<Dd> F (r) = k m 1 m 2 r 2 exp ⁡ (− α r) (\ displaystyle F (r) = k (\ frac (m_ (1) m_ (2)) (r ^ (2))) \ exp (- \ alpha r)) (Laplace) </Dd> <Dd> F (r) = k m 1 m 2 r 2 (1 + α r 3) (\ displaystyle F (r) = k (\ frac (m_ (1) m_ (2)) (r ^ (2))) \ left (1 + (\ alpha \ over (r ^ (3))) \ right)) (Decombes) </Dd> <P> In recent years, quests for non-inverse square terms in the law of gravity have been carried out by neutron interferometry . </P> <P> The n - body problem is an ancient, classical problem of predicting the individual motions of a group of celestial objects interacting with each other gravitationally . Solving this problem--from the time of the Greeks and on--has been motivated by the desire to understand the motions of the Sun, planets and the visible stars . In the 20th century, understanding the dynamics of globular cluster star systems became an important n - body problem too . The n - body problem in general relativity is considerably more difficult to solve . </P>

Prove mathematically universal law of gravitation with diagram