On the importance of astronomical refraction for modern Solar astrometric measurements

TL;DR

This paper investigates the impact of astronomical refraction on ground-based solar measurements, providing correction tools and uncertainty estimates to improve the accuracy of solar astrometry at high zenith distances.

Contribution

It offers exact correction formulae for solar radius measurements affected by refraction and demonstrates their applicability up to 80 degrees zenith distance using standard atmospheric models.

Findings

Corrections are valid up to 70 degrees with approximate formulas.

Exact formulae extend correction validity up to 80 degrees zenith distance.

Uncertainty estimates help determine maximum observation zenith distance for desired accuracy.

Abstract

In this work we study in details the influence of pure astronomical refraction on solar metrologic measurements made from ground-based full disk imagery and provide the tools for correcting the measurements and estimating the associated uncertainties.For a given standard atmospheric model, we first use both analytical and numerical methods in order to test the validity of the commonly or historically used approximations of the differential effect of refraction as a function of zenith distance. For a given refraction model, we provide the exact formulae for correcting solar radius measurements at any heliographic angle and for any zenith distance. Then, using solar images recorded in the near infrared between 2011 and 2016, we show that these corrections can be applied up to $70\deg$ using the usual approximate formulae and can be extended up to $80\deg$ of zenith distance provided that a standard atmospheric model and a full numerical integration of the refraction integral are used. We also provide estimates of the absolute uncertainties associated with the differential refraction corrections and show that approximate formulae can be used up to $80\deg$ of zenith distance for computing these uncertainties. For a given instrumental setup and the knowledge of the uncertainties associated with local weather records, this can be used to fix the maximum zenith distance one can observe depending on the required astrometric accuracy.