提高中性大气折射延迟改正精度的可能途径

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．     

A Possible Means of Improving the Accuracy of Refraction Delay Correction of Neutral Atmosphere

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.     

Determination of the Instantaneous Values of Astronomical Atmospheric Refraction and Local Observational Modeling

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.     

天文实测蒙气差的研究

建立在子午—卯酉交替观测原理基础上的低纬子午环（ＬｏｗＬａｔｉ－ｔｕｄｅＭｅｒｉｄｉａｎＣｉｒｃｌｅ）即将出厂投入调试及试运行阶段，进一步研究天文蒙气差修正将是低纬子午环进行高精度观测的重要保证之一。作为对天文蒙气差修正的初步研究，本文首先分析了影响天文蒙气差的主要气象因素，对蒙气差随各种条件的变化情况进行了讨论；在此基础上，推算了大气平面平行层模型以及同心球层模型下的蒙气差值，论述了蒙气差表的编制方法，进而对各种蒙气差理论公式计算所得的修正值进行了分析比较；针对理论计算蒙气差值精度的不足，本文着重阐述了利用低纬子午环（ＬＬＭＣ）进行大气蒙气差实测的方法、原理，较为详尽的说明传统的方法不能满足实测大气折射的要求，而低纬子午环由于自身一些新的特点，能够满足Ｔｅｌｅｋｉ所提出的四个要求；在此基础上推导了相应的计算公式并进一步探讨了实测大气等密度倾斜的方法，最后给出了相应的精度估计，就如何建立一个适合于观测点的实用的实测大气模型进行了探讨     

Astronomical refraction: formulas for all zenith distances

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.     

关于大气分布模型

简述了大气垂直分布情况和高空探测方法,分析了目前只能采用球对称大气分布模型的原因;论证了随观测站、随方位而异的天文大气折射实测模型和折射延迟改正模型,已经包含了观测站上空大气实际分布的非球对称特性,不必再去寻找或建立随地势而异和随季节而变的大气分布模型,避免了大气分布模型选择不当的影响,从一个方面为提高天文大气折射改正精度和电磁波大气折射延迟改正精度提供了保证。     

New consideration of atmospheric refraction in laser ranging data

In this paper we reconsider the formulae of tropospheric refraction correction for the Satellite Laser Range technique. From the expansion of the complementary error function, a new continued fraction form of the mapping function at optical frequencies is derived. The correction terms related to the operation frequency of the laser beam are considered in both the zenith delay and the mapping function. The correction for low-elevation satellites is briefly reviewed. The theoretical accuracy of the new mapping function has been analysed via the ray tracing integrals under the standard atmospheric profile. With respect to the radiosonde data, the deviations of the new mapping function are investigated in an elevation range down to near 1°, which is comparable with the results of the Marini–Murray formulae .     

大气折射与路径弯曲延迟

电磁波信号在地球大气中的传播受到折射的影响,传播的方向发生了改变,传播的路径变为曲线,长度大于直线距离,相应的传播时间也被延长了,采用一个简化的球对称大气模型计算了光线在不同天顶距下由于路径弯曲而引起的延迟改正.     

On Astronomical Atmospheric Refraction

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.     

Improvement on Atmospheric Hydrostatic Delay Correction at Low Elevation Angles

Observation made at low evelation angles is the trend of development of GPS (Global Positioning System) meteorology, wherein the development of highly accurate atmospheric hydrostatic delay corrections at low elevating angles is the main key technique. The comparison among three methods for calculating the atmospheric hydrostatic delay correction of the radio waves from space to the ground-based receiver is made: (1) the atmospheric hydrostatic delay obtained from the path integration of the sounding balloon data under the assumption of atmospheric spherical symmetry, (2) the atmospheric hydrostatic delay acquired from the reanalyzed data of the NCEP (National Centers for Environmental Prediction) under the assumption of atmospheric spherical symmetry and (3) the atmospheric hydrostatic delay got from Niell's atmospheric hydrostatic mapping function. The results of the comparison of them with the atmospheric hydrostatic mapping function obtained from the calculation carried out by taking advantage of the data acquired at 89 sounding balloon stations in China in 2001 show that the accuracy of the method of the path integration of the reanalyzed data of NCEP at low elevating angles (bellow 5°) is about 5 times better than that of the Niell mapping function model.     

Constancy of the refraction constant

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.     

双波长卫星激光测距

双波长卫星激光测距不必借助大气改正模型，利用双波长往返时间差就可以进行大气折射改正，采用皮秒级事件计时器等技术测量往返时间差，修正精度可以达到毫米量级，介绍了这一领域的研究进展、双波长大气改正的基本原理，分析了双波长激光测距的精度，最后对双波长卫星激光测距前景进行了展望。     

对流层大气折射延迟改正：（Ⅱ）：当前主要研究方向和进展

在文献「１」，综述了对流层大气折射延迟改正的基本概念和研究方法。本文中，介绍了在此领域中的主要研究方向的动态，以及一些最新成果。同时，还评述和分析了这些研究工作的主要特色和将来的发展方向。在本文的第８节，简要地介绍了作者在大气折射研究中的最新进展－大气折射母函数方法。     

The Method of Differential Measurement of Astronomical Refraction and Results of Trial Observations

Because of the influence of atmospheric refraction the astronomical observations of the objects with the angles of elevation below 15° are generally avoided, but for the sake of the complete theoretical research the atmospheric refraction under the condition of lower angles of elevation is still worthy to be analyzed and explored. Especially for some engineering applications the objects with low angles of elevation must be observed sometimes. A new idea for determining atmospheric refraction by utilizing the differential method is proposed. A series of observations of the starry sky at different heights are carried out and by starting from the zenith with a telescope with larger field of view, the derivatives of various orders of atmospheric refraction function at different zenith distances are calculated and finally the actually observed values of atmospheric refraction can be found via numerical integration. The method does not depend upon the strict local parameters and complex precise observational instrumentation, and the observational principle is relatively simple. By the end of 2007 a simply constructed telescope with a larger field of view at Xinglong Observing Station was employed to carry out trial observations. The values of atmospheric refraction at the true zenith distances of 44.8° to 87.5° were obtained from the practical observations based on the differential method, and the feasibility of the method of differential measurement of atmospheric refraction was preliminarily justified. Being limited by the observational conditions, the accuracy of the observed result was limited, the maximal accidental error was about 6” and there existed certain systematic errors. The value of the difference between the result obtained at the zenith distance of 84° and that given in the Pulkovo atmospheric refraction table was about 15”. How to eliminate the cumulative error introduced due to the integration model error is the key problem which needs to be solved in future.     

大气折射母函数方法、大气折射解析解和映射函数

回顾了作为实用天文学和大地测量学中基本研究课题之一的大气折射映射函数研究的进展。介绍了近几年上海天文台发展的大气折射母函数方法 ,以及由此导出的大气折射解析解。对如今广泛地应用在空间测量技术中的几种映射函数做出评述 ;分析了NMF模型的优点和不足之处。介绍了由大气折射母函数方法引出的大气延迟新连分式映射函数和天文大气折射的映射函数方法。利用VLBI实验中高度截止角与基线长度重复率的关系、探空气球 (radiosonde)观测资料、PRARE资料比较了各种映射函数的结果。特别指出了映射函数方法对天文大气折射和光学波段测距精度的改进。讨论了大气折射计算中的主要误差源。     

长波信号中周期修正项对授时精度的影响

周期修正项是长波授时信号的一个特征量,它通常与长波授时信号的跟踪点有关。在授时过程中,它是影响长波传播路径时延计算的重要因素。讨论了长波定时信号接收端感应电动势周期修正项与发射端电流信号周期修正项的不同,分析了磁天线和电天线对周期修正项的影响,计算了实际传播介质中周期修正项的大小。结果表明:当传播路径上的电参数恒定时,周期修正项与传播距离有关,传播距离越大,感应电动势的周期修正项也越大,并且两者呈线性关系。同时,周期修正项也受等效电导率等因素的影响,在恒定的距离上,等效电导率越小,周期修正项反而越大。授时用户可以利用感应电动势周期修正项的数值计算结果修正传播路径上的时延,有效地提高传播路径时延计算的精度,从而提高授时精度。     

中性大气折射映射函数和大气折射母函数方法

回顾了作为实用天文学和大地测量学中基本研究课题之一的大气折射函数研究的最新进展;介绍了近几年发展的大气折射母函数方法。对如今广泛地应用在空间测量技术中的几种映射函数,如ＣｆＡ２．２、ＭＴＴ等模型作出评述;特别分析了ＮＭＦ模型的优点和不足之处。还介绍了由大气折射母函数方法引出的大气延迟新连分式映射函数和天文大气折射的映射函数方法,利用ＶＬＢＩ实验中高度截止角与基线长变化的关系和探空气球（ｒａｄｉｏｓ     

Study of the atmospheric refraction in a single-mode instrument – application to AMBER/VLTI

This paper presents a study of the atmospheric refraction and its effect on the light coupling efficiency in an instrument using single-mode optical fibres. We show the analytical approach which allowed us to assess the need to correct the refraction in J and H bands while observing with an 8-m Unit Telescope. We then developed numerical simulations to go further in calculations. The hypotheses on the instrumental characteristics are those of AMBER (Astronomical Multi BEam combineR), the near-infrared focal beam combiner of the Very Large Telescope Interferometric mode, but most of the conclusions can be generalized to other single-mode instruments. We used the software package caos to take into account the atmospheric turbulence effect after correction by the European Southern Observatory system Multi-Application Curvature Adaptive Optics. The optomechanical study and design of the system correcting the atmospheric refraction on AMBER is then detailed. We showed that the atmospheric refraction becomes predominant over the atmospheric turbulence for some zenith angles z and spectral conditions: for z larger than 30° in J band for example. The study of the optical system showed that it allows to achieve the required instrumental performance in terms of throughput in J and H bands. First observations in J band of a bright star, α Cir star, at more than 30° from zenith clearly showed the gain to control the atmospheric refraction in a single-mode instrument, and validated the operating law.     

实测大气折射值的新方法

简单评述了现有各种版本的大气折射表所依据的理论基础和编制方法，指出了实测大气折射值、建立随地形而异的实测大气折射模型的必要性和应具备的基本条件；在分析了长期以来不能直接测定大气折射值的原因后，介绍了一种在不同方向精确测定大气折射值和建立观测点大气折射模型的新方法，以及所依赖的观测仪器具备的特性，最后给出了用实测数据建立的本地大气折射模型。