Results 281 to 290 of about 20,312 (304)
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Physical Review Letters, 1993
We calculate properties of neutron star matter at subnuclear densities using an improved nuclear Hamiltonian. Nuclei disappear and the matter becomes uniform at a density of about 0.6n(s), where n(s) of about 0.16/cu fm is the saturation density of nuclear matter. As a consequence, the mass of matter in the crusts of neutron stars is only about half as
, Lorenz, , Ravenhall, , Pethick
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We calculate properties of neutron star matter at subnuclear densities using an improved nuclear Hamiltonian. Nuclei disappear and the matter becomes uniform at a density of about 0.6n(s), where n(s) of about 0.16/cu fm is the saturation density of nuclear matter. As a consequence, the mass of matter in the crusts of neutron stars is only about half as
, Lorenz, , Ravenhall, , Pethick
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Nuclear Physics A, 1971
Abstract The matter in neutron stars is essentially in its ground state and ranges in density up to and beyond 3 × 10 14 g/cm 3 , the density of nuclear matter. Here we determine the constitution of the ground state of matter and its equation of state in the regime from 4.3 × 10 11 g/cm 3 where free neutrons begin to “drip” out of the nuclei, up ...
GORDON BAYM +2 more
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Abstract The matter in neutron stars is essentially in its ground state and ranges in density up to and beyond 3 × 10 14 g/cm 3 , the density of nuclear matter. Here we determine the constitution of the ground state of matter and its equation of state in the regime from 4.3 × 10 11 g/cm 3 where free neutrons begin to “drip” out of the nuclei, up ...
GORDON BAYM +2 more
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Astrophysics and Space Science, 1975
Current theories, and the astrophysical implications, of the nature of high density neutron star matter are reviewed. Suggestions are made for a compromise between the alternatives of neutron crystallization and pion condensation.
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Current theories, and the astrophysical implications, of the nature of high density neutron star matter are reviewed. Suggestions are made for a compromise between the alternatives of neutron crystallization and pion condensation.
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Merger and Postmerger of Binary Neutron Stars with a Quark-Hadron Crossover Equation of State
Physical Review Letters, 2022Hajime Sotani +2 more
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The equation of state of hot, dense matter and neutron stars
Physics Reports, 2016James Lattimer, Madappa Prakash
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Thermal luminosities of cooling neutron stars
Monthly Notices of the Royal Astronomical Society, 2020Alexander Potekhin, Mikhail Beznogov
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The masses and spins of neutron stars and stellar-mass black holes
Physics Reports, 2015Cole Miller
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Approximate universal relations for neutron stars and quark stars
Physics Reports, 2017Nicolas Yunes, Kent Yagi
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