Method and system for measuring atmospheric refraction value at large zenith distance

Abstract

The invention provides a method for measuring an atmospheric refraction value at a large zenith distance. The method comprises the following steps: S0, providing a telescope, an image acquisition terminal, a processor and a corner reflector, and measuring the actual included angle L0 between the two reflectors, wherein the corner reflector is provided with two reflectors to enable the telescope has first and second fields of view; S1, observing two different zenith areas positioned at the small and large zenith distances by virtue of the first and second fields of view, and extracting star images acquired by the image acquisition terminal; S2, distinguishing which zenith area the observation star image in each star image comes from, and acquiring the corresponding celestial coordinates of each observation star image; S3, marking the zenith as Z, and solving horizontal coordinates (A0, h0) and (A1, h1) corresponding to the actual field-of-view centers sigma0 and sigma1 in the first and second fields of view according to the corresponding celestial coordinates of each observation star image; and S4, acquiring the atmospheric refraction value at the actual field-of-view center sigma1 in the second field of view according to Z, A0, A1 and L0. According to the method disclosed by the invention, the influence of place parameters, instrument parameters and other system errors is avoided, the accumulative measurement error is eliminated, and the measurement accuracy is improved.

Description

technical field [0001] The invention relates to the field of astronomical measurement, in particular to a method and system for measuring atmospheric refraction values ​​at large zenith distances. Background technique [0002] Atmospheric refraction refers to the difference between the direction of light from a celestial body before it enters the atmosphere and when it reaches the observer. Compared with other factors that affect the direction of celestial bodies, the biggest characteristic of atmospheric refraction is its uncertainty, because the influence of factors such as aberration, parallax, proper motion, and gravitational bending of light on the direction of celestial bodies can be calculated accurately theoretically, but the atmosphere The influence of refraction is notable to be simulated, and its irregularity is sometimes obvious, especially in the case of large zenith distance. Therefore, atmospheric refraction is the main obstacle to improve the accuracy of gro...

AI Technical Summary

Problems solved by technology

The actual measurement results prove the feasibility of this scheme, but at the same time, it also shows that the processing results of single-field telescope observations will be affected by cumulative errors. Moreover, the star positioning accuracy of large-field telescopes is low, which affects the final atmospheric refraction measurement results. the accuracy of

Images