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How do neutron stars overcome neutron degeneracy? - Physics Stack Exchange
Neutron stars and General Relativity In neutron stars, the reason for the upper limit is also because hydrostatic equilibrium cannot be reached, either because of the increasing density (even if the neutrons remain intact) but possibly accelerated if the neutrons are removed.
Can there be Electron and/or Proton Stars? - Physics Stack Exchange
What happens to all of the electrons and protons in the material of a neutron star? Could there ever be an electron star or a proton star?
thermodynamics - What is the core temperature of neutron star as a ...
From 100- $10^5$ years, the interior becomes isothermal and neutrino cooling dominates over photon cooling. The details of how the interior (and hence surface) temperature behaves then depends greatly on the composition of the core, hence the mass of the neutron star, and the extent to which superfluidity operates in the neutron fluid.
How do neutron stars burn? Is it decay or fusion or something else?
Second, neutron stars have a maximum possible mass, dictated by the rules of general relativity and the mass of a neutron. If a neutron star has extra mass beyond this dumped on its surface (say, because it is orbiting an ordinary star, and that star accretes mass onto the NS), they can explode in a violent way.
Position of Neutron Stars in H R diagrams - Physics Stack Exchange
The HR diagram is an . Whilst neutron stars could be placed in the HR diagram in the same way as white dwarf stars are, it turns out to be impractical to do so because the luminosity and temperature of neutron stars is next to impossible to determine. The reason for this is two-fold: (i) Neutron stars start off very hot (interior temperatures of ∼1010 ∼ 10 10 K and photospheric ...
astrophysics - What is the theoretical lower mass limit for a ...
But, I think this is not the smallest possible neutron star mass - it is only the smallest mass that can be produced by stellar evolution processes. For example, black holes have also a lower limit: the Tolman-Oppenheimer-Volkoff limit, which is around 1.5-3.0 Solar masses.
How do neutron stars emit black body radiation?
Neutron stars have a charged components (mostly protons and electrons). For pure neutron matter, it is possible to consider non-minimal coupling of the neutron with the electromagnetic field (minimal coupling is via the monopole: the electric charge) Role of the vacuum energy in the thermodynamics of neutron matter.
What happens to Protons and Electrons when a Neutron star forms?
What happens to Protons and Electrons when a Neutron star forms? At some point gravity overcomes the Pauli Exclusion Principle ( I assume) and they are all forced together. What happens in the proc...
Size and density of neutron stars - Physics Stack Exchange
These are kind of "order of magnitude" estimates determined by balancing neutron degeneracy pressure with the gravitational force exerted by a rough range of stellar masses. Typically, the result is that the acceptable range of masses results in neutron stars with radii on the order of 10 km. There have been attempts to confirm this experimentally using Doppler effects on accreting matter and ...
Is the speed of sound almost as high as the speed of light in neutron ...
In the center of a neutron star you get quite close to this. Interaction change this result by factors of order one (indeed, recent observations of neutron star masses and radii suggest that the speed of sound near the center is close to c c), but as an order of magnitude estimate these simple results are quite good.
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