Relativistic mean-field theory with non-linear σ and ω terms for neutron stars and supernovae

Sumiyoshi, Kohsuke; Kuwabara, Hitoshi; Toki, H.

doi:10.1016/0375-9474(94)00335-k

Cited by 105 publications

(115 citation statements)

References 30 publications

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“…In this work we consider two types of them: models with constant meson-nucleon couplings described by the Lagrangian density of the nonlinear Walecka models (NLWM), and models with density-dependent couplings (hereafter called densitydependent hadronic models (DDHM)). In particular, within the first type, we consider the models GM1 and GM3 [73], TM1 [74], NL3 and NL3-II [75] and NL-SH [76]. For the DDHM models, we consider the models DDME1 and DDME2 [77], TW99 [78], and the models PK1, PK1R and PKDD of the Peking group [79].…”

Section: Nuclear Equation Of State Modelsmentioning

confidence: 99%

Nuclear symmetry energy and ther-mode instability of neutron stars

Vidaña

2012

Phys. Rev. C

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We analyze the role of the symmetry energy slope parameter L on the r-mode instability of neutron stars. Our study is performed using both microscopic and phenomenological approaches of the nuclear equation of state. The microscopic ones include the Brueckner-Hartree-Fock approximation, the well known variational equation of state of Akmal, Pandharipande and Ravenhall, and a parametrization of recent Auxiliary Field Diffusion Monte Carlo calculations. For the phenomenological approaches, we use several Skyrme forces and relativisic mean field models. Our results show that the r-mode instability region is smaller for those models which give larger values of L. The reason is that both bulk (ξ ) and shear (η) viscosities increase with L and, therefore, the damping of the mode is more efficient for the models with larger L. We show also that the dependence of both viscosities on L can be described at each density by simple power-laws of the type ξ = A ξ L B ξ and η = A η L B η . Using the measured spin frequency and the estimated core temperature of the pulsar in the low-mass X-ray binary 4U 1608-52, we conclude that observational data seem to favor values of L larger than ∼ 50 MeV if this object is assumed to be outside the instability region, its radius is in the range 11.5 − 12(11.5 − 13) km, and its mass 1.4M ⊙ (2M ⊙ ). Outside this range it is not possible to draw any conclusion on L from this pulsar.

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Section: Nuclear Equation Of State Modelsmentioning

confidence: 99%

Nuclear symmetry energy and ther-mode instability of neutron stars

Vidaña

2012

Phys. Rev. C

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“…Starting from the RMF models NL3 [42], TM1 [66], and Z271 [46], we build six families of models; each one having the same isoscalar properties, but varying the isovector properties through the mixed nonlinear terms ωρ and σρ (see Sec. III A).…”

Section: Resultsmentioning

confidence: 99%

Vlasov formalism for extended relativistic mean field models: The crust-core transition and the stellar matter equation of state

Pais

Providência

2016

Phys. Rev. C

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The Vlasov formalism is extended to relativistic mean field hadron models with nonlinear terms up to fourth order and applied to the calculation of the crust-core transition density. The effect of the nonlinear ωρ and σρ coupling terms on the crust-core transition density and pressure and on the macroscopic properties of some families of hadronic stars is investigated. For that purpose, six families of relativistic mean field models are considered. Within each family, the members differ in the symmetry energy behavior. For all the models, the dynamical spinodals are calculated, and the crust-core transition density and pressure and the neutron star mass-radius relations are obtained. The effect on the star radius of the inclusion of a pasta calculation in the inner crust is discussed. The set of six models that best satisfy terrestrial and observational constraints predicts a radius of 13.6 ± 0.3 km and a crust thickness of 1.36 ± 0.06 km for a 1.4M star.

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“…In this work, unless otherwise stated, we use a set of constants usually identified as NL1 [28], which is not unique, but it gives a good description of the ground state properties of many stable nuclei. The consequences of using different parameterizations is also investigated and, for this purpose, we use two other sets known as NL3 [29] and TM1 [30]. The values of the constants are displayed in table 1 and the most important bulk properties obtained with these three parameterizations are displayed in table 1a.…”

Section: Non Linear Walecka Modelmentioning

confidence: 99%