The Sun's position in the sky

TL;DR

This paper presents a comprehensive mathematical framework for calculating the Sun's position in the sky based on time and location, including effects like Earth's orbit eccentricity and atmospheric refraction, with practical applications such as predicting Manhattanhenge.

Contribution

It introduces explicit formulas and methods for accurately determining solar position and related phenomena, enhancing precision over previous models.

Findings

Derived direct expressions for solar altitude and azimuth as functions of date and location.

Demonstrated applications include predicting Manhattanhenge and plotting solar trajectories.

Accounted for orbital eccentricity, precession, and atmospheric effects for improved accuracy.

Abstract

We express the position of the Sun in the sky as a function of time and the observer's geographic coordinates. Our method is based on applying rotation matrices to vectors describing points on the celestial sphere. We also derive direct expressions, as functions of date of the year and geographic latitude, for the duration of daylight, the maximum and minimum altitudes of the Sun, and the cardinal directions to sunrise and sunset. We discuss how to account for the eccentricity of the earth's orbit, the precessions of the equinoxes and the perihelion, the size of the solar disk, and atmospheric refraction. We illustrate these results by computing the dates of "Manhattanhenge" (when sunset aligns with the east-west streets on the main traffic grid for Manhattan, in New York City), by plotting the altitude of the Sun over representative cities as a function of time, and by showing plots ("analemmas") for the position of the Sun in the sky at a given hour of the day.