During its evolution, a star of 1 solar mass (the mass of our Sun) expands to 3.33 times its original radius. Assume that, during this expansion:

- the star has no appreciable loss of mass

- the mass is uniformly distributed through the volume

- the star remains spherical during the entire process

a) If the star was initially spinning with a period of To = 36.9 days: find Tf, the period of rotation of the star after the expansion

1 days

b) Calculate the ratio R., where

R = (final kinetic energy of the star)/(initial kinetic energy of the star)

NOTE: You may assume there is no translational motion.

R = 2

- the star has no appreciable loss of mass

- the mass is uniformly distributed through the volume

- the star remains spherical during the entire process

a) If the star was initially spinning with a period of To = 36.9 days: find Tf, the period of rotation of the star after the expansion

1 days

b) Calculate the ratio R., where

R = (final kinetic energy of the star)/(initial kinetic energy of the star)

NOTE: You may assume there is no translational motion.

R = 2

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