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Complete relativistic equation of state for neutron stars

H. Shen
(
)

Feb, 2002

23 pages

Published in:

Phys.Rev.C 65 (2002) 035802

e-Print:

nucl-th/0202030 [nucl-th]

DOI:

10.1103/PhysRevC.65.035802

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Abstract:

We construct the equation of state (EOS) in a wide density range for neutron stars using the relativistic mean field theory. The properties of neutron star matter with both uniform and non-uniform distributions are studied consistently. The inclusion of hyperons considerably softens the EOS at high densities. The Thomas-Fermi approximation is used to describe the non-uniform matter, which is composed of a lattice of heavy nuclei. The phase transition from uniform matter to non-uniform matter occurs around

0.06 \rm{fm^{-3}}

, and the free neutrons drip out of nuclei at about

2.4 \times 10^{-4}\ \rm{fm^{-3}}

. We apply the resulting EOS to investigate the neutron star properties such as maximum mass and composition of neutron stars.

24.10.Jv
21.65.+f
26.60.+c
n: matter
mean field approximation: relativistic
critical phenomena
hyperon: coupling
Thomas-Fermi approximation
star: mass
nucleon: density

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