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In some pulsars off-pulse emission is detected. In fact it is coherent emission resulting from cyclotron resonance between highly energetic primary particles and the low gamma secondary particles in the pulsar magnetosphere

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Before the escape velocity reach the light speed, photons, which are produced on the star can escape from there and therefore star can shine (it does not have to be a visible light, though). As you have pointed out, while the mass of the star increases the escape velocity rires too. At some point of time, this velocity, as calculated, is higher then the ...

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In a neutron star there are mostly "free" neutrons and the question then is why they don't all beta decay into electrons and protons? Well, some of them do, but the point is that when the electron (or proton, there are equal numbers of each) numbers build up then they become degenerate (meaning no more than two electrons can occupy the same energy state and ...

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Regarding neutrons in neutron stars the answer is a direct extension of the argument use by madR. In a neutron star there are mostly "free" neutrons and the question then is why they don't all beta decay into electrons and protons? Well, some of them do, but the point is that when the electron/proton (there are equal numbers of each) numbers build up then ...

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How about this: In an $n,p,e$ gas the ratio of neutrons to protons decreases with density. For ideal degenerate gases the Fermi energies are related by $E_{F,n} = E_{F,p} + E_{F,e}$. In this situation, the largest the proton to neutron ratio can become is 1/8 when all the particles are ultra-relativistic at infinite density. To conserve momentum in the ...

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