利用测日实现快速天文定向

介绍了天文方位角测量原理,给出了实用的计算太阳视位置的方法;研究了在白天恒星无法应用的情况下,利用电子经纬仪测日进行快速天文定向及方位角测量,给出了具体的实施方法及数据解算过程,并对实际测量数据进行了精度分析.     

惯性制导初始方位角标定基准测量精度分析

惯性制导设备初始方位角标定通常采用一等天文方位角作为基准。在实际作业中,标定位置常因场地受限而无法直接进行天文观测,需要通过边角测量将实测天文方位角精确传递至标定位置。因此,标定基准方位角的精度受天文方位角测量精度和方位角传递精度的共同影响。对近年实测的多组一等天文方位角成果进行统计分析,通过中误差和正反方位角不符值两个精度指标,估计一等天文方位角测量精度在±0.5″左右。角度传递测量后,按照导线网平差中最弱边方位角精度估计公式,在传递4次的情况下,方位角闭合传递得到的基准方位角精度在±1.2″左右;经纬仪互瞄传递得到的基准方位角精度在±0.8″左右。     

利用测日实现快速天文定向

介绍了天文方位角测量原理,给出了实用的计算太阳视位置的方法;研究了在白天恒星无法应用的情况下,利用电子经纬仪测日进行快速天文定向及方位角测量,给出了具体的实施方法及数据解算过程,并对实际测量数据进行了精度分析。     

新技术在北极星天文方位角测量中的应用

使用GPS接收机的UTC作为北极星天文方位角测量的时间比对的标准时间，利用推估UTl与UTC的差值，将时间归算到UTl的方法，可满足各等级天文方位角测量的要求，现场计算零点恒星时和北极星坐标的精度满足北极星天文方位角测量的要求，实现了现场评估测量精度。     

图像全站仪拍照时延的标定方法及对天文定向的影响分析

精确测定时间对于天文测量至关重要。针对图像全站仪拍摄恒星存在时延的问题,利用计算机内部时钟与全站仪拍照之间的时间关系,设计了一种简便高效准实时的时延标定方法。推导了拍照时延对天文方位角测量的影响公式,并以北极星定向为例进行了数值分析。大量野外实测数据表明,拍照时延的大小约为4.2 s,且半年内较稳定。经过拍照时延改正之后,能够满足利用北极星时角法进行一等天文方位角测量的精度要求。     

WILD T4全能经纬仪测量天文成果精度分析

WILD T4全能经纬仪是我国一、二等天文测量中的常用仪器.选择近20年部分实测成果作为样本,对中误差、人仪差、方位角对向不符值改正进行统计分析.纬度、经度、方位角的平均中误差为限差的1/2左右,一等天文方位角的外符合精度在±0.9″左右,人仪差成果符合正态分布规律,数学期望接近于0.     

基于大视场光学测量设备的多星观测和解算天文经纬度研究

本文提出了一种新的基于大视场光学测量设备和GPS测量点位天文坐标的方法,即测量多个星体方位角相对于主光轴方位角的增量,然后通过非线性最小二乘法解算出点位的天文坐标。采用该方法不仅可以避免讨论大气蒙气差的修正问题,而且能够满足高精度天文坐标的测量要求。     

射向标定测量中天文成果的归心计算方法

推导出射向标定测量中天文归心计算公式,通过实测数据,对其适用范围进行了分析.结果表明,在中纬度平坦地区,偏心距小于1000m时,天文成果归心计算的精度在纬度0.2”、经度0.01 s、方位角1”以内.     

地球自转参数预报误差对天文测量影响的分析

由于地球自转参数(ERP)的滞后性,目前主要使用国际地球自转和参考服务IERS发布的Bulletin A(简称A公报)预报值进行解算,ERP预报误差对于天文测量的影响目前缺少系统的研究。为此,本文选取IERS 2015—2021近7年A公报的ERP参数对其长期预报及不同时间跨度预报误差分析,并以某站数字天顶望远镜观测结果为例,分析了ERP预报误差对于天文测量的影响。结果表明,随着时间的增加,预报精度越来越差,对于极移参数,1年跨度的预报误差值达到了0.021 as,预报误差对天文经、纬度及方位角的影响分别为0.045 as、0.041 as和0.042 as,完全满足一等天文测量的精度要求;而UT1-UTC预报精度是限制A公报精度的主要因素,60天UT1-UTC的预报误差值已达到了0.007 s,对天文经度的影响达到了0.379 as,已超出一等天文测量的精度要求。为了满足一等天文测量的要求,选取UT1-UTC预报值时,其时间跨度最大为40 d。     

无水天线观测的船舶天文定位新方法

针对船舶天文定位需要同时观测天体和水天线来获取天体高度角,其定位的结果和精度常受制于水天线的可观测时段问题,该文提出了一种无需水天线观测的船舶天文定位新方法。该方法将双天体的方位角作为观测量,通过牛顿迭代法直接计算船位,不受水天线有限观测时段的限制,并且可避免画天文位置线的繁琐作业。基于天体高度方位表数据对该方法模型进行验证分析得:天体方位角测量精度越高,该方法的船舶定位误差越小,当天体方位角测量精度在±0.05°时,船舶定位误差在5nmile之内,该方法可用于夜间船舶定位,从而扩大传统天文定位使用时段。     

Method of simultaneous determination of astronomic latitude,azimuth and longitude by observing only time and horizontal angles between a pair of stars near elongation and a south star near meridian

Summary This paper endeavours to evolve a method of simultaneous determination of astronomic latitude, azimuth and longitude from observations of a star-pair near their times of east and west elongations and a south star near its time of meridian transit. The star-pair of observation being within a short distance of elongation, either east or west, their motion in azimuth then is extremely slow and the small error in time has therefore insignificant effect on their azimuth, and in addition, the south star with its azimuth known from observations of the previous star-pair, being very fast-moving, the method is especially suitable for determining the astronomic latitude, azimuth and longitude by observing only the time and horizontal angees between them, and also a reference mark for ensuring the orientation of the horizontal circle side by side.     

The accuracy of astronomic azimuth determinations

Astronomic azimuths are used in classical geodesy, through the Laplace equation, to control the orientation of geodetic networks. The method most commonly used by the United States National Geodetic Survey for the determination of astronomic azimuth is often referred to as the “direction method”, and is based on observations of Polaris at any hour angle. We have analyzed repeat determinations, by analysis of variance (ANOVA) techniques, to derive realistic estimates of the expected accuracy of typical astronomic azimuths to be used in the readjustment of the North American Datum. We found that the dominant errors are systematic in nature, with a very important source being observer bias, or “personal equation”. We were unable to decompose the remaining systematic error, which presumably consists primarily of instrument biases, anomalous refraction, and setup errors. We found, from an analysis of determinations that were first corrected for observer bias, an increase in the variance of repeat azimuth determinations as a function of latitude that agrees reasonably well with theoretical expectations.     

On the meaning of geodetic orientation

After deriving models for changes of coordinates and azimuths due to rotations, the investigation considers methods for modeling terrestrial orientation in adjustments of geodetic networks. If a misorientation of a geodetic network exists, this can be due to systematic errors in astronomic longitude or in astronomic azimuth, or in both. A separation of these two effects is not possible in practice. The initial azimuth at the datum origin contributes to the orientation only as much as any other azimuth of the same weight.     

隧道工程横向贯通误差的影响因素及其误差分析

影响隧道贯通误差的因素主要有洞内起始方位角、测角精度和测边精度,本文分析起始方位角、测边、测角对隧道贯通误差的影响,得到曲线型、直伸型两种隧道的公式,尤其是分析不同长度、不同精度、不同导线边长条件下横向贯通误差的变化,得出一定规律来指导实践。     

瞬时极坐标与时号改正的自动解算

天文测量数据处理软件在解算经纬度、方位角和人仪差时,需要预先计算出瞬时极坐标值和测前测后时号改正值。本文使用天文数据处理软件的准备文件数据直接进行极坐标和时号改正的解算,对传统内业解算步骤进行编程,减少内业计算的人工干预和数据处理环节。实验与分析表明,自动解算方法能够显著提高作业效率,减少计算的人为误差。     

CANADIAN SHORAN EFFORT, 1949–1953

Abstract

The application, in Oanada, of shoran electronic length measurement to surveying and mapping may be regarded as having been initiated in 1947, when experimental work by Federal Government bureaus was conducted in the vicinity of Ottawa over several long lines between stations of the first-order triangulation. During the succeeding two winters this work was continued, and the results indicated shoran as suitable for establishing position, in Canada's vast northland, quickly and with greater accuracy than by means of astronomic methods. It was realized that trilateration might fail in securing the necessary accuracy because of the many factors involved. Since no information was available, or even existed, from the experience of other survey organizations as to the error in position which might be generated in a comparatively long arc, the first work planned was for a 1100-mile axial-length arc between geodetic bases. This arc, situated in Manitoba and Saskatchewan, was measured in 1949 and 1950. The result indicated that shoran, with careful supervision of all details, could produce results of accuracy superior to astronomic positioning, which is the only reasonable and speedy alternative method of control for mapping at the present stage of development of the northern areas.     

Mini SAR影像的定向参数计算方法分析

首先分析对比了国产小型IMU/GPS组合导航获取的小POS数据特点,因仪器精度有限引起的测量误差无法在成像过程中消除,相位误差导致了Mini SAR影像中部分目标成像出现方位向散焦、模糊,导致目标像点坐标出现误差。将传统定向参数计算方法用于Mini SAR单幅影像定位时,地面控制点数量、像点坐标、定向参数误差向量的限差、地形特征、DEM分辨率及POS数据精度等因素都会影响定位结果。当对定位精度要求不高时,多项式插值POS数据获取的天线相位中心的空间位置、速度比拟合更准确。     

利用SAR影像配准偏移量提取地表形变的方法与误差分析

单一的InSAR观测技术可提取地表沿雷达视线方向(LOS)上的一维位移,而利用SAR影像配准过程中的同名像素偏移量可提取地表沿雷达方位向(近南北向)与距离向(近东西向)的二维形变场,与LOS方向的一维形变形成优势互补。本文在分析SAR影像配准偏移量提取地表形变场方法的基础上,推导建立了雷达方位向与距离向形变提取的误差模型,探讨了该方法提取地表形变的主要误差源。以Bam地震ASAR影像和玉树地震PALSAR影像为数据源,分别开展同震形变场的提取与误差分析试验,结果表明,基于SAR像素配准偏移量提取同震形变场的精度主要受匹配窗口尺寸与过采样因子影响,形变提取误差随匹配计算窗口的增大而减小,形变提取精度随过采样因子的增大有适量提高,地形起伏效应在高差较大的SAR影像区域中表现较为显著。     

解析法测定天文方位角计算软件

介绍北极星时角法测定天文方位角的基本方法，进而说明解析法测定天文方位角的基本原理，阐述计算软件的功能、菜单设计特点和操作方法，以实例说明软件的实用性。