Test of the equivalence principle in space

Summary Any violation of the equivalence principle (EP) between test masses in the near-Earth orbit is about 500 times bigger than on the ground, which makes the case for a space experiment very strong. Indeed, ESA and NASA (the European Space Agency and the American National Aeronautics and Space Administration) are currently studying at Phase A level the space mission STEP, whose main goal is to test the universality of free fall to 1 part in 10¹⁷ by means of a combination of very advanced technologies (drag free with proportional thrusters, superfluid-He temperature, SQUID sensors). We discuss the key features of STEP as well as some novel ideas about the possibility of testing the equivalence principle at room temperature in a non-drag-free satellite. Paper presented at the 6th Cosmic Physics National Conference, Palermo, 3–7 November 1992.     

同步卫星扫描视锥与轨道的绘制算法

为了模拟同步卫星在外太空的飞行状态,建设先进的同步卫星模拟仿真系统对于卫星的研制与性能分析有着重要的意义;由于卫星是在特定的轨道上飞行,所以对卫星轨道的绘制建模是卫星模拟仿真系统开发中关键的一环;在这篇文章中介绍了同步卫星与地面观察站通信过程中的扫描视锥与同步卫星运行轨道的绘制算法,重点探讨了基于OpenGL基本矢量图元的绘制以及利用世界坐标系和向量的方法对在绘制过程中所需数据的求解过程;分析了根据同步卫星的运行姿态与其所在轨道的位置来确定同步卫星扫描视锥的角度;最后通过一个虚拟世界的3D引擎验证算法的可行性与绘制效果。     

Observation results of relativistic electrons detected by Fengyun-1 satellite and analysis of relativistic electron enhancement (REE) events

The space particle component detector on Fengyun-1 satellite which works at the sun-synchronous orbit of about 870 km altitude has detected relativistic electrons for a long time. In comparison with the SAMPEX satellite observations during 1999–2004, the relativistic electron data from Fengyun-1 satellite from June 1999 to 2005 are used to analyze the relativistic electron enhancement (REE) events at the low earth orbit, and the possible correlation among REE events at the low earth orbit, high-speed solar wind and geomagnetic storms is discussed. The statistical result presents that 45 REE events are found in total during this time period, and the strong REE events with the maximum daily average flux > 400 cm⁻²·sr^t-1·s⁻¹ occur mostly during the transition period from solar maximum to solar minimum. Among these 45 REE events, four strong REE events last a longer time period from 26-to 51-day and correlate closely with high speed solar wind and strong geomagnetic storms. Meanwhile, several strong geomagnetic storms occur continuously before these REE events, and these continuous geomagnetic storms would be an important factor causing these long-lasting strong REE events. The correlation analysis for overall 45 events indicates that the strength of the REE events correlates with the solar wind speed and the strength of the geomagnetic storm, and the correlation for strong REE events is much stronger than that for weak REE events.     

Mo/Si多层膜在质子辐照下反射率的变化

为了检验应用在极紫外波段空间太阳望远镜上Mo/Si多层膜反射镜在空间辐射环境下反射率的变化情况, 模拟了部分空间太阳望远镜运行轨道的辐射环境, 利用不同能量和剂量的质子对Mo/Si多层膜反射镜进行辐照实验.辐照前后反射率测量结果显示,由于带电粒子的辐照损伤,质子辐照会使Mo/Si多层膜反射镜的反射率降低,且质子能量越低、剂量越大,对多层膜的反射率影响越明显. 当质子能量E=160keV,剂量＝6×10¹¹/mm²时,反射率降低4.1%;能量E=100keV,剂量=6×10¹¹/mm²时, 反射率降低5.7%;能量E=50keV,剂量=8×10¹²/mm²时,反射率降低10.4%. 用原子力显微镜测量辐照后Mo/Si多层膜反射镜的表面粗糙度比辐照前明显增加,致使散射光线能量逐渐增大并最终导致反射率的降低. 关键词： 质子辐照 Mo/Si多层膜反射镜 辐照损伤     

基于泊松分布单光子源的量子误码率的分析

在自由空间量子密钥分配中,单光子源采用具有泊松分布的高度衰减激光脉冲,量子密码术协议采用BB84和B92协议。通过引入量子信道传输率、单光子捕获概率、测量因子和数据筛选因子,建立了量子误码率理论模型,给出了量子误码率的表达式。对于自由空间量子信道,引起量子误码率的主要因素是光学元件、探测器暗噪声和空间光学环境,并对这些因素进行了分析。针对低轨卫星_地面站间链路,进行了量子误码率的数值仿真研究。结果表明,在低轨卫星_地面站间进行量子密钥分配是可行的,限制自由空间量子密钥分配链路距离的主要因素是探测器暗噪声和空间光学环境。     

“Galileo Galilei-GG”: design,requirements, error budget and significance of the ground prototype

“Galileo Galilei-GG” is a proposed experiment in low orbit around the Earth aiming to test the equivalence principle to the level of 1 part in 10¹⁷ at room temperature. A unique feature of GG, which is pivotal to achieve high accuracy at room temperature, is fast rotation in supercritical regime around the symmetry axis of the test cylinders, with very weak coupling in the plane perpendicular to it. Another unique feature of GG is the possibility to fly 2 concentric pairs of test cylinders, the outer pair being made of the same material for detection of spurious effects. GG was originally designed for an equatorial orbit. The much lower launching cost for higher inclinations has made it worth redesigning the experiment for a sun-synchronous orbit. We report the main conclusions of this study, which confirms the feasibility of the original goal of the mission also at high inclination, and conclude by stressing the significance of the ground based prototype of the apparatus proposed for space.     

对地观测高分辨率TDICCD相机调焦控制系统设计

本文详细介绍了一种基于卫星平台的对地观测高分辨率空间TDICCD相机调焦控制系统的设计与实现。针对相机轨道标称值为644.6 km的太阳同步轨道,为实现对地全色成像2 m分辨率和多光谱成像8 m分辨率,推扫成像不小于100 km的地面覆盖宽度要求,采用8片TDICCD高精度交错拼接技术获得高分辨率相机焦平面,以实现对地推扫成像高分辨率和宽覆盖的要求。首先,介绍高分辨率TDICCD相机的离轴光学系统设计;然后,介绍相机调焦系统组成和TDICCD长焦平面拼接技术;最后,对相机调焦系统进行调焦精度测试,根据测试数据分析出相机调焦精度并与理论设计值进行比较分析,调焦,精度测试结果为±7.2 μm(3σ),满足高分辨率TDICCD相机在轨成像需要的高精度调焦要求。     

Optical testing of star sensor (II): Alignment of star sensor from off-line pictures taken in orbital test

Alignment error of an image sensor relative to the optical axis of a star sensor head and alignment errors between four heads were calculated from pictures taken in an orbital experiment. When comparing the image sensor alignment parameters in the orbital test and a ground test, both values matched well. By determining the relative relationship of the four heads using four pictures taken at the same moment in orbit and uploading the parameters to the star sensor system in orbit, the estimated attitude error was improved from 0.29 to 0.17°, though the accuracy was limited by the ±0.2° determination accuracy of the satellite itself. We estimated the attitude determination accuracy from separation angles between boresights of the four heads, calculated from pattern matching between downloaded pictures and a star catalogue. The estimated accuracy, in terms of potential optical performance, was 0.60 arcmin at 3σ, which is sufficient to satisfy the specification of 1 arcmin.     

The TUS Fesnel mirror production and optical parameters measurement

The TUS space experiment is aimed to study energy spectrum, composition, and angular distribution of the Ultra-High Energy Cosmic Ray (UHECR) at E ～ 10²⁰ eV. The TUS mission is planned for operation at the end of 2012 at the dedicated “Mikhail Lomonosov” satellite. The TUS detector will measure the fluorescence and Cherenkov light radiated by EAS of the UHECR using the optical system—Fresnel mirror-concentrator of 7 modules of ～2 m² area in total. Production of the flight model of the optical system is in progress. Status of the Fresnel mirror production, the method, and results of their optical parameters measurement are presented.     

基于厄米-高斯光束的单光子捕获理论研究

从光波电磁场方程的TEM10和TEM01模厄米-高斯光束出发,推导了自由空间量子密钥分配的单光子捕获概率表达式.针对低轨卫星-地面站间激光链路,进行了单光子捕获分析.理论研究表明,对于低轨卫星-地面站间量子密钥分配,采用TEM10和TEM01模厄米-高斯型高度衰减激光脉冲作为单光子源是可行的.     

地表反照光对天基空间目标的成像影响

天基空间目标观测时, 在对空间目标的可见光特性提取的过程中, 随着其姿态的不断变化, 存在太阳光照射不到目标表面、或是在某一特定位置由于目标的强烈反射导致太阳光照度不均匀的情况. 针对这些问题, 分析了在可见光和近红外波段空间目标表面的光照特性, 提出了利用地表反照光作为天基空间目标成像辅助照明光源的思想, 给出了一种精确的建模方法. 基于漫反射模型建立了地表反照光在空间目标表面的照度计算方法, 借助satellite tool kit卫星工具软件获取太阳、目标的坐标, 省去了以往方法中烦琐的矩阵相乘和坐标转换过程; 对任意时刻的地表有效反照区域给出了判断, 引入对地球表面进行网格划分的方法, 对划分后的每一个面元均匀采样, 通过数值积分可计算出整个有效地表反照区域的地表反照辐射. 以某天基成像任务中的太阳同步轨道卫星为例, 就地表反照光对目标的光照情况进行仿真, 计算得出卫星在经过北极上空时可以利用地表反照光作为辅助光源这一重要结论. 仿真结果验证了建模方法的正确性.     

The principle of the positioning system based on communication satellites

It is a long dream to realize the communication and navigation functionality in a satellite system in the world. This paper introduces how to establish the system, a positioning system based on communication satellites called Chinese Area Positioning System (CAPS). Instead of the typical navigation satellites, the communication satellites are configured firstly to transfer navigation signals from ground stations, and can be used to obtain service of the positioning, velocity and time, and to achieve the function of navigation and positioning. Some key technique issues should be first solved; they include the accuracy position determination and orbit prediction of the communication satellites, the measuring and calculation of transfer time of the signals, the carrier frequency drift in communication satellite signal transfer, how to improve the geometrical configuration of the constellation in the system, and the integration of navigation & communication. Several innovative methods are developed to make the new system have full functions of navigation and communication. Based on the development of crucial techniques and methods, the CAPS demonstration system has been designed and developed. Four communication satellites in the geosynchronous orbit (GEO) located at 87.5°E, 110.5°E, 134°E, 142°E and barometric altimetry are used in the CAPS system. The GEO satellites located at 134°E and 142°E are decommissioned GEO (DGEO) satellites. C-band is used as the navigation band. Dual frequency at C1=4143.15 MHz and C2=3826.02 MHz as well as dual codes with standard code (CA code and precision code (P code)) are adopted. The ground segment consists of five ground stations; the master station is in Lintong, Xi’an. The ground stations take a lot of responsibilities, including monitor and management of the operation of all system components, determination of the satellite position and prediction of the satellite orbit, accomplishment of the virtual atomic clock measurement, transmission and receiving navigation signals to and from each satellite. In the north, the south, the east, the west and the center of Chinese main land, the function of CAPS demonstration system is checked and measured. In cars and on board the system is also checked and measured. The results are as follow: CA-code, horizontal positioning accuracy, 15–25 m (1 σ), vertical, 1–3 m; P-code, horizontal positioning accuracy, 8–10 m (1 σ), vertical, 1–3 m; velocity accuracy, CA-code, 0.13–0.30 m/s, P-code, 0.15–0.17 m/s; time accuracy, CA-code, 160 ns, P-code, 13 ns; determination accuracy of orbit ≤2 m. About 20 million US $ and two years are spent for the development of demonstration. A complete CAPS system is now being established. Supported by the National Natural Science Foundation of China (Grant No. 10453001), the National Basic Research Program of China (Grant No. 2007CB815500), the National High Technology Research and Development Program of China (Grant No. 2004AA105030), and the Funds of the Chinese Academy of Sciences for Key Topics in Innovation Engineering (Grant No. KGCXI-21)     

Theoretical Study of Quantum Bit Rate in Free-Space Quantum Cryptography

The quantum bit rate is an important operating parameter in free-space quantum key distribution. We introduce the measuring factor and the sifting factor, and present the expressions of the quantum bit rate based on the ideal single-photon sources and the single-photon sources with Poisson distribution. The quantum bit rate is studied in the numerical simulation for the laser links between a ground station and a satellite in a low earth orbit. The results show that it is feasible to implement quantum key distribution between a ground station and a satellite in a low earth orbit.     

OPNET和STK联合的空间光骨干网络仿真设计

空间光骨干网络是我国空间信息网络的核心。为了对空间光骨干网络中的协议体系、网络架构和关键技术进行可行性验证，开发了基于OPNET和STK(satellite tool kit，卫星工具包)联合的空间光骨干网络仿真平台。设计了由4颗GEO卫星组成的天基骨干网、由10颗LEO卫星组成的天基接入网；开发了由物理层到应用层的光网络协议仿真模型和LEO、GEO、地面站3种节点进程模型，对光骨干网络进行了仿真测试。仿真结果表明:空间光骨干网络最大时延为5.48 s，最小为0.35 s，网络全局平均时延为1.06 s，地面站实时吞吐量最大值为0.88 Gb/s，最小为0.3 Gb/s，证明该平台可准确模拟空间光骨干网络功能，满足空间业务高效传输的需求，为空间光骨干网络性能验证提供仿真平台支持。     

临近空间相干激光通信链路外差效率分析

临近空间相干激光通信链路是天地一体化高速通信网络节点间连接的重要链路。围绕外差效率这一表征大气湍流扰动后信号光和本振光相干合成的指标,推导了非均匀湍流路径上的外差效率理论表达式,并结合大气折射率结构常数廓线,开展了临近空间-地面、临近空间-临近空间和临近空间-低轨卫星三类临近空间相干激光通信链路的外差效率仿真。仿真结果表明:临近空间-低轨卫星链路可以忽略大气对外差效率的影响;如果临近空间-临近空间链路距离大于500km或是临近空间-地面链路天顶角大于60°,外差效率将小于50%,有必要采用自适应光学技术进行补偿。     

宽温变环境的空间反射镜结构分析与研究

相机在从地面到太空的过程中,需要经历重力、温度、气压、辐射等多种环境因素的变化,而这些因素都可能导致空间相机分辨率下降、像质变坏、功能失效甚至系统破坏。所描述的系统工作于18±15℃的温度环境,要求光学反射镜在30℃温度变化范围内仍能正常成像。经优化设计,应用计算机仿真手段进行了静、动态及热特性的分析,提出了一种采用中心粘接结合Bipod柔性支撑形式,解决了在大跨度环境温度范围下的反射镜结构支撑问题。     

Electronic states and spectroscopic properties of MgH in absence and presence of spin–orbit coupling − a configuration interaction study

Electronic spectrum of astrophysically important molecule magnesium hydride (MgH) has been studied using configuration interaction methodology excluding and including spin–orbit coupling. Potential energy curves of several spin-independent (Λ?S) electronic states have been constructed and spectroscopic constants of low-lying bound Λ?S states within 8.2 eV of term energy are reported in the first stage of calculations. The X²Σ⁺ is identified as the ground state in the Λ?S level. In the subsequent stage, the spin–orbit interaction has been incorporated and its effects on the potential energy curves and spectroscopic features of different electronic states of the species have been investigated. The X²Σ⁺_1/2 is identified as the spin–orbit (Ω) ground state of the species. Transition moments of several dipole-allowed transitions are computed in both the stages and radiative lifetimes of the corresponding excited states are computed. Electric dipole moments (µ) for a number of low-lying bound Λ?S states as well as several low-lying Ω-states are also calculated in the present study.     

应用方位反向技术提取反射镜零重力面形

为了预估碳化硅反射镜在空间零重力环境下的面形精度,本文开展了在地面环境下利用方位反向技术提取碳化硅反射镜零重力面形的研究。首先,介绍了方位反向技术提取零重力面形的理论依据;其次,利用有限元分析软件,分析了方位反向对反射镜面形的影响;然后,按照试验流程,先后检测了反射镜在0°和180°状态的面形精度,计算两次检测数据的平均值,得到了反射镜零重力面形。结果表明:反射镜地面零重力面形误差RMS值为12.3 nm,能够满足设计指标要求。最后,对数据可信度进行了分析,确认了试验数据真实可信。该结果预示了反射镜在空间零重力环境下的面形精度,对反射镜光学加工与装调有重要的指导意义。     

Energetic neutrons and gamma rays measured on the Aryabhata satellite

An experiment to measure energetic neutrons and gamma rays in space was launched in the first Indian scientific satellite,Aryobhata, on April 19, 1975. From this experiment, the first measurements in space of the Earth’s albedo fiux of neutrons of energy between 20 and 500 MeV have been made; the values obtained for two mean geomagnetic vertical cut-off rigidities of 5.6 and 17.0 GV are (6.3±0.4)×10⁻² and (1.4±0.3)×10⁻² neutrons cm⁻² sec⁻¹ respectively. These measurements confirm that protons arising from cosmic ray albedo neutron decay, can adequately account for the protons in the inner radiation belt. Observations on gamma rays of energy between 0.2 and 24 MeV have enabled the determination of the total background gamma ray flux in space as a function of latitude. This in turn has permitted useful information on the diffuse cosmic gamma rays. We have also observed four events that showed sudden increases in the gamma ray counting rates between 0.2 and 4.0 MeV. Observational details of these events are given.     

大长宽比长条形SiC反射镜的优化设计与试验

针对某离轴三反光学系统中的大长宽比长条形SiC反射镜镜面边缘随机振动加速度响应均方根值过大的特点,提出一种采用"基结构法"的反射镜结构拓扑优化方法,以随机振动加速度响应均方根值最小化为优化目标.首先对某初始反射镜结构进行有限元分析,发现反射镜镜面边缘点Z向加速度响应均方根值过大.其次,应用连续体结构拓扑优化思想,以反射镜镜面边缘点的随机振动加速度响应均方根值作为优化目标,以镜面峰谷值、镜体一阶约束频率作为约束条件,以反射镜筋板式基结构作为优化空间,对反射镜镜体结构进行拓扑优化设计,得到了一种各项力学性能指标及面形精度均满足指标要求的反射镜轻量化结构.最后,通过有限元分析与振动试验,验证了本文设计的反射镜结构拥有良好的力学性能,其中反射镜镜体质量相比优化前降低了13%,镜面边缘点的Z向随机振动加速度响应均方根值降低了58%,证明了本文优化方法的有效性.