大地测量学基础

出版时间：2011-10  出版社：测绘出版社  作者：张西光　等编著  

内容概要

本书为测绘类专业本科《大地测量学基础》(普通高等教育“十一五”国家级规划教材，吕志平，乔书波编著，测绘出版社，2010．3)的英语辅助教材，目的是使学生在学习《大地测量学基础》课程的同时，学习掌握该课程的基本概念、基本理论在英文中的表达和描述，为以后阅读英文专业文献，撰写专业论文打下良好的基础。
本书可作为高等院校测绘类各专业本科生的通用教材，对于从事与测绘工程有关的技术人员也是一本值得推荐的基础性参考书。

书籍目录

1 Introduction
　1.1 Definition of Geodesy
　1.2 Classification of Geodesy
　1.3 Aim of Geodesy
　1.4 Historical Introduction
　1.5 Recent Developments of Space Geodesy
　Vocabulary
2 Reference System
　2.1 Time Systems
　2.2 International Earth Rotation Service
　2.3 Celestial Reference System
　2.4 Terrestrial Reference System
　2.5 Gravity Field Related Reference Systems
　Vocabulary
3 Methods of Measurement in Geodesy
　3.1 Terrestrial Geodetic Measurements
　3.2 Satellite Observations
　3.3 Gravity Measurements
　3.4 Astronomic Measurements
　Vocabulary
4 Geodetic Networks
　4.1 Horizontal Control Networks
　4.2 Vertical Contr01 Networks
　4.3 Three.dimensional Networks
　4.4 Gravity Networks
　Vocabulary
5 The gravity field of the Earth
　5.1 Fundamentals of the Gravity Field
　5.2 Level Surfaces and Plumb Lines
　……

章节摘录

版权页：插图：Geodetic astronomy is based on spherical astronomy.Its importance has decreased since the development of efficient satellite positioning and gravimetric methods and is now restricted to more local applications of gravity field（plumb line direction）and azimuth determinations.On the other hand，radio waves emitted from extragalactic sources are used extensively in order to derive base line vectors between fundamental terrestrial stations and to determine earth-rotation parameters：Very Long Baseline Interferometry.The determination of astronomic latitude，longitude and azimuth is based on the relations given in geodetic astronomy，where the star positions are given by star catalogues.We ignore here the methods，such as Horrebow-Talcott method，developed in geodetic astronomy.Observations of extragalactic radio sources such as quasars，can provide the geodetic information to determine the vector separations between the antennas of two widely separated radio telescopes.The components of the vector are its length and direction.To accomplish this，it is necessary to measure very accurately the difference in the time of arrival，recorded at the two antennas，of a particular wavefront from a given（point）source of radio radiation.The phenomena called interference，in Very Long Baseline Interferometry（VLBI），is produced by electronically superimposing the recorded signals to produce a resultant disturbance or“interference”pattern.The theoretical expression for the relative phase delay shows it to be a function of the source direction，the antenna locations，the relative clock error between the two sites，the time of day，the model atmosphere employed，the earth’S tidal parameters，the radio frequency at which the observation is made，etc.Proper account must also be taken of the earth’S rotation.Two of the main limiting factors in the VLBI technique are clock stability and atmospheric variations.A major goal of VLBI is to reduce the uncertainty in intercontinental baselines to the centimeter level.

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