Two planets \(P_1\) and \(P_2\) having masses \(M_1\) and \(M_2\) revolve around the Sun in elliptical orbits, with time periods \(T_1\) and \(T_2\), respectively. The minimum and maximum distances of planet \(P_1\) from the Sun are \(R\) and \(3R\), respectively, whereas for planet \(P_2\), these are \(2R\) and \(4R\), respectively, where \(R\) is a constant. Assuming \(M_1\) and \(M_2\) are much smaller than the mass of the Sun, the magnitude of \(\dfrac{T_2}{T_1}\) is: