J/A+A/291/155 Rotating neutron stars models. I. (Salgado+, 1994)
High precision rotating neutron star models. I. Analysis of neutron star
properties
SALGADO M., BONAZZOLA S., GOURGOULHON E., HAENSEL P.
<Astron. Astrophys. 291, 155 (1994)>
=1994A&A...291..155S 1994A&A...291..155S (SIMBAD/NED Reference)
ADC_Keywords: Pulsars; Models, evolutionary
Keywords: relativity - stars: neutron; rotating; pulsar; evolution -
equations of state
File Summary:
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File Name Lrecl Records Explanations
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ReadMe 80 . This file
table1 79 568 Neutron star properties at fixed baryon mass
for four equations of state (EOS).
table1.tex 66 3104 LaTeX version of table1
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Byte-by-byte Description of file: table1
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Bytes Format Units Label Explanations
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1- 15 A15 --- EOS EOS Equation of State used
18- 22 F5.3 --- Hc Central pseudoenthalpy
24- 29 F6.3 14.94x10+23kg/m/s2 Ec Central energy-density
31- 36 F6.4 10+4s-1 Omega Rotational frequency
38- 45 F8.4 ms P Period of rotation
48- 52 F5.3 solMass M Gravitational mass
54- 58 F5.3 solMass Beta Baryon mass
60- 65 F6.3 km Rcirc Circunferential (equatorial) radius
67- 71 F5.3 --- cJ/GM2 Angular momentum
73- 79 E7.2 --- |1-lambda| Per cent error indicator
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Note(1): Equation of state
Relativistci model
HKP: Pure neutron matter, n-n interaction mediated via exchange of σ,
ω, π, ρ mesons. Calculating using an effective Lagrangian,
done within the Hartree approximation. This particular model fits
saturation density of nuclear matter n0-0.17fm-3 (Haensel et al. 1981).
Non-relativistic potential models
PandN: Pure neutron matter. Interaction described by the Reid soft core
potential. Ground state calculating using variational method
(Pandharipande 1971). Causal at the densities encountered in
neutron stars.
WFF(UV14+TNI): Nucleon matter in beta equilibrium with electrons and muons.
Interaction described by a two-body Urbana UV14 potential, combined with
a phenomenological three-nucleon TNI interaction. Ground state of matter
calculated in a very good approximation using sophisticated variational
method (Wiringa et al., 1988). Causal at the densities relevant for neutron
stars.
Schematic analytic model
Pol2: Polytrope p = κn^γ,
e=mBn+({kappa/(γ-1))n^γ with κ=1mBfm3
and γ=2. Causal at all n.
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References:
Haensel P. et al., 1981, A&A 102, 299
Pandharipande V.R., 1971, Nucl. Phys. A174, 641
Wiringa R.B. et al., 1988, Phys. rev. C38, 1010
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(End) Patricia Bauer [CDS] 16-Jun-1994