J/A+AS/108/455 Rotating neutron stars models. II. (Salgado+, 1994)
High precision rotating neutron star models. II. Large sample of neutron
stars properties
SALGADO M., BONAZZOLA S., GOURGOULHON E., HAENSEL P.
<Astron. Astrophys. Suppl. Ser. 108, 455 (1994)>
=1994A&AS..108..455S 1994A&AS..108..455S (SIMBAD/NED Reference)
ADC_Keywords: Pulsars; Models, evolutionary
Keywords: relativity - stars: neutron; rotation; pulsar - equations of state
File Summary:
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File Name Lrecl Records Explanations
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ReadMe 80 . This file
tables 79 2274 Neutron star properties at fixed baryon mass
for four equations of state (EOS).
tables.tex 78 6746 LaTeX version of tables
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Byte-by-byte Description of file: tables
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Bytes Format Units Label Explanations
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1- 16 A16 --- EOS EOS Equation of State used (1)
18- 22 F5.3 ---- Hc Central pseudoenthalpy
24- 29 F6.3 14.94x10+23kg/m/s2 Ec Central energy-density in Rho_nuc.c2
31- 36 F6.4 10+4s-1 Omega Rotational frequency
38- 45 F8.4 ms P []? Period of rotation
46 A1 --- n_P A 'i' means infinity
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): Equations of state
Relativistiv models
DiazII: Pure neutron matter, n-n interaction mediated via exchange of
σ, π, ρ, ω mesons. Ground state calculated by using
renormalized Hartree approximation (Diaz Alonso 1985).
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).
Glend1: "Case 1" model of Glendenning (1985). Baryon matter including
nucleons, hyperons, {DELTA}s, and a pion condensate, in beta equilibrium
with leptons. Strong interactions described by an effective Lagrangian,
including couplings of baryons to σ, ω, π, ρ, K mesons.
Couplings of hyperons to meson fields reduced as compared to those of
nucleons and {DELTA}s. Hartree approximation for the ground state.
Glend2: "Case 2" model of Glendenning (1985). Similar to Glend1, but with no
pion condensation because of an assumed repulsion between couplings of all
baryons.
Glend3: "Case 3" model of Glendenning (1985). Similar to Glend2, but with
universal couplings of all baryons.
WGW: For nb<0.3fm-3, neutron matter described using {LAMBDA}00 ladder
approximation, with realistic Bonn meson-exchange interaction. For
n>0.3fm-3, baryon matter described using relativistic Hartree
approximation with effective Lagrangian, including couplings of nucleons
and hyperons to σ, ω, π, ρ, η, δ mesons
(Weber et al. 1991).
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.
BJ1: Baryon matter composed of nucleons, hyperons and {DELTA}s, in beta
equilibrium with leptons. Baryon-baryon interaction described by the
modified Reid soft core potential. Ground state calculated using
variational method. This is model IH of Bethe & Johnson (1974) (see also
Malone et al. 1975). Causal at the densities encountered in neutron stars.
FP: Neutron matter, with nucleon-nucleon interaction described by a two-body
Urbana UV14 potential, combined with a phenomenological three-neutron TNI
interaction. Ground state of neutron matter calculated using variational
method (Friedman & Pandharipande 1981). Non-causal at n>1fm-3.
WFF(AV14+UVII): Nucleon matter in beta equilibrium with electrons and muons.
Interaction described by a two-body Argonne AV14 potential, combined with
phenomenological three-nucleon UVII interaction. Ground state of matter
calculated in a very good approximation using sophisticated variational
method (Wiringa et al., 1988). Non-causal at n>1.1fm-3
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.
WFF(UV14+UVII): Nucleon matter in beta equilibrium with electrons and muons.
Interaction described by a two-body Urbana UV14 potential, combined with
a phenomenological three-nucleon UVII interaction. Ground state of matter
calculated in a very good approximation using sophisticated variational
method (Wiringa et al., 1988). Non-causal at n>1fm-3
Schematic analytic models
Pol2: Polytrope p = κn^γ,
e=mBn+({kappa/(γ-1))n^γ with κ=1mBfm3
and γ=2. Causal at all n.
CLES: Causality-limit EOS. BJ1 model up to n=n*=0.3fm-3, continued by a
schematic EOS p=e-e*+p*, where p*=p(n*), e*=e(n*) are given analytically
(see Eq.3 of Haensel & Proszynski 1982). Maximally stiff while causal
(velocity of sound = c) above n*.
References:
Behte H.A. & Johnson M.B., 1974, Nucl. Phys. A230, 1
Diaz Alonso J., 1985, Phys. Rev. D31, 1315
Friedman J.L. & Pandharipande V.R., 1981, Nucl. Phys. A361, 502
Glendenning N.K., 1985, ApJ 293, 470
Haensel P. et al., 1981, A&A 102, 299
Haensel P. & Proszynski, 1982, ApJ 258, 306
Malone R.C. et al., 1975, ApJ 199, 741
Pandharipande V.R., 1971, Nucl. Phys. A174, 641
Weber F. et al., 1991, Phys. Lett. B265, 1
Wiringa R.B. et al., 1988, Phys. rev. C38, 1010
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(End) Patricia Bauer [CDS] 16-Jun-1994