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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      (SIMBAD/NED Reference)
ADC_Keywords: Pulsars;  Models, evolutionary

Keywords: relativity - stars: neutron; rotation; pulsar - equations of state


File Summary:

       FileName      Lrecl  Records   Explanations

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


Byte-by-byte Description of file: tables

   Bytes Format  Units            Label    Explanations

   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

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
(End)                                          Patricia Bauer [CDS] 16-Jun-1994