A unified equation of state of dense matter and neutron star structure
نویسندگان
چکیده
منابع مشابه
Neutron Star Radii, Core-collapse Supernovae, and the Equation of State of Dense Matter
Neutron star mass and radius measurements are becoming sufficiently accurate as to offer astrophysical constraints on the properties of neutron-rich matter near the nuclear saturation density. Current observations, which imply that the radius of a 1.4 solar mass neutron star lies between 10.4 and 12.9 km (95% confidence), also imply that 43 < L < 67 MeV, where L is a parameter describing the sl...
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Properties of dense nucleon matter and the structure of neutron stars are studied using variational chain summation methods and the new Argonne v18 two-nucleon interaction, which provides an excellent fit to all of the nucleonnucleon scattering data in the Nijmegen data base. The neutron star gravitational mass limit obtained with this interaction is 1.67M⊙ . Boost corrections to the two-nucleo...
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The sudden spin jumps, or glitches, commonly seen in isolated neutron stars are thought to represent angular momentum transfer between the crust and the liquid interior [1]. In this picture, as a neutron star’s crust spins down under magnetic torque, differential rotation develops between the stellar crust and a portion of the liquid interior. The more rapidly rotating component then acts as an...
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The structure of neutron stars is considered from theoretical and observational perspectives. We demonstrate an important aspect of neutron star structure: the neutron star radius is primarily determined by the behavior of the pressure of matter in the vicinity of nuclear matter equilibrium density. In the event that extreme softening does not occur at these densities, the radius is virtually i...
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ژورنال
عنوان ژورنال: Astronomy & Astrophysics
سال: 2001
ISSN: 0004-6361,1432-0746
DOI: 10.1051/0004-6361:20011402