基于遥测电流的太阳翼在轨振动参数辨识方法

针对传统太阳翼在轨振动特性测试需采用高精度星载设备或额外增设测量装置的问题,建立了太阳翼发电电流与太阳光线入射角之间、太阳翼在轨振动与太阳翼发电电流波动之间的关系。在此基础上提出了仅依靠遥测电流波动信息辨识太阳翼在轨振动固有频率和阻尼比的方法,即：首先通过傅里叶变换获取电流波动信号的幅频响应;结合模态分析结果辨识振动频率及对应阶次信息;通过滤波算法分解各阶次振动,逐一计算对应阻尼比。为验证本方法有效性及误差水平,构造了由多个单自由度衰减振动及随机信号叠加而成的模拟电流波动信号进行仿真分析,结果表明方法有效,误差可接受。在某卫星太阳翼在轨振动参数辨识上的应用实例也表明,本文所提出的方法满足工程应用需求。     

空间太阳能电站技术的可行性研究

简要介绍世界空间太阳能电站的太阳发电卫星／太阳能发电（ＳＰＳ／ＬＳＰ）系统两种设想及相关技术的可行性研究与发展情况。总体说，实现空间电站所需无线电能传输技术（ＷＰＴ）、太阳电池技术及空间技术已基本成熟，可望于下世纪初建立初步的空间太阳能发电系统。     

SiCp/Al复合材料在太阳电池阵展开机构上的应用

介绍了SiCp/Al复合材料的机械性能、热力学性能、加工性能，以及在太阳电池阵展开机构中的应用情况。分析认为采用SiCp/Al复合材料，充分发挥了其高比模量、高比强度和良好的耐磨性能，其管材、型材已达到了应用阶段。     

太阳能热推进技术的研究进展

综述了太阳能热推进的发展历程及现状,分析了不同方案太阳能热推进的原理、结构和性能特点,并对研究中的重点、难点问题结合国外发展情况进行了进一步的探讨,这对我国开展相关研究,赶上世界先进水平具有重要意义。     

Johannes Geiss: Explorer of the Elements

The extraordinary life and scientific achievements of Johannes Geiss span an almost impossible breadth of scientific topics, from the study of rocks to tenuous plasmas, from volcanoes to meteorites. But, his impact also extends way beyond the field of science. Professor Geiss is a well-known teacher and a highly successful science leader whose impact has been felt at the University of Bern, in Switzerland, and around the globe. We present here a brief summary of this highly successful career via a pictorial overview and a movie compiled by a former student who had the good luck to work with Professor Geiss during his years at the University of Bern. Electronic Supplementary Material The online version of this article () contains supplementary material, which is available to authorized users.     

太阳帆材料研究进展

太阳帆飞船由于无需动力等优势近年来引起了各国科学家的研究兴趣,并在深空探测领域具有重要的应用前景.太阳帆的结构设计和材料选择是影响其性能的重要因素,本文结合太阳帆飞行环境的特点,介绍了太阳帆的基本结构和飞行原理,重点针对目前几种比较典型的太阳帆设计,对其支撑材料以及帆面薄膜材料进行了综述,并分析了各种材料和设计的性能特点.     

Effects of X2-class solar flare events on ionospheric GPS-TEC and radio waves over Brazilian sector

In this investigation, we present and discuss the effects of 6 X2-class solar flare events in the ionospheric F region over Brazilian sector that occurred during 2013 to 2015. For this investigation, we present the vertical total electron content (VTEC) observations from nearly 120 Global Positioning System (GPS) receivers all over the Brazilian sector for each event. Also, ionospheric sounding observations obtained in São José dos Campos (23.2°S, 45.9°W, dip latitude 17.6°S; hereafter referred to as SJC), under the southern crest of the equatorial ionospheric anomaly (EIA), Brazil, are presented. The observations show that the greatest TEC impact occurs with the EUV fluxes increases lasting for more than one hour and when the solar active region is located close to the solar disc center. We present a detailed study of the efficiency of the EUV flux with wavelengths ranging from 0.1 to 190?nm for the F region ionization. The largest increase of ΔTEC occurs below the magnetic equator line, covering mainly the central, northeast, southeast and south regions, which includes the equatorial ionospheric anomaly (EIA) region. The ionograms show partial or total fade out in the echoes traces observed causing blackouts of radio signals of up to 60?min, which can have serious consequences to technological systems of public and private agencies around Brazilian sector. This study can help to better understand the effects of solar flares in the ionospheric F region.     

The solar cycle variation of plasma parameters in equatorial and mid latitudinal areas during 2005–2010

Based on the ISL data detected by DEMETER satellite, the solar cycle variation in electron density (Ne) and electron temperature (Te) were studied separately in local daytime 10:30 and nighttime 22:30 during 2005–2010 in the 23rd/24th solar cycles. The semi-annual, annual periods and decreasing trend with the descending solar activity were clearly revealed in Ne. At middle and high latitudes, there exhibited phase shift and even reversed annual variation over Southern and Northern hemisphere, and the annual variation amplitudes were asymmetrical at both hemispheres in local daytime. In local nighttime, the annual variations of Ne at south and north hemispheres were symmetrical at same latitudes, but the annual variation amplitudes at different latitudes differed largely, showing obviously zonal features. As for Te, the phase shift in annual variations was not as apparent as Ne with the increase of latitudes at Southern and Northern hemisphere in local daytime. While in local nighttime the reversed annual variations of Te were shown at low latitudinal areas, not at high latitudes as those in Ne. The correlation study on Ne and Te illustrated that, in local daytime, Ne and Te showed strong negative correlation at equator and low latitudes, but during the solar minimum years the correlation between Ne and Te changed to be positive at 25–30° latitudes in March 2009. The correlation coefficient R between Ne and Te also showed semi-annual periodical variations during 2005–2010. While in local nighttime, Ne and Te exhibited relatively weak positive correlation with R being about 0.6 at low latitudes, however no correlation beyond latitudes of 25° was obtained.     

Outreach activities during the 2006 total solar eclipse sponsored by the International Heliophysical Year

The International Heliophysical Year (IHY) is an international program of scientific research to advance our understanding of the physical processes that govern the Sun, Earth and heliosphere. It has a strong educational component, linking research and education. Here, we describe the outreach activities during the 2006 total solar eclipse sponsored by IHY.     

Saturn kilometric radiation as a monitor for the solar wind?

Since the Voyager mission it is known that Saturn Kilometric Radiation (SKR) is strongly influenced by external forces, i.e., the solar wind and in particular the solar wind ram pressure. Recent studies using Cassini data essentially confirmed these findings for particular periods during the first Cassini orbit of Saturn. The data coverage of SKR by the Cassini/RPWS experiment for the period of six months prior to Saturn Orbit Insertion (July 1, 2004) is rather continuous, whereas there are gaps in the solar wind plasma data. The strong correlation of SKR with the solar wind may provide an indication on the variations of the solar wind plasma, specifically during the gap periods. These periods lacking solar wind data are substituted by Ulysses solar wind data which have been propagated over ∼4 AU, applying magnetohydrodynamic propagation models. Cross correlation studies showed that Ulysses solar wind data can be taken as a substitute for missing Cassini data. The use of SKR as monitor for solar wind variations is discussed. With the present set of observations the SKR proxy lacks significant reliability.