式系统,故CC可以作为并发函数式程序设计的核心语言和理论模型。本文首先给出CC的语法、语义和例子,然后研究CC的高阶双向模拟等价关系以及CC的代数定律。最后简单讨论了相关的工作和今后的研究方向。     

湿度换算软件包

湿度不论是在科研领域还是在工业生产中，都是一个很重要的参量指标，在具体的应用中，各领域对湿度参量的使用单位和范围要求是不同的，由此我们编写了一套“湿度换算软件包”，可以在湿度的不同参量和单位间进行换算。本文主要介绍了该软件的主要功能、使用说明以及同国外其它同类软件的数据比对情况。     

rom 15 sel

with primary goat embryonic fibroblast showed no difference from traditional feederlayer-based culture method used in mouse and human. The putative primary EG colonies were multilayer clumps ofcompact cel     

微重力科学与应用研究（上）

空间微重力环境的独特物理现象对航天器各系统均产生无法回避的影响，在型号研制中正确计入微重力效应是航天事业发展中的一个重要研究领域。在现阶段，航天器发动机再启动相关的微重力研究以及载人航天防火安全相关的微重力研究应当引起人们的高度重视。随航天事业的发展，微重力效应问题日益会严重起来（结构动力学、耦合动力学、多相流温控、低重星球场着陆撞击……），进行深入广泛的微重力效应研究对保证航天器飞行任务完成有着不应忽视的作用     

数学教学中培养创造能力的探索

本文结合多年教学实践，对激发学生的创造意识，培养发散思维，运用创造技法等方面进行了探索。     

计算机帧时间对半实物仿真的影响

半实物仿真试验中,要求计算机帧时间与计算积分步长相一致,但在实际试验中不容易精确地做到。本文分析了这种不一致给半实物仿真试验带来的影响,给出了解决的办法,文章中还给出了一实例来说明。     

Field formation around negatively biased solar arrays in the LEO-plasma

Heavy emission caused by impacting plasma ions results in a fast discharging effect of the initially large surface potentials on the dielectric solar cells. This eventually counteracts the energization process of the plasma ions to the cover glasses and leaves no significant electric fields. Thus, with an existing thermal plasma, electrons are again able to reach dielectric surfaces. Strong localized electric fields of the order of several 10 kV/cm form near the interconnector-cover glass interface.     

人体分层媒质内的微波聚焦场

本文是近年来在微波聚焦热疗人体深部癌病灶研究工作推动下完成的。文中给出了光学及电磁学界感兴趣的某些结果。在人体分层媒质前的一有限口径处,置一时谐电流分布,在每一分层内的微波传输场及反射场可利用传输矩阵及并矢格林函数给出计算结果。     

The Electron Radiation Belt

Electron radiation belts can change dramatically in a few seconds or slowly over years. Important issues in understanding such changes are: (1) What is the source of electrons in the radiation belts? (2) How important is radial diffusion compared to other radial transport mechanisms? (3) What are the detailed changes in the magnetosphere that produce radial diffusion? (4) Why is the response of the electron radiation belt to changes in the solar wind different from that of substorms and of the ring current? (5) Are processes other than radial transport, such as wave-particle interactions, important in energizing electrons in the radiation belts?     

EUV emission from normal galaxies

Using data from the Wide Field Camera EUV all-sky survey, we have established upper limits to the EUV flux from a sample of 30 bright, nearby, non-active spiral galaxies. These galaxies were chosen to be those most likely to be detected in the EUV on the basis of (i) low interstellar absorption within our own galaxy, (ii) brightness in other wavebands, (iii) high star formation activity, and (iv) proximity. The derived EUV upper limits are restrictive, and establish for the first time that the EUV flux escaping from galaxies does not constitute a major component of their bolometric luminosity, and in particular that it cannot be the sink for the energy injected into the interstellar medium by supernova explosions, as had been suggested following the failure to detect this power in the X-ray band.