圆度误差的一种微机图像测量法

将圆度误差测量的影像法与最小二乘圆法相结合，利用多媒体图像处理技术，设计了一种圆度误差的微机自动测量系统，实现了非接触、远距离快速测量，提高了测量精确度，为某些特殊工件的测量提供了一套实用的测量方法。     

可展开式辐射器热控对航天器轨道调整的适应性分析

为提高航天器热控系统对轨道调整的适应能力，本文研究了与流体回路耦合的可展开式辐射器热控方案在不同轨道高度下的热控性能，分析了不同轨道高度时辐射器面临的热环境的影响，在不同轨道高度下比较了固定辐射器与可展开辐射器的热控特性。结果表明，随着辐射器展开角度的变化，辐射器吸收的空间热流随之发生变化，从而对热控系统的散热能力带来直接影响，调节辐射器的角度可以扩大其对外散热能力。在工程应用中，基于热控流体回路，通过调节可展开式辐射器的展开角度，可以有效提高航天器的轨道热适应能力。     

显微镜采集图象的自动化

介绍了一种利用ＰＣ机与单片机通讯控制显微镜载物平台作三维运动从而实现了自动搜索视场，自动聚焦的方法，文中较详细地介绍了作为自动采集系统前台控制和驱动部分的单片机系统的硬，软件结构，以及作为上位机的ＰＣ机的控制策略和软件流程，由于采用了微机技术并配以精密的机械传动机构，使得对数据的获取和分析快速，准确，克服了手动调节动作慢，误差大等问题，为以后进一步对图象信息进行分析处理提供了便利。     

一种计算二维图象矩的神经网络方法

提出一种计算二维图象矩的神经网络方法，首先，导出一维信号矩与一维Ｈａｄａｍａｒｄ变换之间的关系。通过２Ｎ－一维Ｈａｄａｍａｒｄ变换和极少量加法，移位及乘法运行可计算二维图象矩。然后给出用Ｔａｎｋ－Ｈｏｐｆｉｅｌｄ神经网络实现Ｈａｄａｍａｒｄ变换的方法，并对该网络作了改进。     

Crew autonomy for deep space exploration: Lessons from the Antarctic Search for Meteorites

Future piloted missions to explore asteroids, Mars, and other targets beyond the Moon will experience strict limitations on communication between vehicles in space and control centers on Earth. These limitations will require crews to operate with greater autonomy than any past space mission has demonstrated. The Antarctic Search for Meteorites (ANSMET) project, which regularly sends small teams of researchers to remote parts of the southern continent, resembles a space mission in many ways but does not rely upon a control center. It provides a useful crew autonomy model for planners of future deep space exploration missions. In contrast to current space missions, ANSMET gives the crew the authority to adjust competing work priorities, task assignments, and daily schedules; allows the crew to be the primary monitor of mission progress; demands greater crew accountability for operational errors; requires the crew to make the most of limited communication bandwidth; adopts systems designed for simple operation and failure recovery; and grants the crew a leading role in the selection and stowage of their equipment.     

Solar Sources of Heliospheric Energetic Electron Events—Shocks or Flares?

Electrons with near-relativistic (E≳30 keV, NrR) and relativistic (E≳0.3 MeV) energies are often observed as discrete events in the inner heliosphere following solar transient activity. Several acceleration mechanisms have been proposed for the production of those electrons. One candidate is acceleration at MHD shocks driven by coronal mass ejections (CMEs) with speeds ≳1000 km s⁻¹. Many NrR electron events are temporally associated only with flares while others are associated with flares as well as with CMEs or with radio type II shock waves. Since CME onsets and associated flares are roughly simultaneous, distinguishing the sources of electron events is a serious challenge. On a phenomenological basis two classes of solar electron events were known several decades ago, but recent observations have presented a more complex picture. We review early and recent observational results to deduce different electron event classes and their viable acceleration mechanisms, defined broadly as shocks versus flares. The NrR and relativistic electrons are treated separately. Topics covered are: solar electron injection delays from flare impulsive phases; comparisons of electron intensities and spectra with flares, CMEs and accompanying solar energetic proton (SEP) events; multiple spacecraft observations; two-phase electron events; coronal flares; shock-associated (SA) events; electron spectral invariance; and solar electron intensity size distributions. This evidence suggests that CME-driven shocks are statistically the dominant acceleration mechanism of relativistic events, but most NrR electron events result from flares. Determining the solar origin of a given NrR or relativistic electron event remains a difficult proposition, and suggestions for future work are given.     

Non-Thermal Processes in Cosmological Simulations

Non-thermal components are key ingredients for understanding clusters of galaxies. In the hierarchical model of structure formation, shocks and large-scale turbulence are unavoidable in the cluster formation processes. Understanding the amplification and evolution of the magnetic field in galaxy clusters is necessary for modelling both the heat transport and the dissipative processes in the hot intra-cluster plasma. The acceleration, transport and interactions of non-thermal energetic particles are essential for modelling the observed emissions. Therefore, the inclusion of the non-thermal components will be mandatory for simulating accurately the global dynamical processes in clusters. In this review, we summarise the results obtained with the simulations of the formation of galaxy clusters which address the issues of shocks, magnetic field, cosmic ray particles and turbulence.     

BP网络进行0-9十个数字图像的识别

在BP算法和数字图像处理技术的基础上,本文在MATLAB软件环境下提取Word文档中26种字体的0-9十个数字的图像,使用MATLAB神经网络工具箱及图像处理工具箱进行数字的识别,给出了较详细的处理步骤及相关程序,并比较了各种识别算法的收敛速度和识别率。     

磁悬浮框架飞轮磁轴承技术研究与发展现状

对磁悬浮框架飞轮(MSGFW)和高精度磁轴承研究现状及其未来发展进行了详细阐述。根据转子悬浮力类型，将磁悬浮框架飞轮分为磁阻力构型、洛伦兹力构型和混合力构型，并结合三种构型论述了国内外框架飞轮的发展过程。在此基础上，对球面磁阻力磁轴承和洛伦兹力磁轴承进行了详细介绍，并结合磁路图分析其工作原理，比较了同类磁轴承的优劣。展望了磁悬浮框架飞轮与高精度磁轴承的未来发展方向，指出高动态响应检控共位平动球面磁阻力磁轴承，标准磁悬浮动量球和磁悬浮控制敏感球是磁悬浮框架飞轮的研究重点。     

Evolution of the periodicities in 2S 0114+650

We have analysed 9 years of data from the All Sky Monitor on the Rossi X-ray Timing Explorer for 2S 0114+650 to study the evolution of its spin, binary, and super-orbital periods. The spin history of the neutron star in this system exhibits torque reversals lasting 1 year. The newly discovered super-orbital period has remained stable over the 9-year span, making 2S 0114+650 the fourth known system to exhibit stable super-orbital modulation. We compare its super-orbital period evolution with those of the other three such systems.