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Will Oakley
Is there a theoretical limit to the size of neutron stars? It seems likely neutron stars are not simply electrons orbiting a proton so what is their life cycle? Can they just evaporate slowly by neutron decay?
phyzguy said:The neutrons are not free neutrons, so they don't decay. The neutrons are crushed together like a big atomic nucleus. They won't evaporate because they are very tightly gravitationally bound so no matter can really escape. In answer to your question about the maximum size, there is a maximum mass beyond which the neutron star will collapse to a black hole, but we don't know exactly what it is because the exact properties of matter at these densities are only known approximately. The maximum mass is probably somewhere between 2 and 3 solar masses.
phyzguy said:The neutrons are not free neutrons, so they don't decay. The neutrons are crushed together like a big atomic nucleus. They won't evaporate because they are very tightly gravitationally bound so no matter can really escape. In answer to your question about the maximum size, there is a maximum mass beyond which the neutron star will collapse to a black hole, but we don't know exactly what it is because the exact properties of matter at these densities are only known approximately. The maximum mass is probably somewhere between 2 and 3 solar masses.
Will Oakley said:OK, phyzguy. So I'll imagine them as protons in a fixed 3D lattice surrounded by an electron "cloud". For stability all the proton-proton links will be the same at a given star radius, with the links maybe getting shorter at smaller radii due to increasing pressure. Perhaps the protons shrink together until they all touch!
2.5 solar masses are about 5 x 10^30kg, and 3 x 10^57 protons, giving a sphere radius of 9 x 10^18 protons. So a proton radius of 0.86fm would give a star radius of about 7.7km. Does that make any sense?
Do we know if neutron stars rotate?
Ouch!phyzguy said:1000 revolutions per second
Neutrons packed close together repel each other strongly due to the Pauli exclusion principle.Will Oakley said:This begs the question, why does the matter in neutron stars stop shrinking at the proton radius?
None of this makes any sense at all.Will Oakley said:One possible answer is … there is no space to compress and the proton radius indicates the quark size. But a radius of 0.865fm, a circumference of 5.44fm, corresponds to a quantum loop of one 36.3MeV wavelength. The proton radius is uncertain by at least ± 5%, so the the energy is in the range 34.6MeV to 38.1 MeV.
The electron is frequently considered a photon in a toroidal orbit and relativistic by the inverse fine structure constant, 1/α, (= 137), so the EM energy in a frame rotating close to velocity c is 137 x 0.511MeV, (the electron rest mass energy), at about 70MeV. It's perhaps a coincidence that half the spin-1 electron EM energy is 35MeV, within the uncertainty of the 36.3MeV noted above.
There is no such thing.Will Oakley said:my main point was the rigid crystal like proton lattice
That doesn't make any sense.Will Oakley said:But the neutron charge is zero so it seems likely the neutron is an EM wave orbiting a proton with its E field oriented to cancel the proton charge. So perhaps the EM waves in a neutron star bind the protons together in a similar manner to which shared electrons bind atoms in a crystal.
No.Will Oakley said:Are there any theories about neutron stars along this line of thought?
The theoretical limit to the mass of neutron stars is called the Tolman-Oppenheimer-Volkoff Limit, and is approximately 3.0 solar masses. Their paper was published in February 1939. A relatively recent paper (originally published in 2002 and revised in 2013) suggests that the maximum mass limit of a neutron star could be as much as 3.8 solar masses.Will Oakley said:Is there a theoretical limit to the size of neutron stars? It seems likely neutron stars are not simply electrons orbiting a proton so what is their life cycle? Can they just evaporate slowly by neutron decay?
Gravitational collapse is the process by which a massive object, such as a star, collapses under its own gravity, leading to an extremely compact and dense object.
As a star collapses under its own gravity, the pressure and density in its core increases tremendously. At a certain point, the pressure becomes so high that it forces the electrons and protons in the core to combine and form neutrons. This results in a neutron star, which is extremely dense and small in size due to the strong gravitational forces.
No, a Neutron Star cannot continue to collapse infinitely. Once the core of a star has become a neutron star, it is stabilized by the repulsive force between the neutrons, known as neutron degeneracy pressure. This prevents further collapse and limits the size of the neutron star.
Yes, the size limit of a Neutron Star can be affected by various factors such as the mass of the star, its composition, and the strength of its magnetic field. A more massive star will have a larger size limit, while a stronger magnetic field can prevent the collapse of a star into a neutron star.
Yes, there is evidence of the size limit of a Neutron Star. Observations of neutron stars have shown that they have a maximum mass of about 2-3 times the mass of our sun, known as the Tolman-Oppenheimer-Volkoff limit. This provides evidence that gravitational collapse does limit the size of a neutron star.