Neutron star

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A neutron star is a type of stellar remnant that can result from the gravitational collapse of a massive star during a Type II, Type Ib or Type Ic supernova event. Such stars are composed almost entirely of neutrons, which are subatomic particles without electrical charge and a slightly larger mass than protons. Neutron stars are very hot and are supported against further collapse because of the Pauli exclusion principle. This principle states that no two neutrons (or any other fermionic particle) can occupy the same place and quantum state simultaneously.

A typical neutron star has a mass between 1.35 and about 2.1 solar masses, with a corresponding radius of about 12 km if the Akmal-Pandharipande-Ravenhall equation of state (APR EOS) is used.[1][2] In contrast, the Sun's radius is about 60,000 times that. Neutron stars have overall densities predicted by the APR EOS of 3.7×1017
to 5.9×1017
 kg/m3
(2.6×1014
to 4.1×1014
times the density of the Sun),[3] which compares with the approximate density of an atomic nucleus of 3×1017
 kg/m3
.[4] The neutron star's density varies from below 1×109
 kg/m3
in the crust increasing with depth to above 6×1017
or 8×1017
 kg/m3
deeper inside.[5] This density is approximately equivalent to the mass of the entire human population compressed to the size of a sugar cube.[6]

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