Conservation of Angular Momentum A collapsing Star

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SUMMARY

The discussion focuses on the conservation of angular momentum in a collapsing star, specifically when its radius is reduced to half its initial size. Participants confirm that the angular velocity increases due to the conservation principle, leading to a higher angular speed characteristic of neutron stars. The change in rotational kinetic energy can be calculated using the formula for rotational kinetic energy, and the energy is derived from the gravitational forces acting on the star.

PREREQUISITES
  • Understanding of angular momentum conservation principles
  • Familiarity with rotational kinetic energy formulas
  • Basic knowledge of stellar physics and neutron stars
  • Ability to perform calculations involving mass and radius changes
NEXT STEPS
  • Study the conservation of angular momentum in astrophysical contexts
  • Learn how to calculate rotational kinetic energy using I = 2/5MR²
  • Explore the properties and formation of neutron stars
  • Investigate gravitational forces in collapsing stellar bodies
USEFUL FOR

Astronomy students, astrophysicists, and anyone interested in stellar dynamics and the physics of collapsing stars.

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1. After a collapsing star decreases its radius to half its initial size, predict what will happen to its angular velocity(Assume uniform density at all times)Your answer describes the high angular speed of neutron stars. Find the change in the rotational kinetic energy of the star. Where does the energy come from?



I=2/5MR^2 I think the energy comes from the force of the stars own gravity,

I also thought that the angular velocity would increase but I don't know how to find the change in kinetic energy. Any clear explanation would be great, I think I am on the right track but need a little help.



The Attempt at a Solution

 
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You are completely correct about the source of the energy. Find the change in angular velocity using conservation of angular momentum. Use the change in angular velocity to find the change in rotational kinetic energy.
 

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