Three stars of equal mass $$M$$ rotate in a circular path of radius $$r$$ about their center of mass such that the stars always remain equidistant from each other. The common angular speed $$\omega$$ of rotation of the stars can be expressed as

A

$$\left(\frac{GM\sqrt3}{r^3}\right)^{1/2}$$

B

$$\left(\frac{GM}{r^3}\right)^{1/2}$$

C

$$\left(\frac{2GM}{\sqrt3 r^3}\right)^{1/2}$$

D

$$\left(\frac{GM}{\sqrt3 r^3}\right)^{1/2}$$