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J/A+A/291/155       Rotating neutron stars models .I.           (Salgado+, 1994)
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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      (SIMBAD/NED Reference)
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ADC_Keywords:Pulsars;  Models, evolutionary 
Keywords: relativity - stars: neutron; rotating; pulsar; evolution -
          equations of state

Abstract:
    A new and precise numerical code for computing equilibrium configurations 
    of relativistic rotating bodies has been used to construct 'realistic' 
    rotating neutron star models. Fourteen equations of state including recent
    dense matter models have been employed. Detailed comparisons of our results
    with previous studies have been performed. Maximum mass and maximum angular
    velocity models are presented and confronted with the constraints imposed 
    by observed pulsars. A special emphasis is put on the construction of 
    rotating configurations along sequences of constant baryon number, which 
    may represent evolutionary sequences of rotating neutron stars. Two kinds 
    of such sequences have been identified: the normal sequences which connect
    to the non-rotating limit and whose stars have a baryon number lower than 
    the maximum one supported by static configurations and the supremassive 
    sequences which do not connect to the non-rotaing limit, its stars having 
    a bayron number above the maximum one supported by static configurations. 
    A remarkable feature of supramassive stars is the phenomenon of spin-up by
    loss of angular momentum which takes place just before the star enters the
    regime of instability with respect to axisymmetric perturbations. In 
    constrast, such a behavior has not been observed for normal stars. 

File Summary:
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 FileName    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 {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).
 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(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.
Schematic analytic model
  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.
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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