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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 (SIMBAD/NED Reference)
ADC_Keywords: Pulsars; Models, evolutionary Keywords: relativity - stars: neutron; rotating; pulsar; evolution - equations of state File Summary:
FileName Lrecl Records Explanations
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
Byte-by-byte Description of file: table1
Bytes Format Units Label Explanations
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
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. 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
(End) Patricia Bauer [CDS] 16-Jun-1994
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