基于模块度的复杂网络社团结构聚类新算法

针对传统的分裂聚类算法删除连边会影响节点划分的问题,结合K-means算法的思想并加以改进,提出了一种以邻居节点为聚类备选集,所有社团中心节点同时聚类的同步聚类算法。该算法根据节点中心度和最短路变化率确定社团中心节点集,然后以中心节点为社团中心,以邻居节点为聚类备选集合进行聚类,完成社团的划分。将算法应用到Zachary网络中并与GN算法、Top Leader算法进行比较,仿真结果表明该算法对网络有较好的划分。     

基于我国深空站三向测量模式的数据精度分析

为了验证我国深空站三向测量模式的正确性,以同步星跟踪试验中的测量数据为基础,建立了站间同步修正算法和三向测量观测模型,通过与同步卫星的精密星历反算测量值比较,得到了测量数据的标定参数,结果表明,我国深空站测控能够实现dm级的测量精度,明显优于“嫦娥二号”测量的水平;同时利用测量数据进行定轨策略分析,最终实现了10 m量级的同步卫星定轨精度.分析结果为“嫦娥三号”探测器实施有效测控提供了依据.     

Multi-h CPM遥测信号的定时频率联合估计技术

针对Multi-h CPM（Multi-h Continue Phase Modulation,多指数连续相位调制）遥测接收机的符号定时和载波频率同步问题,在分析MLSD（Maximum-likelihood Sequence Detection,最大似然序列检测）度量值是符号定时偏差和频率偏差的凸函数的基础上,提出一种基于迟/早门和升/降频门的符号定时和频率同步联合估计算法,通过似然值比较,对符号定时偏差和频率偏差进行迭代估计;并对该算法进行仿真,得到不同参数下的同步性能,给出同步参数选择建议.仿真结果表明：将该算法应用到Multi-h CPM遥测系统中,可实现低信噪比信号的快捕和高精度同步.     

无线传感器网络时间同步协议动态切换机制

针对当前无线传感器网络时间同步协议通用性差的问题,提出了基于主动编程思想的时间同步协议动态切换机制,设计了能够动态适配的时间同步协议切换框架,重点讨论了节点间相互通信、时间戳标记、协议切换、本地时间与全局时间的转换等4个关键问题,并且在TinyOS（Tiny Operating System,微操作系统）平台上对新机制进行了仿真验证,比较了新机制同2种主流时间同步协议之间的性能差异.仿真结果表明：新机制能实现时间同步协议的动态配置,提高协同效率,节省切换开销,具有良好的应用前景.     

基于滑模自适应控制的不确定混沌系统修正函数投影同步

研究了一类不确定混沌系统的修正函数投影同步。首先,设计了一类滑模曲面;基于该曲面设计了同步控制器,并采用自适应技术设计了自适应律对不确定参数进行逼近。在一定条件下,该同步控制方案可以实现2个不确定异结构混沌系统的修正函数投影同步。然后,为保证合适的控制量,对控制增益进行了优化。从同步效果来看,所设计的控制器对混沌系统的不确定项的影响具有较强的鲁棒性。最后,数值仿真验证了该控制器的有效性和可行性。     

Dynamics of Coronal Loop Oscillations Recent Improvements and Computational Aspects

We will discuss the observed, heavily damped transversal oscillations of coronal loops. These oscillations are often modeled as transversal kink oscillations in a cylinder. Several features are added to the classical cylindrical model. In our models we include loop curvature, longitudinal density stratification, and highly inhomogeneous radial density profiles. In this paper, we will first give an overview of recently obtained results, both analytically and numerically. After that, we shed a light on the computational aspects of the modeling process. In particular, we will focus on the parallellization of the numerical codes.     

Spartan 201 white light coronagraph experiment

A white light coronagraph was launched into orbit aboard the space shuttle OV 103 (Discovery) on 7 April 1993. This device was one of two instruments included in the SPARTAN 201-1 payload, a completely autonomous sub-satellite deployed from the shuttle for a period of about 47 hours. The WLC system is an externally occulted coronagraph system which incorporates a rotating half-wave plate polarimeter, and the image data is used to infer the brightness, the polarized brightness and the degree of polarization of the white light emission from the solar corona. These data are in turn used to infer estimates of the K- and F-coronal brightnesses and density distributions. We shall present preliminary results of the electron density estimate in the coronal streamer and hole region and describe the methods employed.affiliated to USRA     

Radial profile measurements of the solar wind speed using radio sounding techniques

Velocity measurements of the solar wind in the region of its acceleration were carried out in 1984 with Venera Orbiters using the following specific radio sounding techniques: (i) phase and frequency correlations from two or three widely-spaced ground stations; (ii) phase and frequency correlations from two spacecraft and two widely-spaced ground stations; (iii) two station two-way coherent Doppler measurements; (iv) determination of the break frequency in power spectra of intensity fluctuations. Our results are substantially lower than those derived from direct Doppler shift measurements of transition region and lower coronal resonance lines and those from measurements applying the Doppler dimming technique.     

Probing solar and stellar interior dynamics and dynamo

Solar and stellar activity is a result of complex interaction between magnetic field, turbulent convection and differential rotation in a star’s interior. Magnetic field is believed to be generated by a dynamo process in the convection zone. It emerges on the surface forming sunspots and starspots. Localization of the magnetic spots and their evolution with the activity cycle is determined by large-scale interior flows. Thus, the internal dynamics of the Sun and other stars hold the key to understanding the dynamo mechanism and activity cycles. Recently, significant progress has been made for modeling magnetohydrodynamics of the stellar interiors and probing the internal rotation and large-scale dynamics of the Sun by helioseismology. Also, asteroseismology is beginning to probe interiors of distant stars. I review key achievements and challenges in our quest to understand the basic mechanisms of solar and stellar activity.     

The Seed Population for Energetic Particles Accelerated by CME-Driven Shocks

Understanding properties of solar energetic particle (SEP) events associated with coronal mass ejections has been identified as a key problem in solar-terrestrial physics. Although recent CME shock acceleration models are highly promising, detailed agreement between theoretical predictions and observations has remained elusive. Recent observations from ACE have shown substantial enrichments in the abundances of ³He and He⁺ ions which are extremely rare in the thermal solar wind plasma. Consequently, these ions act as tracers of their source material, i.e., ³He ions are flare suprathermals and He⁺ ions are interstellar pickup ions. The average heavy ion composition also exhibits unsystematic differences when compared with the solar wind values, but correlates significantly with the ambient suprathermal material abundances. Taken together these results provide compelling evidence that CME-driven shocks draw their source material from the ubiquitous but largely unexplored suprathermal tail rather than from the more abundant solar wind peak. However, the suprathermal energy regime has many more contributors and exhibits much larger variability than the solar wind, and as such needs to be investigated more thoroughly. Answers to fundamental new questions regarding the preferred injection of the suprathermal ions, the spatial and temporal dependence of the various sources, and the causes of their variability and their effects on the SEP properties are needed to improve agreement between the simulations and observations.