Two stars of masses M and m, separated by a distance d, revolve in circular orbits about their center of mass (Fig. P13.69). Show that each star has a period given by T2 = 4π2d3/G (M + m) Proceed as follows: Apply Newton€™s second law to each star. Note that the center-of-mass condition requires that Mr2 = mr1, where r1 + r2 = d.

M2 CM Figure P13.69