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The Physics of Neutron Stars
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abstract
Neutron stars are some of the densest manifestations of massive objects in the universe. They are ideal astrophysical laboratories for testing theories of dense matter physics and provide connections among nuclear physics, particle physics and astrophysics. Neutron stars may exhibit conditions and phenomena not observed elsewhere, such as hyperon-dominated matter, deconfined quark matter, superfluidity and superconductivity with critical temperatures near ${10^{10}}$ kelvin, opaqueness to neutrinos, and magnetic fields in excess of $10^{13}$ Gauss. Here, we describe the formation, structure, internal composition and evolution of neutron stars. Observations that include studies of binary pulsars, thermal emission from isolated neutron stars, glitches from pulsars and quasi-periodic oscillations from accreting neutron stars provide information about neutron star masses, radii, temperatures, ages and internal compositions.
Forward citations
Cited by 20 Pith papers
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Fastest spinning millisecond pulsars: indicators for quark matter in neutron stars?
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EP251023a: A fast X-ray transient featuring a magnetar-powered optical internal plateau followed by a steep decay
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QCD phase transition at finite isospin density and magnetic field
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Impact of Anisotropy on Neutron Star Structure and Curvature
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Mass-Gap Neutron Stars from Vector \texorpdfstring{$f(R)$}{f(R)} Gravity Inflationary Deformations
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Probing Neutron Star Interiors and the Properties of Cold Ultra-dense Matter with the SKAO
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