A strategic “viewfinder” for SETI research

One of the most important reasons why unsuccessful results have been obtained so far by the SETI Project is due to the fact that no sure targets to aim at have been available up-to the present state of research. All-sky surveys, even if very accurate and complete, might result to be time-consuming. SETI needs at least one effective “viewfinder” in order that a true targeted research is carried out with a possible success. The best foundation to get this can be identified with the search for the evidence of extraterrestrial astro-engineering activity in form of the Dyson spheres predicted by theory. The existence of such stellar objects can be ascertained by finding the evidence of two main signatures in stars of solar spectral type: infrared excess and anomalous light curves due to transiting artificial objects. These are probably the most powerful viewfinders in order to allow SETI techniques for intelligent signal search to be aimed at more appropriate targets. This paper is not intended to be a research paper but rather a review paper whose goal is not to present calculations and/or operational research but rather to be a research proposal for a more focused research in SETI just using Dyson Spheres as crucial markers.     

潜射自航式声诱饵发射方向研究

为使用自航式声诱饵并结合潜艇的规避机动来对抗声自导鱼雷,运用运筹学的优化原理,将鱼雷和自航式声诱饵最终相遇时距我潜艇的距离归结为有约束的目标函数,根据不同的鱼雷报警舷角、距离,定量分析了三种常用的自航式声诱饵发射方向对目标函数的影响,利用MATLAB的优化工具箱函数进行仿真计算,给出了最优的自航式声诱饵发射方向。     

实用化光力加速度计中单微球重复起支技术

针对光力加速度计的小型化应用,设计并制作了一种基于V型槽的片上光纤光阱,并采用机械振动方法实现了单微球重复起支。理论研究了利用机械振动方法实现微球起支、捕获的动力学过程。结果表明,只有当微球脱离捕获室底面的初始速度满足一定范围时才能稳定捕获,该初始速度范围与捕获室的几何参数有关。提出了利用两光纤中相向传播光的耦合功率监测微球捕获状态的方法,并通过实验完成了微球起支过程的自动控制,实现了单微球的重复起支与捕获。该片上光纤光阱制备方法和单微球重复起支技术可推动光力加速度计的实用化进程。     

高亚声速靶弹拖曳式诱饵系统的拖缆姿态分析

拖缆姿态分析是高亚声速靶弹拖曳诱饵系统结构及布局设计的基础。针对常见的诱饵气动外形,利用旋成体空气动力学理论,分析估算高亚声速环境下拖曳诱饵的气动阻力。采用离散化方法,将柔软拖缆视为由多段刚体连接而成的链状结构,利用力矩平衡原理,由诱饵端起计算缆绳每一离散刚体段的姿态,并逐次向载弹拖缆定位点递推,最终近似计算出整条拖缆姿态。     

三点源诱偏系统对抗反辐射导弹研究

首先分析了有源诱偏的基本原理,然后建立了三点源诱偏系统模型,最后以HARM为例,对三点源系统诱偏ARM进行了仿真分析,导出了一些普遍适用的结论,对雷达诱饵的实际布站有着一定的参考意义。     

用于新型雷达/红外无源复合诱饵的等离子体参数选择

根据电磁波在分层介质中阻抗匹配原理,计算了非均匀非磁化等离子体平行与垂直极化波的功率反射系数。基于碱金属盐的高温电离特性,以功率反射系数为研究对象,对雷达无源诱饵用等离子体的厚度、温度和电子密度分布等参数选择进行了分析,并根据所选择的参数讨论了入射角对无源诱饵应用的影响。     

一种基于图像的星体表面撞击坑自动提取方法

以星体表面的图像数据为基础,根据撞击坑的向阳面呈亮色调而背阳面呈暗色调的原理,提出了一种基于图像的星体表面撞击坑自动提取方法。该方法先用自适应双阈值分割法对星体表面的光学图像进行分割处理,获取图像中明暗区域的形状和位置信息;再用统计学原理分析明暗区域组成结构、像平面上光照方向,结合相关的约束条件来匹配同一撞击坑的明暗区域,同时拟合出撞击坑的外边缘并确定其半径、位置等信息。实验结果表明,该方法能够从常见的星体表面光学图像中快速、可靠地提取出撞击坑的中心位置和半径大小,具有较宽的普适应性和一定的应用价值。     

Influence of dark matter on light propagation in solar system

We investigated the influence of dark matter on light propagation in the solar system. We assumed the spherical symmetry of spacetime and derived the approximate solution of the Einstein equation, which consists of the gravitational attractions caused by the central celestial body, i.e. the Sun, and the dark matter surrounding it. We expressed the dark matter density in the solar system in the following simple power-law form, ?(t,r)=ρ(t)(?/r)^k$?(t\text{,}r)=\rho (t)(?/r{)}^k$, where t is the coordinate time; r, the radius from the central body; ?, the normalizing factor; k, the exponent characterizing r  -dependence of dark matter density; and ρ(t)$\rho (t)$, the arbitrary function of time t. On the basis of the derived approximate solution, we focused on light propagation and obtained the additional corrections of the gravitational time delay and the relative frequency shift caused by the dark matter. As an application of our results, we considered the secular increase in the astronomical unit reported by Krasinsky and Brumberg (2004) and found that it was difficult to provide an explanation for the observed dAU/dt = 15 ± 4 m/century.     

多点源诱偏系统对抗反辐射导弹效能分析

基于有源诱偏系统对抗反辐射导弹(ARM,Anti-Radiation Missile)的理论,导出诱偏误差公式,以3种典型布局方案(三点源布局1、三点源布局2及四点源布局)为例,对误差公式进行简化处理,通过数值计算得到诱偏误差曲线,分析不同布局方案下辐射源功率比对诱偏误差的影响;同时分析ARM的实际攻击过程,引入ARM机动修正,通过仿真分析得到ARM落点图和雷达保护概率曲线,对比不同布局方案下的诱偏效果,结果表明四点源布局为最优方案,对研究多点源诱偏系统对抗ARM的作战效能具有指导意义.     

High resolution science with high redshift galaxies

We summarize the high-resolution science that has been done on high redshift galaxies with Adaptive Optics (AO) on the world’s largest ground-based facilities and with the Hubble Space Telescope (HST). These facilities complement each other. Ground-based AO provides better light gathering power and in principle better resolution than HST, giving it the edge in high spatial resolution imaging and high resolution spectroscopy. HST produces higher quality, more stable PSF’s over larger field-of-views in a much darker sky-background than ground-based AO, and yields deeper wide-field images and low-resolution spectra than the ground. Faint galaxies have steadily decreasing sizes at fainter fluxes and higher redshifts, reflecting the hierarchical formation of galaxies over cosmic time. HST has imaged this process in great structural detail to z  6, and ground-based AO and spectroscopy has provided measurements of their masses and other physical properties with cosmic time. Last, we review how the 6.5 m James Webb Space Telescope (JWST) will measure First Light, reionization, and galaxy assembly in the near–mid-IR after 2013.