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J/A+AS/108/455 Rotating neutron stars models. II. (Salgado+, 1994)
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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 (SIMBAD/NED Reference)
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ADC_Keywords: Pulsars; Models, evolutionary
Keywords: relativity - stars: neutron; rotation; pulsar - equations of state
Abstract:
A new and highly precise numerical approach for computing stationary
rotating stellar configurations in general relativity has been employed to
construct rotating neutron star models. Fourteen equations of state (EOS)
of cold dense matter have been used to produce a "catalog" of thousands
neutron star models, parametrized by the EOS, the central energy density
and the angular velocity. The results are presented in a series of tables
for each EOS. A particular emphasis is put on the properties of maximal
mass models. These latter are useful to constrain the EOS, taking into
account the observed pulsars.
File Summary:
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FileName 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 Sun M Gravitational mass
54- 58 F5.3 Sun 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
{sigma}, {pi}, {rho}, {omega} mesons. Ground state calculated by using
renormalized Hartree approximation (Diaz Alonso 1985).
HKP: Pure neutron matter, n-n interaction mediated via exchange of {sigma},
{omega}, {pi}, {rho} 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 {sigma}, {omega}, {pi}, {rho}, 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 {sigma}, {omega}, {pi}, {rho}, {eta}, {delta} 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 UV_14_ 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(AV_14_+UVII): Nucleon matter in beta equilibrium with electrons and muons.
Interaction described by a two-body Argonne AV_14_ 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(UV_14_+TNI): Nucleon matter in beta equilibrium with electrons and muons.
Interaction described by a two-body Urbana UV_14_ 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(UV_14_+UVII): Nucleon matter in beta equilibrium with electrons and muons.
Interaction described by a two-body Urbana UV_14_ 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 = {kappa}n^{gamma},
e=m_B_n+({kappa/({gamma}-1))n^{gamma} with {kappa}=1m_B_fm^3^
and {gamma}=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