Abstract
The ecliptic and equatorial coordinates discussed so far are specified in terms of the mean plane of the Earth’s orbit and of the position of the Earth’s axis. Neither of these systems is particularly suitable, however, for an observer situated on the surface of the Earth. As such an observer (without being aware of it) takes part in the Earth’s daily rotation, it appears as if the Sun, Moon, and stars follow large arcs across the sky from East to West during the course of a day, reaching their highest point above the horizon when they are on the meridian.
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References
L. D. Schmadel, G. Zech; Empirical transformations from UT to ET for the period 1800–1988; Astronomische Nachrichten, vol. 309, pp. 219–221 (1988). Representation of the observed difference between Universal Time and Ephemeris Time by a 12th-order polynomial, with validity over a period of almost 200 years.
Algorithms for the calculation of rising and setting of objects and for handling refraction are given in Almanac for Computers [3].
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© 1998 Springer-Verlag Berlin Heidelberg
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Montenbruck, O., Pfleger, T. (1998). Calculation of Rising and Setting Times. In: Astronomy on the Personal Computer. Springer, Berlin, Heidelberg. https://doi.org/10.1007/978-3-662-03349-4_3
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DOI: https://doi.org/10.1007/978-3-662-03349-4_3
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