A power series solution to this scientist's equation converges in the Laplace limit.
A power series solution to this scientist's equation converges in the Laplace limit. Given a solution to this scientist's equation at a given time, the solution at future times can be calculated simply using the F and G functions, which are sometimes called the Lagrange coefficients. That equation named for this scientist is a transcendental equation that relates mean anomaly to eccentric anomaly. A vector equal to p cross L minus mÂ kÂ r-hat is conserved in this scientist's namesake (*) problems, which involve two bodies interacting via a central and inverse-square force. One of his laws states that the square of the period is proportional to the cube of the semi-major axis, while another of his laws states that the radius vector of an orbit sweeps out "equal areas in equal times." For 10 points, name this scientist who proposed three laws of planetary motion.
A power series solution to this scientist's equation converges in the Laplace limit.
Johannes Kepler