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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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Identification of strontium in the merger of two neutron stars
Nature, 2019Half of all of the elements in the Universe that are heavier than iron were created by rapid neutron capture. The theory underlying this astrophysical r-process was worked out six decades ago, and requires an enormous neutron flux to make the bulk of the
D. Watson +17 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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Superfluidity in the Interiors of Neutron Stars
, 2019The discoveries of more than 400 neutron stars as radio pulsars continue to provide an intellectual challenge to physicists and astronomers with diverse backgrounds.
J. Sauls
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Superfluidity in nuclear systems and neutron stars
European Physical Journal A, 2018.Nuclear matter and finite nuclei exhibit the property of superfluidity by forming Cooper pairs. We review the microscopic theories and methods that are being employed to understand the basic properties of superfluid nuclear systems, with emphasis on the
A. Sedrakian, J. W. Clark
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Black Holes, White Dwarfs, and Neutron Stars
, 1983S. Shapiro, S. Teukolsky
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