Resisting Collapse: The Physics Behind a Star's Stability

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A star resists gravitational collapse through the process of nuclear fusion, which generates high pressure within its core. This pressure is crucial for maintaining equilibrium against gravitational forces. In white dwarfs, the stability is achieved through electron degeneracy pressure, a consequence of Pauli's exclusion principle that prevents electrons from occupying the same quantum state. If a star exceeds the Chandrasekhar limit of 1.4 solar masses, electron degeneracy pressure fails, leading to further collapse into a neutron star or black hole. Understanding these principles is essential for grasping stellar evolution and stability.
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of how a star is able to resist collapsing under its own gravitational attraction??
 
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I wonder if there might be anything going on inside the star, pushing out?
 
nuclear fusion = high pressure, I think.
 
The pressure inside a white dwarf (a collapsed star) which remains in equiblirum with the gravitational attraction is the result of Pauli's exclusion principle, which states that two electrons cannot occupy the same quantum state at the same time. This principle gives rise to what is called electron degeneracy pressure and is what counteracts gravitational contraction. If the mass of the original star is greater than 1.4 solar masses (the Chandrasekhar limit), the electron degeneracy pressure will not be sufficient to counteract gravity, and the star will collapse further into either a neutron star or a black hole.
 
thanks for helping me to better understand :smile:
 

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