总量控制与排污权交易的理论分析

本文从总量控制与排污权交易的概念出发，论述了排污权交易的基本理论和市场机制模型，分析了总量控制与排污权交易的经济、环境和社会效益，阐述了排污权的初始分配方式及交易方式。     

多架无人机协同航路规划方法研究

根据敌方防御区域内雷达，导弹等威胁阵地的具体分布情况，采用划分Voronoi多边形的方法制订初始航路，然后对初始航路进行了合理的离散处理，最后采用动态链类比法调整航路，航程并对航路进行光顺处理，提出了一种协调多架无人机（UAVs）于同一时间到达目标点的航路规划方法，用数字仿真技术对该方法进行了验证，结果表明该方法是可行的。     

针对变速机动目标的变速导弹三维导引律

应用李雅普诺夫稳定理论，提出一种三维制导算法，在算法设计中，既考虑了目标机动，包括目标速度的变化，又考虑了导弹速度的变化，为实现所提出的算法，进一步将与目标运动的加速度和速度方位信息的有关的项归为两项，给出了其估计方法，仿真结果验证了该方法的有效性。     

机动目标三维空间导引运动建模及导引律研究

给出了导弹—目标追逃运动的空间矢量方程，在此基础上推导了三维导引运动模型。对机动目标应用李雅普诺夫稳定性分析方法提出了一种自适应变结构制导算法。六自由度数学仿真结果表明了模型的正确性和制导算法的有效性。     

Coronal fast wave trains of the decimetric type IV radio event observed during the decay phase of the June 6, 2000 flare

The 22 min long decimetric type IV radio event observed during the decay phase of the June 6, 2000 flare simultaneously by the Brazilian Solar Spectroscope (BSS) and the Ond?ejov radiospectrograph in frequency range 1200–4500 MHz has been analyzed. We have found that the characteristic periods of about 60 s belong to the long-period spectral component of the fast wave trains with a tadpole pattern in their wavelet power spectra. We have detected these trains in the whole frequency range 1200–4500 MHz. The behavior of individual wave trains at lower frequencies is different from that at higher frequencies. These individual wave trains have some common as well as different properties. In this paper, we focus on two examples of wave trains in a loop segment and the main statistical parameters in their wavelet power and global spectra are studied and discussed.     

一种改进的多目标粒子群优化算法

为了增强多目标粒子群优化算法的收敛性与多样性,提出一种改进的多目标粒子群算法.采用Kent映射对种群进行初始化,并将目标空间均匀划分为若干扇形区域;基于一种新的多样性和收敛性判定标准,选取合适的收敛性最优解和多样性最优解,并提出一种改进的粒子群更新公式进行全局搜索;采用聚类算法对外部种群与坐标轴夹角进行分析,维护外部种群.通过标准测试函数的仿真实验,与多目标优化算法基本MOPSO(Multi-objective Particle Swarm Optimization Algorithm)和NSGA-II(Nondominated Sorting Genetic Algorithm II)进行对比,结果表明了该改进算法的有效性.     

The origin of the prompt optical emission in GRB 060111B

The detection of a bright optical emission measured with good temporal resolution during the prompt phase makes GRB 060111B a rare event that is especially useful for constraining theories of the prompt optical emission. Comparing this burst with other GRBs with evidence of optical peaks, we find that the optical peak epoch (t_p) is anti-correlated with the high energy burst energetic assuming an isotropic energy release (E_iso) in agreement with Liang et al. (2009), and that the steeper is the post-peak afterglow decay, the less is the agreement with the correlation. GRB 060111B is among the latters and it does not match the correlation. The Cannonball scenario is also discussed and we find that this model cannot be excluded for GRB 060111B.     

Volatile Trapping in Martian Clathrates

Thermodynamic conditions suggest that clathrates might exist on Mars. Despite observations which show that the dominant condensed phases on the surface of Mars are solid carbon dioxide and water ice, clathrates have been repeatedly proposed to play an important role in the distribution and total inventory of the planet’s volatiles. Here we review the potential consequences of the presence of clathrates on Mars. We investigate how clathrates could be a potential source for the claimed existence of atmospheric methane. In this context, plausible clathrate formation processes, either in the close subsurface or at the base of the cryosphere, are reviewed. Mechanisms that would allow for methane release into the atmosphere from an existing clathrate layer are addressed as well. We also discuss the proposed relationship between clathrate formation/dissociation cycles and how potential seasonal variations influence the atmospheric abundances of argon, krypton and xenon. Moreover, we examine several Martian geomorphologic features that could have been generated by the dissociation of extended subsurface clathrate layers. Finally we investigate the future in situ measurements, as well as the theoretical and experimental improvements that will be needed to better understand the influence of clathrates on the evolution of Mars and its atmosphere.