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This is a translation from Latin of E348 'Methodus facilis motus corporumcoelestium utcunque perturbatos ad rationem calculi astronomici revocandi', inwhich Euler develops a method to alleviate the astronomical computations in atypical celestial three-body problem represented by Sun, Earth and Moon. Inthis work, Euler's approach consists of two parts: geometrical and mechanical.The geometrical part contains most of the analytical developments, in whichEuler makes use of Cartesian and spherical trigonometry as well - the latternot always in a clear enough way. With few sketches to show the geometricalconstructions envisaged by Euler - represented by several geometrical variables-, it is a hard to follow publication. The Translator, on trying to clear theway to the non-specialized reader, used the best of his abilities to add hisown figures to the translation. In the latter part of the work, Eulerparticularizes his developments to the Moon, ending up with eight coupleddifferential equations for resolving the perturbed motion of this celestialbody, which makes his claim of an "easy method" as being rather fallacious.Despite showing great analytical skills, Euler did not give indications on howthis system of equations could be solved, which renders his efforts practicallyuseless in the determination of the variations of the nodal line andinclination of the Moon's orbit.

A translation of L. Euler's "An easy method for calculating the motion  of celestial bodies perturbed in any manner avoiding astronomical  computations"