Kepler's Equation

Kepler’s Equation


a transcendental equation of the form

yc sin y = x

The case |c| < 1 is important for applications, when is y determined from c and x in a unique manner. The equation was first examined by J. Kepler (Astronomía nova, 1609) in connection with the following problem: point D is given on the diameter AB of the semicircle AOBM; draw a line DM such that it divides the

Figure 1

area of the semicircle in a given ratio (see Figure 1). Kepler’s equation plays an important role in astronomy in the determination of the elements of the elliptical orbits of the planets. In celestial mechanics the equation is usually written in the form

E – e sin E = M

where e is the eccentricity of the ellipse, M is the mean anomaly, and E is the eccentric anomaly. The solution of Kepler’s equation also occupied J. Lagrange (1771), P. Laplace (1823), F. Bessel (1816–17), K. Gauss (1809), and others.


Subbotin, M. F. Kurs nebesnoi mekhaniki, 2nd ed., vol. 1. Leningrad-Moscow, 1941.
References in periodicals archive ?
Kepler's equations pertained to planets in our solar system.