X射线脉冲星计时导航应用模式与空间试验进展

结合国家导航体系发展与工程应用迫切需求，主要讨论了X射线脉冲星计时导航的应用模式，并介绍了国内外空间试验进展。总结了脉冲星计时地基射电与空间X射线观测的特点和发展现状，阐释了脉冲星时研究与发展的重要意义；总结并归纳了X射线脉冲星导航的应用特点和现有水平，讨论了X射线脉冲星导航的技术优势和典型应用场景；总结了国内外X射线脉冲星计时导航的空间试验进展。根据国内外的空间试验结果，脉冲星时稳定度可达10-14量级，脉冲星导航精度可达到km量级，初步具备在轨应用价值。因此，加快推进国内脉冲星计时导航技术的在轨演示验证与工程应用具有重要意义。     

Frequency steering of spaceborne clocks based on XPNAV-1 observations

Due to high stable rotations, timing of pulsars provides a natural tool to correct the frequency deviation of spaceborne atomic clocks. Based on processing the observational data about a year of Crab pulsar given by XPNAV-1 satellite, we study the possibility of correcting the frequency deviation of spaceborne atomic clocks using pulsar timing. According to the observational data in X-ray band and the timing model parameters from radio observations, the pre-fit timing residuals with a level of 6...     

LHG 83: Another outstanding X-ray binary in the LMC

The strongest X-ray point source, LHG 83, discovered in the EINSTEIN survey of the LMC and not being associated with a nearby coronal type stellar emitter or background AGN is identified with a faint blue variable object. Spectrophotometry reveals low mass X-ray binary characteristics at a mean velocity consistent with LMC membership. The He II 4686 emission exhibits a unique blue shifted component suggesting outflow velocities of several thousand km/s. Optical brightness changes by 0.3 mag in less than one hour are likely to be intrinsic to the source rather than induced by orbital motion. The low X-ray to optical flux ratio is probably due to the fact that the central X-ray source is blocked from direct view by the accretion disk.Based on observations obtained at ESO, La Silla, Chile     

基于可变滑动窗口与3σ准则的脉冲星信号去噪算法

针对地面接收射电观测脉冲星信号较弱、信噪比较低的问题,提出了基于可变滑动窗口与两层3σ准则的信号去噪算法。该算法引入可变滑动窗口,对信号进行分步连续处理,同时在筛选噪声时使用两层3σ准则算法,解决了噪声遗漏及过度去噪问题。为证明算法可靠性与实用性,利用佳木斯66 m观测站实测数据进行算法验证,针对J1939+2134与J1744—1134脉冲星的实测数据进行分析处理。结果表明,该算法能够对脉冲星数据进行有效去噪,普遍提高信噪比约10dB。     

鲁棒EKF在脉冲星导航系统中的应用

针对脉冲星导航系统的滤波问题,传统的扩展卡尔曼滤波(EKF)算法存在不能克服系统模型存在不确定性参数以及乘性噪声等缺陷,提出一种鲁棒EKF算法。首先,分析了状态预测误差方程和估计误差方程,利用统计学原理,得到了状态预测方差矩阵和状态估计方差矩阵计算等式。由于系统模型存在不确定性参数,状态预测协方差矩阵和状态估计协方差矩阵无法计算;因此,利用4个重要矩阵不等式,分析并找到预测方差矩阵和状态估计方差矩阵的上界。最后,利用状态估计误差协方差矩阵上界设计状态增益矩阵,使得状态估计协方差矩阵的迹最小。将该算法对脉冲星导航系统进行仿真,仿真结果验证了所提算法的有效性。     

A fast pulse phase estimation method for X-ray pulsar signals based on epoch folding

X-ray pulsar-based navigation (XPNAV) is an attractive method for autonomous deep-space navigation in the future. The pulse phase estimation is a key task in XPNAV and its accuracy directly determines the navigation accuracy. State-of-the-art pulse phase estimation techniques either suffer from poor estimation accuracy, or involve the maximization of generally non-convex object function, thus resulting in a large computational cost. In this paper, a fast pulse phase estimation method based on epoch folding is presented. The statistical properties of the observed profile obtained through epoch folding are developed. Based on this, we recognize the joint prob-ability distribution of the observed profile as the likelihood function and utilize a fast Fourier transform-based procedure to estimate the pulse phase. Computational complexity of the proposed estimator is analyzed as well. Experimental results show that the proposed estimator significantly outperforms the currently used cross-correlation (CC) and nonlinear least squares (NLS) estima-tors, while significantly reduces the computational complexity compared with NLS and maximum likelihood (ML) estimators.     

EXOSAT LE-CMA observations of the Vela supernova remnant

Presented here are Exosat LE1-CMA images of fields in the Vela SNR. Soft X-ray emission is observed in the north of the remnant indicating a filamentry structure. No X-ray emission was seen in two fields to the west and south-west which have optical filaments but were not studied by Einstein. The Vela pulsar is observed and is significantly broader than a point source indicating the presence of a small nebula as seen by the Einstein HRI. The flux seen from the point source in the CMA is consistent with blackbody radiation from a 10⁶ degree neutron star of approx. 10 km radius. A bright ridge of emission is seen north of the pulsar which may be part of the extended synchroton nebula seen in the 2–10 keV range.     

导航星座自主导航技术--自主星历更新

自主星历更新是导航星座自主导航的关键技术之一,包括卫星轨道精密确定和轨道短时预报两个方面的内容。本文在系统地论述导航星座自主导航的信息处理流程的基础上,重点提出星座卫星轨道精密确定的自适应Kalman滤波算法。系统仿真结果表明：通过星间双向测量数据的滤波处理,能够获得高精度的卫星星历和较小的用户测距误差（URE）,满足高精度导航定位需求,初步证明导航星座自主导航信息处理流程及其星历更新算法的合理性和可行性。     

2A0526-328: The white dwarf rotation period revealed

We report results from EXOSAT observations of the intermediate polar system 2A0526-328 (TV Col). The hard X-ray emission (2–8 keV) is modulated with a period of 1943 s, interpreted as the white-dwarf rotation period. Soft and hard X-ray emission show intensity minima, in phase with the orbital period of 0.2286 days; analysis of the hard X-ray spectra shows that these minima are caused by an extra low-energy absorption corresponding to a H column density of 4 × 10²² cm^-2.     

The X-Ray Spectrometer on the MESSENGER Spacecraft

NASA’s MESSENGER (MErcury Surface, Space ENvironment, GEochemistry, and Ranging) mission will further the understanding of the formation of the planets by examining the least studied of the terrestrial planets, Mercury. During the one-year orbital phase (beginning in 2011) and three earlier flybys (2008 and 2009), the X-Ray Spectrometer (XRS) onboard the MESSENGER spacecraft will measure the surface elemental composition. XRS will measure the characteristic X-ray emissions induced on the surface of Mercury by the incident solar flux. The Kα lines for the elements Mg, Al, Si, S, Ca, Ti, and Fe will be detected. The 12° field-of-view of the instrument will allow a spatial resolution that ranges from 42 km at periapsis to 3200 km at apoapsis due to the spacecraft’s highly elliptical orbit. XRS will provide elemental composition measurements covering the majority of Mercury’s surface, as well as potential high-spatial-resolution measurements of features of interest. This paper summarizes XRS’s science objectives, technical design, calibration, and mission observation strategy.     

低轨导航星座增强BDS精密单点定位技术验证CSCD

首先介绍了低轨增强北斗精密单点定位(PPP)的观测模型、参数估计与数据处理策略。然后对低轨导航增强仿真验证系统及误差仿真配置进行了说明,基于验证系统仿真了全球20个监测站的北斗及低轨导航数据,并通过单北斗及低轨增强北斗静态PPP试验,给出了低轨增强北斗的高精度定位测试评估结果。结果表明,加入150颗低轨卫星观测量后,20个测站PPP精度收敛到10cm之内只需约1min;低轨增强北斗实现静态收敛后,定位精度东方向均值为1.5cm,北方向均值为0.3cm,高程方向均值为2.2cm。相较于北斗单独精密定位,20个监测站收敛后组合定位精度从5cm左右提升到3cm左右。加入低轨卫星可大大加快PPP收敛速度,提升定位精度,验证了低轨卫星在增强PPP精度和收敛速度上的优越性,同时仿真验证系统可支持全链路闭环仿真验证。     

Analytical long-term evolution and perturbation compensation models for BeiDou MEO satellites

The current paper establishes the analytical models of the long-term evolution and perturbation compensation strategy for Medium Earth Orbits(MEO)shallow-resonant navigation constellation,with application to the Chinese Bei Dou Navigation Satellite System(BDS).The long-term perturbation model for the relative motion is developed based on the Hamiltonian model,and the long-term evolution law is analyzed.The relationship between the control boundary of the constellation and the offset of the orbital elements is analyzed,and a general analytical method for calculating the offset of the orbit elements is proposed.The analytical model is further improved when the luni-solar perturbations are included.The long-term evolutions of the BDS MEO constellation within 10 years are illustrated,and the effectiveness of the proposed analytical perturbation compensation calculation approach is compared with the traditional numerical results.We found the fundamental reason for the nonlinear variations of the relative longitude of ascending node and the mean argument of latitude is the long-periodic variations of the orbital inclination due to the luni-solar perturbations.The proposed analytical approach can avoid the numerical iterations,and reveal the essential relationship between the orbital element offsets and the secular drifts of the constellation configuration.Moreover,there is no need for maintaining the BDS MEO constellation within 10 years while using the perturbation compensation method.     

X射线脉冲星导航硬件脉冲轮廓累积研究

为了在X射线脉冲星地面实验系统仿真源模拟产生X射线的基础上,能够快速稳定地得到脉冲轮廓,采用硬件历元叠加的方法获得脉冲轮廓。研究了用硬件实现历元叠加及其数据整合的算法,该算法首先在MATLAB现场可编程逻辑阵列(FPGA)中实现,再通过MATLAB硬件描述语言(HDL)代码生成模块把算法转换成HDL,经编译后获得配置硬件的Bit文件,最终在开发板FPGA上实现数据处理的硬件模块。一段时间内的光子到达时间数据通过MATLAB算法得到的脉冲轮廓数据与通过硬件模块处理后得到的数据结果存在误差,在单个时间窗口内误差最大值为2个光子数,误差平均值占光子数统计平均值的0.084%;两组统计的脉冲轮廓数据中不同数据占总数据个数的9.481%,这样的误差不影响后端模拟导航模块的导航。利用硬件实现的历元叠加及其数据整合模块具有处理速度快、设备紧凑、功耗低的特点,为航天器利用X射线脉冲星导航提供了一种可行的硬件数据处理技术上的支持。     

基于低轨通信星座的导航增强技术发展概述

在我国北斗三号卫星导航系统全面完成组网建设的背景下,世界卫星导航步入新时代.各卫星导航大国均瞄准更高服务精度、更加多样功能、更加可靠服务,正在着手开展新一代系统建设和技术迭代.随着各国对于大型低轨通信星座的积极开发与广泛部署,应用低轨卫星技术实现导航增强与PNT系统备份能力,因其易与GNSS协同,具有提高全球自主导航精...     

The system AM Her = 4U 1814 + 50

The binary system AM Herculis = 4U 1814 + 50 gives the first well ascertained example of an X-ray emitting magnetic white dwarf. The orbital period (3.1^h) is apparent from X-ray to IR frequencies and in linear and circular polarization. Since the time of the identification of the X-ray source the system has been extensively studied. The observations (which range from 1 MeV to 20 m) are reviewed and compared with the present theory of X-ray emitting white dwarfs.     

Locating the LCROSS Impact Craters

The Lunar CRater Observations and Sensing Satellite (LCROSS) mission impacted a spent Centaur rocket stage into a permanently shadowed region near the lunar south pole. The Sheperding Spacecraft (SSC) separated ～9 hours before impact and performed a small braking maneuver in order to observe the Centaur impact plume, looking for evidence of water and other volatiles, before impacting itself. This paper describes the registration of imagery of the LCROSS impact region from the mid- and near-infrared cameras onboard the SSC, as well as from the Goldstone radar. We compare the Centaur impact features, positively identified in the first two, and with a consistent feature in the third, which are interpreted as a 20 m diameter crater surrounded by a 160 m diameter ejecta region. The images are registered to Lunar Reconnaisance Orbiter (LRO) topographical data which allows determination of the impact location. This location is compared with the impact location derived from ground-based tracking and propagation of the spacecraft’s trajectory and with locations derived from two hybrid imagery/trajectory methods. The four methods give a weighted average Centaur impact location of ?84.6796°, ?48.7093°, with a 1σ uncertainty of 115 m along latitude, and 44 m along longitude, just 146 m from the target impact site. Meanwhile, the trajectory-derived SSC impact location is ?84.719°, ?49.61°, with a 1σ uncertainty of 3 m along the Earth vector and 75 m orthogonal to that, 766 m from the target location and 2.803 km south-west of the Centaur impact. We also detail the Centaur impact angle and SSC instrument pointing errors. Six high-level LCROSS mission requirements are shown to be met by wide margins. We hope that these results facilitate further analyses of the LCROSS experiment data and follow-up observations of the impact region.     

无人机软管式自主空中加油视觉导航技术

近年来,机器视觉技术的迅速发展给无人机自主空中加油提供了一种新思路,克服了传统GPS动态适应能力差的不足。基于双目视觉,提出了一种实用的无人机自主空中加油导航方案,并提出了一种利用深度学习进行检测跟踪配合几何约束进行位姿计算的技术。根据加油机和受油机距离的不同,将导航分为远端导航和近端导航。全程对加油锥套进行检测和跟踪,并在近端进行锥套位姿计算。实验结果表明,该算法满足加油的鲁棒性要求,稳定跟踪锁定目标距离范围大于40m。当与目标距离小于10m时,距离误差优于±10cm。说明本文提出的方法具有较强的应用前景。     

Comparison of strapdown inertial navigation algorithm based on rotation vector and dual quaternion

 For the navigation algorithm of the strapdown inertial navigation system, by comparing to the equations of the dual quaternion and quaternion, the superiority of the attitude algorithm based on dual quaternion over the ones based on rotation vector in accuracy is analyzed in the case of the rotation of navigation frame. By comparing the update algorithm of the gravitational velocity in dual quaternion solution with the compensation algorithm of the harmful acceleration in traditional velocity solution, the accuracy advantage of the gravitational velocity based on dual quaternion is addressed. In view of the idea of the attitude and velocity algorithm based on dual quaternion, an improved navigation algorithm is proposed, which is as much as the rotation vector algorithm in computational complexity. According to this method, the attitude quaternion does not require compensating as the navigation frame rotates. In order to verify the correctness of the theoretical analysis, simulations are carried out utilizing the software, and the simulation results show that the accuracy of the improved algorithm is approximately equal to the dual quaternion algorithm.     

基于RTS滤波的GPS+BDS 非差非组合PPP/INS紧组合模型

GPS高精度定位技术在动态复杂环境中,其定位精度、可靠性和连续性因卫星信号频繁失锁而变差。为此,提出了采用基于RTS滤波(Rauch-Tung-Striebel Filter)的GPS+BDS非差非组合PPP(Precise Point Positioning)与INS(Inertial Navigation System)紧组合模型的策略来克服GPS在动态定位中的弱点。其中,采用GPS+BDS双系统观测数据,可提高PPP解算中的可用卫星数,改善星站间定位几何强度和提高PPP收敛速度;采用PPP/INS紧组合,利用INS的自主定位特性和短期高精度特性,可有效改善复杂环境下的定位精度和连续性;采用RTS滤波,可进一步提高PPP/INS紧组合性能。首先推导了GPS+BDS非差非组合函数模型、PPP/INS紧组合函数模型和RTS滤波函数模型,然后利用一组车载动态数据,对动态GPS PPP、GPS+BDS PPP、GPS/INS紧组合、GPS+BDS PPP/INS紧组合和基于RTS的GPS+BDS PPP/IMU紧组合的定位、测速和定姿性能进行分析。实验结果表明,该方案可有效提高定位(58%～72%)、测速(74%～82%)和定姿(4%～23%)精度,特别是对卫星失锁期间的定位性能改善尤为明显。     

单兵自主导航技术研究

针对美国MicroPNT计划中的单兵导航技术开展了理论分析、样机研制及试验工作,设计了单兵导航技术的基本原理、系统组成和基本算法,分析了室内作业的定位和指挥需求,分析了影响系统实现和定位精度的关键因素,研制了原理样机并开展了导航试验,结果表明：采用微机电惯导系统+零速修正的方案来实现单兵导航的方案是可行的;以目前微机电惯性仪表的性能水平,有望实现100米/小时的定位精度;随着微型惯性仪表性能的提高,有望在5-10年内实现定位精度10米/天的单兵自主导航系统。