33533022113212(2.7 10 m/s) (1.70 days)(86400 s/day)6.90 10 kg()22(6.6710m/kgs)3.467,smvTmmGMππ−×===×+×⋅=where301.99 10 kgsM=×is the mass of the sun. With 16smM=, we write 2sα=and solve the following cubic equation for :323.4670(6)−=+.The equation has one real solution: 9.3=, which implies 2/9s≈.56. The two stars are in circular orbits, not about each other, but about the two-star system’s center of mass (denoted as O), which lies along the line connecting the centers of the two stars. The gravitational force between the stars provides the centripetal force necessary to keep their orbits circular. Thus, for the visible, Newton’s second law gives
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