What prevents a star from collapsing under its own gravitational attraction?

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SUMMARY

Stars resist collapsing under their own gravitational attraction due to several counteracting forces. In the case of our sun, nuclear fusion generates significant heat and radiation, creating radiation pressure that maintains equilibrium. For white dwarfs, electron degeneracy pressure, a quantum effect, prevents collapse by limiting the number of electrons in a given volume. Neutron stars experience a similar phenomenon known as neutron degeneracy pressure, which arises from the behavior of neutrons under extreme conditions.

PREREQUISITES
  • Newton's Law of Gravitation
  • Nuclear fusion processes in stars
  • Concept of radiation pressure
  • Quantum mechanics principles, specifically electron and neutron degeneracy pressure
NEXT STEPS
  • Study the mechanics of nuclear fusion in stars
  • Explore the concept of radiation pressure in astrophysics
  • Investigate electron degeneracy pressure and its implications in white dwarfs
  • Learn about neutron degeneracy pressure in neutron stars
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Astronomers, astrophysics students, and anyone interested in stellar dynamics and the forces that govern star stability.

nlink1979
According to Newton's Law of Gravitation, all objects with mass attract one another. This law implies that all of the atoms that make up a star, such as our sun, are gravitationally attracted to one another. How is a star able to resist collapsing under its own gravitational attraction?

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Nicole
 
Physics news on Phys.org
There are numerous interactions that counteract gravity, preventing such a collapse. In our sun, the process of nuclear fusion creates large amounts of heat and radiation; this radiation pressure keeps the star in equilibrium. In stars like white dwarfs, something called electron degeneracy pressure keeps the star from collapsing. This is a quantum effect that restricts the number of electrons we can squish into a certain volume, and acts to keep them apart. In neutron stars, a similar pressure arises from neutron degeneracy.
 

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