Methods for numerical integration of equations of motion of stationary satellites

A three-step numerical integration method for the motion equations of stationary satellites is presented with attention to the simplification of computer programming without reducing accuracy. In the first step, gravity and centrifugal force are eliminated from the equations by the establishment of a coordinate whose origin is at the satellite point, and which revolves around the earth with the satellite. The second step consists of a simplification of the tesseral harmonics resulting from earth-satellite interaction. Finally, the equations are integrated using formulas equivalent to the Taylor series, whose terms of