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.     

别尔曼特反例的扩充

别尔曼特关于微元法提出了一个反例，本文是对别尔曼特反例的扩充，并通过对这些反例的分析，提出了微元的多样性及正确选取微元的若干方法。     

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。     

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.     

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.     

一种获取耀斑光变曲线的高精度,高分辨方法

一种获取耀斑光变曲线的高精度、高分辨方法栗志，周卫红（中国科学院云南天文台，昆明６５００１１）关键词太阳耀斑，光变曲线，测量方法太阳耀斑物理机制的研究，需要得到耀斑核的辐射的演化，在光学波段常用耀斑在单色光的辐射强度的时间变化曲线作为分析依据［１］．...     

新型行波光调制器单脊波导的微波电路研究

设计了一种采用单脊波导作为微波电路的新型行波光调制器。分析计算了脊缝间距小于１．００ｍｍ的脊波导中的电场分布、截止波长、频带宽度和特性阻抗；设计了与矩形波导联接的过渡段。结果表明：采用单脊波导作为光调器将使微波电场得到充分的利用，将提高调制效率；使波导单模工作频带增宽；具有较低的特性阻抗；通过过渡段易与矩形波导联接及保证单模传输。最后，经论证选择了切实可行的脊波导各几何参数ａ＝１３．００ｍｍ，ｂ＝１０．１６ｍｍ，ｄ＝０．５０ｍｍ，ｓ＝１．００ｍｍ。     

轻型飞行模拟器并联机构约束检验算法的研究

采用6-3UPS边置式座舱结构的轻型飞行模拟器,其工作空间受约束条件的限制。在数学描述的基础上,对影响工作空间的各项约束检验算法进行研究,并分析约束条件下轻型飞行模拟器的工作空间,为控制算法的研究提供依据。     

SETI implications of gravitational assist via chaotic trajectories of binary objects

Extrapolating from the technique of gravitational assist via chaotic trajectories of binary objects, this paper considers how such techniques might be used in other systems. We examine which types of systems are the best candidates for harvesting gravitational energy for payload ejection. We also consider what signatures might be present in either the asteroid orbits or radiation of the central body if extraterrestrial intelligences were to use such techniques about these candidate systems.The simulation studies show that current technology cannot approach the sensitivity needed to detect either of these signals. Instead, we provide these results as guidance to studies in coming decades on patterns that may indicate the use of an asteroid ejection system.