Collapsars vrs. QM degeneracy pressure

In summary, the QM degeneracy pressure puts up a fight but the immensity of the star wins out. This is because the Pauli exclusion principle won't let the electrons lose heat as gravity would normally take over, but gravity can still win by releasing energy before the system reaches its ground state.
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Helios
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The QM degeneracy pressure puts up a fight but the immensity of the star wins out. Why is this? Is the Pauli Exclusion Principle really a principle? Why does it surrender in this case?
 
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From white dwarf to neutron star, the electrons are forced to combine with protons to form neutrons. Neutron stars collapsing to black holes is unknown - could be quark gluon soup.
 
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Or if strings have anything to do with it, quark gluon soup with noodles.
 
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You can read the book of Pranab Gosh, "Rotation and Accretion Powered Pulsars", ch. 2 about this. But this phenomena is something like this: there is a range for every interaction all over the universe. For instance, almost all of the celestial objects are dipole dominated magnets but we don't see that they're pushing each other away (this is not exactly the same case but just an example). So, the Pauli exclusion principle is really a principle but in that kind of circumstances, I mean under such a huge degeneracy pressure and in such a tiny volume, it can not work as usual. All of the particles are lined up in the Fermi surface. In the so-called "well potential" examples as we know that the principle is valid, the mean range is always taken about the atomic range, 10^{-15} meters. For further info, you should read the chapter that I've mentioned above.
 
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Helios said:
The QM degeneracy pressure puts up a fight but the immensity of the star wins out. Why is this? Is the Pauli Exclusion Principle really a principle? Why does it surrender in this case?
The Pauli exclusion principle never surrenders, all the principle says is that the electrons reach a ground state where they cannot lose any more heat. Losing heat is normally how a star gradually succumbs to gravity, but the PEP prevents that from proceeding to its ultimate conclusion. However, there is still a way that gravity can win out-- by releasing enough energy to make the electrons go relativistic before the whole system reaches its ground state. Relativistic electrons have a different relationship between momentum and kinetic energy, which makes them able to be in their ground state without uniquely specifying a radius-- any radius will do. This makes them susceptible to drastic contraction, especially if processes are going on (like neutronization) that remove kinetic energy via the escape of neutrinos. So we should not say the PEP surrenders, we should say that gravity finds a way to collapse the core without violating the PEP.
 
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1. What is a collapsar and how does it relate to quantum degeneracy pressure?

A collapsar is a type of massive, rotating star that has reached the end of its life and collapsed under its own gravity. This collapse creates a supernova explosion and can result in the formation of a black hole. Quantum degeneracy pressure is a fundamental force that counteracts gravity in very dense objects, such as a collapsar, and prevents it from collapsing further.

2. How does quantum degeneracy pressure differ from other types of pressure?

Quantum degeneracy pressure is a result of the Pauli exclusion principle, which states that two particles cannot occupy the same quantum state. This creates a repulsive force between particles in a dense object, unlike other types of pressure which are caused by collisions or thermal energy.

3. Can quantum degeneracy pressure prevent the collapse of a collapsar into a black hole?

Quantum degeneracy pressure can only delay the collapse of a collapsar, but it cannot prevent it entirely. As the star continues to collapse and reach higher densities, the quantum degeneracy pressure becomes insufficient to counteract the force of gravity, resulting in the formation of a black hole.

4. How does the mass of a collapsar affect the strength of quantum degeneracy pressure?

The strength of quantum degeneracy pressure is directly proportional to the mass of the star. This means that the more massive the collapsar, the stronger the quantum degeneracy pressure will be, and the longer it will take for the star to collapse into a black hole.

5. How does the rotation of a collapsar affect its collapse and the strength of quantum degeneracy pressure?

The rotation of a collapsar can impact its collapse in two ways. First, it can create a centrifugal force that counteracts the force of gravity, delaying the collapse. Second, the rotation can also increase the density of the star, making quantum degeneracy pressure stronger and further delaying the collapse. However, if the rotation becomes too fast, it can overcome the quantum degeneracy pressure and lead to the formation of a black hole.

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