GPS多接收机组合的共视时间比对技术研究

为提高GPS共视时间比对的性能，本文介绍了利用中科院国家授时中心（NTSC）和德国物理技术研究院（PTB）两个守时实验室的多台接收机，基于多接收机组合技术原理，构建了NTSC和PTB各自的多接收机组合系统，采用数据融合技术，计算得出两个多接收机系统的观测数据并进行了时间比对试验及性能分析。结果表明，多接收机组合不仅提高了GPS共视的可靠性和稳定性，且提高了时间比对链路的精度。多接收机链路共视时间比对结果的标准偏差STDEV为1.36ns，比单接收机链路时间比对结果的STDEV值平均提高了19.4%，日稳可达3.2×10^-14。     

Coronal mass-ejection events

Nearly fifteen years have passed since the discovery of coronal mass ejection events from the solar atmosphere. Progress in the interpretation of the observational results has led to a body of knowledge concerning the geometrical and evolutionary properties, physical characteristics, and the association of this type of event with other forms of solar activity. Recent interpretive results taken from the large body of observational data now available are discussed below in some detail. A classification system based on kinetic properties of these events is presented.     

Time Transfer by Laser Link: Data analysis and validation to the ps level

The Time Transfer by Laser Link (T2L2) is a very high resolution time transfer technique based on the recording of arrival times of laser pulses at the satellite. T2L2 was designed to achieve time stability in the range of 1 ps over 1000 s and an accuracy better than 100 ps. The project is in operation onboard the Jason-2 satellite since June 2008. The principle is based on the Satellite Laser Ranging (SLR) technology; it uses the input of 20–25 SLR stations of the international laser network which participate in the tracking. This paper focuses on the data reduction process which was developed specifically to transform the raw information given by both space instrument and ground network: first to identify the triplets (ground and onboard epochs and time of flight of the laser pulse), second to estimate a usable product in terms of ground-to-space time transfer (including instrumental corrections), and thirdly to produce synchronization between any pair of remote ground clocks. In describing the validation of time synchronizations, the paper opens a way for monitoring the time difference between ultra-stable clocks thanks to a laser link at a few ps level for Common View passes. It highlights however that without accurately characterizing the onboard oscillator of Jason-2 and knowing the unavailability of time calibrations of SLR stations generally, time transfer over intercontinental distances remain difficult to be accurately estimated.     

Astrophysical motivation for X-ray polarimetry

In this paper I will review the motivation for measuring polarization in the X-ray band from astrophysical sources. Emission models designed to reproduce X-ray spectra can be tested using polarization, and polarization detected in other wavelength bands makes clear predictions as to the X-ray polarization. Polarization is a powerful tool to infer geometrical properties of sources which are too small to be spatially resolved. At the same time, there has been recent progress in instrumentation which is likely to allow searches for X-ray polarization at levels significantly below what was possible for early detectors. This paper will review the history of X-ray polarimetry, discuss some experimental techniques and the scientific problems which can be addressed by future experiments.     

Review on latest progress on supergiant fast X-ray transients and future direction

In the recent years, the discovery of a new class of Galactic transients with fast and bright flaring X-ray activity, the supergiant fast X-ray transients, has completely changed our view and comprehension of massive X-ray binaries. These objects display X-ray outbursts which are difficult to be explained in the framework of standard theories for the accretion of matter onto compact objects, and could represent a dominant population of X-ray binaries. I will review their main observational properties (neutron star magnetic field, orbital and spin period, long term behavior, duty cycle, quiescence and outburst emission), which pose serious problems to the main mechanisms recently proposed to explain their X-ray behavior. I will discuss both present results and future perspectives with the next generation of X-ray telescopes.     

太阳冲浪的可能机制

本文综合了冲浪的主要观测特征,特别是冲浪活动区的磁特征;利用等离子体动力箍缩理论及Petschek机制,提出太阳冲浪的一种可能机制:活动区磁流的脉冲式浮现-等离子体的周期性动力箍缩-活动区磁场的快速湮灭-冲浪等离子体抛射.这个机制能较好地解释太阳冲浪的重复性及其它重要物理性质.      

WR 技术的发展与应用

本文介绍一种在精密时钟同步协议（PTP）的基础上发展而来的新技术——WR 技术（White Rabbit，白兔）。WR 联合同步以太网以及双混频时差法测量手段，通过对主从时钟间链路环路延迟的不间断高精度的测量，后以测量结果对从时钟的时钟信息进行动态校准，主从时钟的同步精度达到亚纳秒甚至皮秒级。文章先引出WR的发展历史，以及WR 中所包含的主要技术，并介绍目前WR 在某些科学领域所发挥的作用，最后提出WR 未来在其他领域的应用。     

空间机器人柔性臂动力学模糊控制的研究

重点研究了在空间机器人柔性臂的动力学非线性控制问题,由于柔性臂动力学系统的强非线性和耦合性,使得柔性臂控制系统复杂,控制的实时性和稳定性差,本文针对以往柔性臂控制所存在的问题,综合考虑系统的动态和静态特性,提出了一种带有非线性补偿器及ＰＩＤ控制器的柔性臂模糊复合控制方案,然后,根据所推导了一两连杆的空间机器人柔性臂的这非线性模型,进行了系统控制的仿真研究,实例仿真的结果表明,该控制方案能有效地抑制     

The bright mass ejection on the disk on October 14, 1980

A bright mass ejection appearing as a spray on the disk, associated with a 3b flare has been observed. A gap with a length of 2.5 × 10⁴ km and a width of 2 × 10⁴ km occurred between the flare and spray was observed. The intensity of the gap is about 1.6 times more intense than the undisturbed region. The spectral properties of the radio bursts corresponding to the flare and the spray are different. In addition, the flare and the spray are also different in their hard X ray emissions.Observation has not shown any relation between teh spray and the filament that existed previously in the active region. Perhaps the flare and the spray are produced simultaneously by the same mechanism. An observational model of the flare and the spray is shown in figure 3.     

弹射座椅的静态舒适性仿真

针对弹射座椅舒适性存在的不足,基于Poser软件,首先以中国男性飞行员尺寸为依据,建立了三维静态人体模型,保证了人体主要部位尺寸的准确性;然后把AutoCAD中的弹射座椅导入3Dmax软件中,结合飞机座舱的几何尺寸及各操纵机构的几何尺寸,建立弹射座椅-座舱操纵机构模型.最后把该模型导入Poser 软件中,利用人机工效学的相关理论,建立弹射座椅-飞行员-座舱操纵机构系统平台模型.在系统平台中对飞行员进行操纵仿真和分析,讨论了影响弹射座椅舒适性的因素并提出了优化设计方法.由于系统平台中参数的准确性和可调节性,提高了弹射座椅舒适性研究的标准化和通用化程度.      

Catalogue of ionized emission line spectra in obscured AGN

High-energy, high-resolution in the spatial and energy domains is crucial to derive the geometrical distribution and the physical properties of gas and dust surrounding Active Galactic Nuclei (AGN). These are, in turn, basic ingredients of any serious attempt to build an AGN structure model. We present in this paper CIELO-AGN, the first catalogue of ionized emission lines detected in the soft X-ray spectra of a sample of 69 nearby obscured AGN. This catalogue has been implemented according to an IVOA data model, and can be accessed through VO-compatible applications.     

On the time lag between solar wind dynamic parameters and solar activity UV proxies

The solar activity displays variability and periodic behaviours over a wide range of timescales, with the presence of a most prominent cycle with a mean length of 11 years. Such variability is transported within the heliosphere by solar wind, radiation and other processes, affecting the properties of the interplanetary medium. The presence of solar activity–related periodicities is well visible in different solar wind and geomagnetic indices, although their time lags with respect to the solar cycle lead to hysteresis cycles. Here, we investigate the time lag behaviour between a physical proxy of the solar activity, the Ca II K index, and two solar wind parameters (speed and dynamic pressure), studying how their pairwise relative lags vary over almost five solar cycles. We find that the lag between Ca II K index and solar wind speed is not constant over the whole time interval investigated, with values ranging from 6 years to $～$1 year (average 3.2 years). A similar behaviour is found also for the solar wind dynamic pressure. Then, by using a Lomb-Scargle periodogram analysis we obtain a 10.21-year mean periodicity for the speed and 10.30-year for the dynamic pressure. We speculate that the different periodicities of the solar wind parameters with respect to the solar 11-year cycle may be related to the overall observed temporal evolution of the time lags. Finally, by accounting for them, we obtain empirical relations that link the amplitude of the Ca II K index to the two solar wind parameters.     

Large light X-ray optics: basic ideas and concepts

One of the main guidelines for future X-ray astronomy projects like, e.g., XEUS (ESA) and Generation-X (NASA) is to utilize grazing-incidence focusing optics with extremely large telescopes (several tens of m² at 1 keV), with a dramatic increase in collecting area of about two order of magnitude compared to the current X-ray telescopes. In order to avoid the problem of the source's confusion limit at low fluxes, the angular resolution required for these optics should be superb (a few arcsec at most). The enormous mirror dimensions together with the high imaging performances give rise to a number of manufacturing problems. It is basically impossible to realize so large mirrors from closed Wolter I shells which benefit from high mechanical stiffness. Instead the mirrors need to be formed as rectangular segments and a series of them will be assembled in a petal. Taking into account the realistic load capabilities of space launchers, to be able to put in orbit so large mirror modules the mass/geometric-area ratio of the optics should be very small. Finally, with a so large optics mass it would be very difficult to provide the electric power for an optics thermal active control, able to maintain the mirrors at the usual temperature of 20 °C. Therefore, very likely, the optics will instead operate in extreme thermal conditions, with the mirror temperature oscillating between −30 and −40 °C, that tends to exclude the epoxy replication approach (the mismatch between the CTE of the substrate and that of the resin would cause prohibitively large deformations of the mirror surface profiles). From these considerations light weight materials with high thermal–mechanical properties such as glass or ceramics become attractive to realize the mirrors of future Xray telescopes. In this paper, we will discuss a segments manufacturing method based on Borofloat^TM glass. A series of finite element analysis concerning different aspects of the production, testing and integration of the optics are also presented as well.     

Relativistic astrophysics explorer

The great success of the Rossi X-Ray Timing Explorer (RXTE) has shown that X-ray timing is an excellent tool for the study of strong gravitational fields and the measurement of fundamental physical properties of black holes and neutron stars. Here, we describe a next-generation X-ray timing mission, the Relativistic Astrophysics Explorer (RAE), designed to fit within the envelope of a medium-sized mission. The instruments will be a narrow-field X-ray detector array with an area of 6 m² equal to 10 times that of RXTE and a wide-field X-ray monitor. We describe the science made possible with this mission, the design of the instruments, and results on prototype large-area X-ray detectors.     

基于射频的导航卫星星间链路信息传输与仿真研究

星间链路是导航卫星实现精密定轨和自主导航的关键技术之一。导航卫星通过星间链路完成伪距测量和数据交换,维持系统稳定运行的时空基准,保证系统持续提供精准导航服务。根据全球导航卫星系统的建设情况和发展趋势,首先介绍星间观测和信息传输频段,并从天线特征、多址控制方式和网络拓扑结构等角度分析了射频链路的工作体制。最后,针对实际导航卫星星座,应用OPNET平台建立导航信息传输仿真模型,通过分析信息传输效率,验证了基于射频链路导航信息传输的可行性和有效性,对全球导航卫星系统的星间链路研究具有一定的参考价值。     

地心非旋转坐标系中的卫星双向时间比对计算模型

根据卫星双向时间频率传递 (TWSTFT)的基本原理 ,详细推导了地心非旋转坐标系中TWSTFT的计算模型 ,并与地固系中的计算模型进行了分析比较 ,证明了两种计算模型在亚纳秒量级上的等价性。     

建设我国独立自主时间频率系统的思考

分析了物理量测量中时间频率量的特点 ,主要有 :时间的流逝性 ,时间频率具有最高的测量精密度与准确度 ,时间和频率既密切相关又有区别 ,其计量标准可通过电磁波发播 ,其基准是自然基准 ,其测量精确度与测量时间有关。作者阐述了这些特点对计量技术及建设时间频率系统的影响 ,论述了建设我国独立自主的时间频率系统的必要性及其基本框架 ,从基准、实时、授时、时间频率设备的研制、生产和队伍建设等方面提出了建设的具体设想。     

基于射频的导航卫星星间链路信息传输与仿真研究

星间链路是导航卫星实现精密定轨和自主导航的关键技术之一。导航卫星通过星间链路完成伪距测量和数据交换,维持系统稳定运行的时空基准,保证系统持续提供精准导航服务。根据全球导航卫星系统的建设情况和发展趋势,首先介绍星间观测和信息传输频段,并从天线特征、多址控制方式和网络拓扑结构等角度分析了射频链路的工作体制。最后,针对实际导航卫星星座,应用OPNET平台建立导航信息传输仿真模型,通过分析信息传输效率,验证了基于射频链路导航信息传输的可行性和有效性,对全球导航卫星系统的星间链路研究具有一定的参考价值。     

Initial accuracy and reliability of current BDS-3 precise positioning,velocity estimation,and time transfer (PVT)

The primary system of Chinese global BeiDou satellite system (BDS-3) was completed to provide global services on December 27, 2018; this was a key milestone in the development process for BDS in terms of its provision of global services. Therefore, this study analyzed the current performance of BDS-3, including its precise positioning, velocity estimation, and time transfer (PVT). The datasets were derived from international GNSS monitoring and assessment system (iGMAS) tracking networks and the two international time laboratories in collaboration with the International Bureau of Weights and Measures (BIPM). With respect to the positioning, the focus is on the real-time kinematic (RTK) positioning and precise point positioning (PPP) modes with static and kinematic scenarios. The results show that the mean available satellite number is 4.8 for current BDS-3 system at short baseline XIA1–XIA3. The RTK accuracy for three components is generally within cm level; the 3D mean accuracy is 8.9 mm for BDS-3 solutions. For the PPP scenarios, the convergence time is about 4 h for TP01 and BRCH stations in two scenarios. After the convergence, the horizontal positioning accuracy is better than cm level and the vertical accuracy nearly reaches the 1 dm level. With respect to kinematic scenarios, the accuracy stays at the cm level for horizontal components and dm level for the vertical component at two stations. In terms of velocity estimation, the horizontal accuracy stays at a sub-mm level, and the vertical accuracy is better than 2 mm/s in the BDS-3 scenario, even in the Arctic. In terms of time and frequency transfer, the noise level of BDS-3 time links can reach 0.096 ns for long-distances link NT01–TP02 and 0.016 ns for short-distance links TP01–TP02. Frequency stability reaches 5E–14 accuracy when the averaging time is within 10,000 s for NT01–TP02 and 1E–15 for TP01–TP02.     

基于信道估计自适应算法的AVLC重发机制仿真

航空甚高频链路控制(AVLC)是下一代民航地空数据链甚高频数据链模式2(VDL2)的链路服务规程.为了提高AVLC重发控制效率、减少误重发,提出了基于信道估计的监督帧发送时刻自适应算法.在OPNET平台上建立了物理层、数据链路层和子网层VDL2架构;利用动态进程建模方法,建立了AVLC模型.通过对无监督帧、监督帧发送时刻静态算法和自适应算法分别建模,开展对比仿真,验证了监督帧重发控制对于提高VDL2性能的有效性和自适应算法较静态算法的优越性.实验结果表明,在宽范围的系数合理区间内,所提出的算法可有效增加吞吐量,缩小包延时,同时可增强系统稳定性.