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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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European Physical Journal A, 2018
.By numerically inverting the Tolman-Oppenheimer-Volkov (TOV) equation using an explicitly isospin-dependent parametric Equation of State (EOS) of dense neutron-rich nucleonic matter, a restricted EOS parameter space is established using observational ...
Nai-Bo Zhang, Bao-An Li
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.By numerically inverting the Tolman-Oppenheimer-Volkov (TOV) equation using an explicitly isospin-dependent parametric Equation of State (EOS) of dense neutron-rich nucleonic matter, a restricted EOS parameter space is established using observational ...
Nai-Bo Zhang, Bao-An Li
semanticscholar +1 more source
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
D. G. Ravenhall +2 more
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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
D. G. Ravenhall +2 more
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Astrophysics and Cosmology, 2016
Radio pulsars are unique laboratories for a wide range of physics and astrophysics. Understanding how they are created, how they evolve and where we find them in the Galaxy, with or without binary companions, is highly constraining of theories of stellar and binary evolution.
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Radio pulsars are unique laboratories for a wide range of physics and astrophysics. Understanding how they are created, how they evolve and where we find them in the Galaxy, with or without binary companions, is highly constraining of theories of stellar and binary evolution.
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Physics Letters A, 1968
Abstract It is shown that the radio observations of a rapidly pulsating source are consistent with its identification as a blue star. The determined position of this star in the HR diagram places it in the dwarf region.
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Abstract It is shown that the radio observations of a rapidly pulsating source are consistent with its identification as a blue star. The determined position of this star in the HR diagram places it in the dwarf region.
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1979
To determine the detectability of thermal radiation from the surface of a neutron star, the surface temperature as a function of time is needed. To find this, the surface temperature as a function of core temperature is found; this ratio depending on temperature, stellar mass, and magnetic field strength. The energy loss rates from photon emission and
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To determine the detectability of thermal radiation from the surface of a neutron star, the surface temperature as a function of time is needed. To find this, the surface temperature as a function of core temperature is found; this ratio depending on temperature, stellar mass, and magnetic field strength. The energy loss rates from photon emission and
openaire +2 more sources