(m) (m In Kepler's two-body motion, if one of the objects is not more massive compared to the other, the motion of both objects must be taken into account. We observe this in almost all two-star systems. The simplest case is for two stars with equal masses m. Suppose that they are in a circular with radius r. At any given time, the velocities of both stars are opposite and have exactly the same magnitude. (a) Find the speed v of the stars. U = (b) Find the period T of the motion. T =
(m) (m In Kepler's two-body motion, if one of the objects is not more massive compared to the other, the motion of both objects must be taken into account. We observe this in almost all two-star systems. The simplest case is for two stars with equal masses m. Suppose that they are in a circular with radius r. At any given time, the velocities of both stars are opposite and have exactly the same magnitude. (a) Find the speed v of the stars. U = (b) Find the period T of the motion. T =
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In Kepler's two-body motion, if one of the objects
is not more massive compared to the other, the
motion of both objects must be taken into
account. We observe this in almost all two-star
systems. The simplest case is for two stars with
equal masses m. Suppose that they are in a
circular with radius r. At any given time, the
velocities of both stars are opposite and have
exactly the same magnitude.
(a) Find the speed v of the stars.
U =
(b) Find the period T of the motion.
T =
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