Physics (10th Edition)

Published by Wiley
ISBN 10: 1118486897
ISBN 13: 978-1-11848-689-4

Chapter 9 - Rotational Dynamics - Problems - Page 247: 60



Work Step by Step

Angular momentum is conserved, so $$I_0\omega_0=I_f\omega_f$$ Before the explosion, the star is a solid sphere of radius R, so $I_0=\frac{2}{5}MR^2$ After the explosion, the star is a thin-walled shell of radius 4R, so $I_f=\frac{2}{3}M(4R)^2=\frac{32}{3}MR^2$ Therefore, $$\frac{\omega_f}{\omega_0}=\frac{I_0}{I_f}=\frac{3}{80}$$ $$\omega_f=\frac{3}{80}(2rev/day)=0.075rev/day$$
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