A planet of mass \(M\) has two identical satellites, Satellite A and Satellite B, each of mass \(m\). Satellite A is in a stable circular orbit of radius \(R_A\) around the planet. Satellite B is in a stable elliptical orbit around the same planet. The closest approach of Satellite B to the planet's center (periapsis) is \(R_A\), and its farthest point (apoapsis) is \(R_B\), where \(R_B > R_A\). Figure 1 shows both satellites at the instant they are at the closest approach distance \(R_A\).