Neutron-degenerate matter allows velocities close to speed of light, because e . g . the speed of neutron-star oscillations is relativistic; however; these bodies cannot strictly be said to be " rigid " ( per Born rigidity ).
42.
And if you use truly extreme pressures, it will compress a lot ( it's not anywhere close to electron degenerate matter, much less neutron degenerate matter ) .-- talk ) 01 : 14, 3 September 2011 ( UTC)
43.
And if you use truly extreme pressures, it will compress a lot ( it's not anywhere close to electron degenerate matter, much less neutron degenerate matter ) .-- talk ) 01 : 14, 3 September 2011 ( UTC)
44.
These are not, as the name suggests, perverts hanging around the dark alleys of the universe, but things like black holes, white dwarfs and neutron stars _ the burned-out hulks of long-dead stars that physicists call " degenerate matter ."
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:: : On the contrary, there is a very real possibility that the interior of the neutron star, being made of degenerate matter, will be some kind of superfluid . talk ) 14 : 51, 23 November 2011 ( UTC)
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As a result, in matter with approximately equal numbers of protons and electrons, proton degeneracy pressure is much smaller than electron degeneracy pressure, and proton degeneracy is usually modeled as a correction to the equations of state of electron-degenerate matter.
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Once the temperature reaches 100 million 200 million kelvin and helium fusion begins using the triple-alpha process, the temperature rapidly increases, further raising the helium fusion rate and, because degenerate matter is a good conductor of heat, widening the reaction region.
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As I understand the Wikipedia articles, eventually the Sun becomes a red giant following the asymptotic giant branch, until the core consists of degenerate matter and undergoes a helium flash that drives it out on the horizontal branch, but only temporarily.
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Sufficiently dense matter containing protons experiences proton degeneracy pressure, in a manner similar to the electron degeneracy pressure in electron-degenerate matter : protons confined to a sufficiently small volume have a large uncertainty in their momentum due to the Heisenberg uncertainty principle.
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Without electrons, which keep nuclei apart, the neutrons collapse into a dense ball ( in some ways like a giant atomic nucleus ), with a thin overlying layer of degenerate matter ( chiefly iron unless matter of different composition is added later ).
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