The discussion focuses on deriving the expression for the square of the orbital period, T^2, from the formula T = 2*pi*R^(3/2)/sqrt(G*M). By squaring the original equation, the result is T^2 = 4*pi^2*R^3/G*M. This formulation simplifies the variables, allowing for a clearer representation of the relationship between the orbital period and the semi-major axis. The expression is rooted in Kepler's third law, emphasizing that the square of the orbital period is proportional to the cube of the semi-major axis. This derivation aids in calculating the orbital period for various celestial objects based on their mass and distance.