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