共查询到20条相似文献，搜索用时 578 毫秒
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大气折射映射函数研究中的母函数方法大大地提高了对流层大气折射改正的计算精度，进而提供了在近地平时低高度观测的足够高精度大气折射改正计算方法。作为高精度大气折射模型的进一步考虑，有限距离目标，例如小于几百千米高度，可能对大气延迟和天大气折射都能引入额外的改正。本应用了天大气折射一些新定义，以及详细地讨论了一种有限距离目标的大气折射改正的计算模型，其中包含在映射函数中的角自变量从传统的真天顶距到本征天顶距的改变，对大气延迟和天大气折射的模拟计算表明：本结果对小于向百千米的目标在低于10°的观测具有一定的影响。 相似文献
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目前ＧＰＳ系统中对电离层折射误差的改正主要来用双频技术，双频技术只改正了电离层折射误差的一阶项，可使定位精度达到米级．但对于要求厘米级定位精度的用户来讲，还必须改正电离层折射误差的二阶项；对于要求毫米级定位精度的用户，还应考虑三阶项的改正．笔者提出一个能改正电离层折射误差一阶项、二阶项和三阶项的方法，它是把现有的双频技术与参考文献［１］中提出的双极化技术结合进行的． 相似文献
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YANG KeJun 《时间频率学报》1996,(1)
在卫星定位与授时中，电离层折射误差的影响是十分重要的．目前采用的主要改正方法是双频法，还有电离层模型法．双频法要求卫星发射两个工作频率，而电离层模型法的偏差又较大，这对于使用单频接收机的用户来讲，电离层折射改正就成为一个严重问题，笔者提出的双极化法正好可以解决单频接收机所遇到的问题．双极化法是基于电离层的双折射特性．一个线极化波在电离层中传播时被分裂成两个圆极化波，即左旋圆极化波和右旋圆极化波传播，左旋与右旋圆极化波在电离层中传播的速度不同，则到达接收点的时间也就不同，通过测量两个圆极化波到达接收点的传播时廷差，即可确定电离层折射误差的改正量． 相似文献
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本文调研了大气电离层与非电离层对卫星多卜勒测量的影响及其改正方法,重点介绍Hopfield对流层改正方法的原理,详尽推导了具体结果,指出在Tanenbaum修正的Hopfield模型中,等效参数定义的错误。 相似文献
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综合孔径射电望远镜由于庞大的天线阵结构以及复杂的接收机系统,在其观测中除了遇到一般单天线观测时所面临的一系列误差修正以外,还面临着许多新的误差因素。本文归纳了用于综合孔径观测的三种主要数据处理方法,即:经典的校准方法(采用校准源)、自校准、及多余量——自校准方法。在文中着重将各项误差加以分类并介绍了三种处理方法的工作流程。 相似文献
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测定天文大气折射和建立电磁波折射延迟实测模型(Ⅲ)-专用测量仪器 总被引：1，自引：0，他引：1
针对用天文大气折射测定值,建立随观测站和随方位而异的电磁波折射延迟改正模型的高精度要求,提出了新的仪器误差理论,其主要内容是允许仪器误差存在,并看成是不断变化的,采用相应的测量方法作实时的测定和修正,同时消除仪器的各种变形和误差的影响,排除观测数据中的各种系统误差来源,并达到提高单次测定精度目的;文中还针对不同纬度的观测站、多方位、从天顶直到低空的观测需要,给出了仪器总体结构的安排,和采用视频CCD作为接收器的终端设计方案,也给出了各种仪器误差的测定方法和测量装置的设计要求。 相似文献
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针对空间大地测量技术对中性大气折射延迟改正精度的要求,阐述了折射延迟改正值应随测站和随方位而异的必要性．指出,在尚不能直接测定天文大气折射值的情况下,现有的各种改正模型对大气分布模型的依赖性,不能达到预期的精度和降低观测的截止角．根据云南天文台低纬子午环的特殊结构,和测定大气折射的实践,提出了提高折射延迟改正精度的新方法,即：利用各观测站不同方位从天顶附近直到低地平高度角的天文大气折射实测数据,求解得到折射率差和映射函数的参数,从而建立随测站和随方位而异的大气折射延迟改正模型．这一新方法的实施,将能在不需采用大气分布模型的情况下,把天顶延迟的改正精度提高到1 mm以内,低地平高度角的折射延迟改正精度提高到厘米级,并且把截止高度角压缩到5°以内． 相似文献
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Erik Høg 《Astrophysics and Space Science》1991,177(1-2):203-208
The flexure term and a correction to the atmospheric refraction constant calculated from meteorological data may be determined from the zenith distances of FK5 stars observed each night on a meridian circle. All such determinations on meridian circles and vertical circles have been corrupted-and in fact dominated-byinternal refraction which is often larger than 1" and quite variable. After removing internal refraction by a simple equipment at the CAMC on La Palma, it became apparent that the true flexure and the true correction to the calculated refraction constant vary by less than 0."09 (rms) from night to night. This is a reduction of the estimated uncertainty of these quantities by a factor of about four. This improvement is expected at any meridian circle which is equipped with sufficiently precise (photoelectric) micrometers if internal refraction were removed.Alternative forms of the observation equation for declinations are discussed. Observations over a period of two months may be solved in oneglobal least-squares solution keeping the refraction and the flexure terms constant. Furthermore, one per star is obtained, instead of a different each night for each star. 相似文献
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A. D. Wittmann 《Astronomische Nachrichten》1997,318(5):305-312
In real-time applications fast and accurate algorithms for calculating astronomical refraction are required. Some of the most widely-used expressions are fast, but numerically unstable, and can not be applied where the correction is largest, i.e. close to the horizon. In the present paper a new formula for refraction, which is both fast and numerically stable, is given and compared with previously published refraction formulas. The approximate calculation of refraction 'below the horizon', and of the finite distance correction near the horizon, are also discussed. 相似文献
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《Chinese Astronomy and Astrophysics》2007,31(2):211-220
The space geodetic technology requires an accurate model of correction of refraction delay by the neutral atmosphere that varies from one observing station to another, and from one azimuth to the next. It is pointed out that under the present condition the astronomical refraction can not yet be directly determined, any correction model because of its high dependence on the assumed atmospheric distribution, is incapable of achieving the required accuracy or of improving the cut-off altitude. In this paper, based on the special properties of the lower latitude meridian circle at Yunnan Observatory and our experience of determining atmospheric refraction therewith, a new method is proposed for improving the accuracy of refraction delay correction. Namely, the measured data of astronomical refraction of an observing station from near zenith to low altitudes in different azimuths are used to evaluate the refractivities and the parameters of the mapping functions, thereby establishing a model of atmospheric refraction delay correction that varies with the observing station and the azimuth. Since it is unnecessary for the new method to adopt any atmospheric distribution model, application of this new method will improve correction accuracy of refraction delay to better than 1mm at zenith and to centimeters at low altitudes, and improve the cut-off altitude to below 5 degrees. 相似文献
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Through a comparison between the series expression and mapping function expression of the astronomical refraction, we believe that, as far as a specific atmospheric refraction model is concerned, the computational accuracy is not lower in the former than in the latter, and that the convergence is poorer in the theoretically derived series expression, because of the different approximations made. From an analysis of the method of generating function of the atmospheric refraction mapping function it is considered that this kind of method can not embody the characteristics of geophysics and atmospheric physics. It is pointed out from the comparison that the atmospheric refraction model which is constructed by adopting the specific atmospheric distribution of a certain place does not apply to all other places and cannot be used to evaluate the other atmospheric refraction models. For improving the correction accuracy the key lies in the adoption of an effective method by which the instantaneous refraction values at different positions are directly determined to construct a local, position-dependent model of atmospheric refraction observation. 相似文献
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Focusing on lowering the cut-off elevation in the neutral atmosphere refraction delay correction and on raising the accuracy of the correction, we derive the formulae for calculating the correction for the bending of the light path caused by atmospheric refraction. This is the sort of correction that is given after the principal term in theoretical models of neutral atmospheric refraction delay correction, but is often neglected because it is a small quantity. However, in practice, for a not too low elevation like 15°, this term reaches 1 cm order of magnitude and can not be neglected. Li Yan-xing et al. specially gave a derivation of this correction and a computational method by successive approximation and some calculated values. Yan Hao-jian also proposed a formula of direct calculation but his calculated result was more than 3 times smaller than that of Li Yan-xing, which shows that further study of this correction is called for. Here we give a simple, convenient and reliable formula for calculating the correction. 相似文献
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A new application of astronomical atmospheric refraction in space geodesy is utilized. It is pointed out that in order to meet the high needs of this new application there must be an effective method by means of which the instantaneous value of atmospheric refraction can be directly determined. An atmospheric refraction model fitting in the geographical environment surrounding the observing station is established and then transformed into the neutral atmospheric refraction delay correction model. In this article the necessary conditions for the determination of the value of atmospheric refraction are briefly described. A method for the direct determination of the values of instantaneous atmospheric refraction in various directions and at various zenith distances by taking advantage of the observational principle of the low latitude meridian circle, explored by the Yunnan Observatory, is expounded and the atmospheric refraction observational models built on the basis of stellar spectral type classification in the 4 directions of east, south, west and north and by making use of the observed data are given. 相似文献