月基差分VLBI定位及参数精度探讨

本文首次采用差分VLBI技术对月球探测器进行观测,分析了差分VLBI观测模型中的EOP参数精度对探测器坐标先验误差的灵敏度,模拟了差分VLBI观测量;平差计算了坐标参数和EOP参数的验后精度,并给出了计算结果。较理想的定位结果为我国的探月工程奠定了一定的理论基础。     

月球探测器差分VLBI测量的模型及可估计参数研究

基于月球探测器离地而较近的特点和差分VLBI技术可以消除部分非几何延迟的优势,采用差分VLBI技术对月球探测器进行观测,推导具体町行的定位模型,并分析模型中可估计的地月大地测量参数序列.     

流动VLBI天线系统噪声温度及天线效率测量

我国自行研制的第一套流动VLBI系统--DCW-01型流动VLBI测量仪,目前已在国家重大科学工程"中国地壳运动观测网络"中投入使用.在流动VLBI的观测试验中,天线系统噪声温度和天线效率是观测前系统调试和检测的两项重要内容.天线系统噪声温度是衡量流动VLBI观测系统内部噪声程度的特性指标;天线效率反映了天线系统对到达天线能量的利用率,在很多计算公式中是一个很重要的参数.因此,精确地测量它们的值是进行相关处理和计算的前提.文中结合我国流动VLBI观测站的研制与建设,介绍了流动VLBI测量仪的天线及接收机系统,并详细阐述了其天线系统噪声温度和天线效率的测量.     

流动VLBI选址探讨

本文结合流动VLBI参加的"地壳运动观测网络工程"和"探月工程",从建立和维护我国地心参考框架和深空探测两个角度讨论了流动VLBI站址的选择、以及所选站址对我国VLBI观测网的改善。提出了将流动VLBI站设在海南,这样既增加了南北基线长度,也扩大了可观测射电源的范围,同时在建立和维持我国地心参考框架方面也是较好的选择。     

昆明站流动VLBI观测数据处理初步结果

对我国自行研制的流动VLBI首次长距离观测数据进行处理,得到了初步结果,并对流动VLBI今后的观测提出了一些建议.     

FAST天线用于VLBI观测系统性能分析

讨论了射电天线用于天文观测和VLBI大地测量时的几项性能参数;列出了我国现有射电天线组成系统时的工作性能和观测精度;计算了利用我国现有射电天线与FAST天线组成基线进行观测时的系统性能以及所要求射电源的最低流量密度.由此可以看出FAST天线用于VLBI观测具有巨大潜力.     

卫星VLBI测轨资料处理中的电离层延迟改正

结合我国探月项目卫星VLBI测轨资料分析中的实际需求讨论了两个问题:一是在S、X波段时延测量精度均为1 ns情况下,电离层延迟改正所能够达到的精度;二是在飞行器VLBI测轨过程中,不能确保S、X波段双频观测情况下获取电离层时延改正的可能途径,包括借助于相关电离层模型、利用常规VLBI历史观测资料积累、借助于局域GPS观测网和IGS网单站GPS测量以及借助于专门设计的单站GPS测量等.最后对电离层VLBI和GPS技术实测结果进行了比较和问题分析.     

基于成像几何模型的火星探测器定位研究

对数亿千米之外的火星探测器进行跟踪导航定位,是火星探测的关键技术之一.目前,我国深空网尚未建成,利用中国VLBI网对火星探测器“火星快车”的定位精度仅约0.1as,难以为火星探测器的精密定轨提供数据保障.提出以遥感影像进行火星探测器几何定位的全新技术方法,利用严密传感器成像几何模型,通过地面控制点在物方空间坐标系中的坐...     

流动VLBI数据采集系统及其控制软件的设计与使用

结合我国流动VLBI观测站的研制与建设，介绍流动VLBI观测站的数据采集系统及其系统控制软件MOFS，在整个VIBI观测期间，MOFS软件控制数据采集系统的自动运转，并具有对系统参数的监测功能，长期的使用表明，流动VLBI观测站的数据采集系统及其控制软件很好地满足了我国流动VLBI观测的要求。     

昆明站流动VLBI观测数据处理初步结果

对我国自行研制的流动VLBI首次长距离观测数据进行处理 ,得到了初步结果 ,并对流动VLBI今后的观测提出了一些建议。     

Adjusting VLBI data to obtain geophysical information for mobile VLBI sites

We have used Very Long Baseline Interferometry (VLBI) data to compute the site coordinates and constant velocity components for 29 fixed antenna sites and 25 mobile sites. The three singularities which occur in the adjustment with respect to the rotation of the system have been resolved by a constraint holding the net rotation of seven fixed antennas, distributed on the stable portions of four of the geologic plates, to the net rotation for these sites as defined by the NNR-NUVEL1 no net rotation model. In order to achieve a minimally constrained adjustment of this type we have found it necessary to use a new adjustment procedure in which we solve for the coordinates of each site at the weighted mean epoch of all the observations involving that site.Using the results of the above solution we have computed the departure for each site from the NNR-NUVEL1 rigid plate model. These departures show that the transition zone in western North America from the region of rigidity to the plate boundary is at least 400 km wide, in general agreement with Ward (1988,1990).     

空间VLBI较差测量

本文探讨了空间ＶＬＢＩ较差测量的基本原理和数学模型，对类星体和脉冲星的较差测量进行了分析，列出了ＲＡＤＩＯＡＳＴＲＯＮ空间ＶＬＢＩ站可能观测到的脉冲星。     

Geodetic VLBI correlation in software

Correlation algorithms for geodetic very long baseline interferometry (VLBI) can now be effectively implemented on parallel computers of modest size. We have undertaken a detailed comparison of the output from a trusted geodetic correlator, one that has supported global geodetic VLBI observations for many years, with the output of a software correlator implemented on a small parallel computing cluster. We show that the correlator outputs agree closely, within expected error bounds, after accounting for the differences in the adopted geometric delay models, and therefore that use of the software correlator is feasible for geodetic VLBI processing, as a first step toward routine geodetic data processing. Recent developments in software correlation for geodesy are discussed, including the possibility of real-time processing options.     

The AUSTRAL VLBI observing program

The AUSTRAL observing program was started in 2011, performing geodetic and astrometric very long baseline interferometry (VLBI) sessions using the new Australian AuScope VLBI antennas at Hobart, Katherine, and Yarragadee, with contribution from the Warkworth (New Zealand) 12 m and Hartebeesthoek (South Africa) 15 m antennas to make a southern hemisphere array of telescopes with similar design and capability. Designed in the style of the next-generation VLBI system, these small and fast antennas allow for a new way of observing, comprising higher data rates and more observations than the standard observing sessions coordinated by the International VLBI Service for Geodesy and Astrometry (IVS). In this contribution, the continuous development of the AUSTRAL sessions is described, leading to an improvement of the results in terms of baseline length repeatabilities by a factor of two since the start of this program. The focus is on the scheduling strategy and increased number of observations, aspects of automated operation, and data logistics, as well as results of the 151 AUSTRAL sessions performed so far. The high number of the AUSTRAL sessions makes them an important contributor to VLBI end-products, such as the terrestrial and celestial reference frames and Earth orientation parameters. We compare AUSTRAL results with other IVS sessions and discuss their suitability for the determination of baselines, station coordinates, source coordinates, and Earth orientation parameters.     

VLBI数据库研究

对VLBI数据库进行了详细的研究,揭示了其结构和数据存取格式,给出了数据库信息列表,并对数据库管理程序进行了说明。     

流动VLBI系统及其应用

本文首先探讨了影响流动VLBI系统性能及观测和解算精度的各种因素,提出了建立我国流动VLBI系统的一组参数指标;作为一个应用,探讨了用流动VLBI技术建立特级大地网对可能布设的全国GPS网的定向、尺度和定位控制与改善的情况。     

Advanced relativistic VLBI model for geodesy

Our present relativistic part of the geodetic VLBI model for Earthbound antennas is a consensus model which is considered as a standard for processing high-precision VLBI observations. It was created as a compromise between a variety of relativistic VLBI models proposed by different authors as documented in the IERS Conventions 2010. The accuracy of the consensus model is in the picosecond range for the group delay but this is not sufficient for current geodetic purposes. This paper provides a fully documented derivation of a new relativistic model having an accuracy substantially higher than one picosecond and based upon a well accepted formalism of relativistic celestial mechanics, astrometry and geodesy. Our new model fully confirms the consensus model at the picosecond level and in several respects goes to a great extent beyond it. More specifically, terms related to the acceleration of the geocenter are considered and kept in the model, the gravitational time-delay due to a massive body (planet, Sun, etc.) with arbitrary mass and spin-multipole moments is derived taking into account the motion of the body, and a new formalism for the time-delay problem of radio sources located at finite distance from VLBI stations is presented. Thus, the paper presents a substantially elaborated theoretical justification of the consensus model and its significant extension that allows researchers to make concrete estimates of the magnitude of residual terms of this model for any conceivable configuration of the source of light, massive bodies, and VLBI stations. The largest terms in the relativistic time delay which can affect the current VLBI observations are from the quadrupole and the angular momentum of the gravitating bodies that are known from the literature. These terms should be included in the new geodetic VLBI model for improving its consistency.     

流动VLBI技术用于电离层探测

提出一种用流动VLBI进行电离层探测的方法，并做较详细的分析。     

Radio source instability in VLBI analysis

The source position time-series for many of the frequently observed radio sources in the NASA geodetic very long baseline interferometry (VLBI) program show systematic linear and non-linear variations of as much as 0.5 mas (milli-arc-seconds) to 1.0 mas, due mainly to source structure changes. In standard terrestrial reference frame (TRF) geodetic solutions, it is a common practice to only estimate a global source position for each source over the entire history of VLBI observing sessions. If apparent source position variations are not modeled, they produce corresponding systematic variations in estimated Earth orientation parameters (EOPs) at the level of 0.02–0.04 mas in nutation and 0.01–0.02 mas in polar motion. We examine the stability of position time-series of the 107 radio sources in the current NASA geodetic source catalog since these sources have relatively dense observing histories from which it is possible to detect systematic variations. We consider different strategies for handling source instabilities where we (1) estimate the positions of unstable sources for each session they are observed, or (2) estimate spline parameters or rate parameters for sources chosen to fit the specific variation seen in the position-time series. We found that some strategies improve VLBI EOP accuracy by reducing the biases and weighted root mean square differences between measurements from independent VLBI networks operating simultaneously. We discuss the problem of identifying frequently observed unstable sources and how to identify new sources to replace these unstable sources in the NASA VLBI geodetic source catalog.