Properties of Neutron Stars in the Relativistic Mean-Field Theory

Cheng, K. S.; Dai, Z. G.; Yao, C. C.

doi:10.1086/177325

Cited by 8 publications

(5 citation statements)

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“…For Ðeld-free cases, the BB model results in a B p cr, B p cr, 10B p cr, larger proton fraction of neutron star matter than the ZM model does. Consequently, in the interior region, based on the BB model, the direct Urca process may occur, but only the modiÐed Urca process can occur according to the ZM model (Cheng et al 1996 ;Boguta 1981). Our results indicate that enhances drastically when both for the BB and the ZM models.…”

Section: Resultsmentioning

confidence: 71%

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The Effects of Interior Magnetic Fields on the Properties of Neutron Stars in the Relativistic Mean‐Field Theory

Yuan

Zhang

1999

ApJ

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We investigate the gross properties of the dense neutron star matter and the structure of the stars under the inÑuence of strong magnetic Ðelds, based on two nonlinear p [ u models of nuclear matter, i.e., the BB and the ZM models, within the relativistic mean-Ðeld approximation. Contrary to the results obtained in the linear p [ u model and the BB model, we Ðnd that the inÑuence of the magnetic Ðeld on the e †ective nucleon mass m* is not signiÐcant in the ZM model ; therefore, we predict that the neutrons in the interior of a neutron star might be superÑuid according to the ZM model, if there is a strong magnetic Ðeld in the interior of the star. Moreover, the equations of state (EOSs) will become softer and softer with the increase of the strength of the magnetic Ðeld B. We show the e †ects of the interior magnetic Ðelds on the gross properties of neutron stars, such as the critical masses, their corresponding radii, the moment of inertia, the crust masses, the crust moment of inertia, and the gravitational redshift in both nonlinear p [ u models.

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Section: Resultsmentioning

confidence: 71%

“…The ZM model also yields reasonable values of incompressibility. The application of the ZM model to neutron stars and supernova has been investigated (Prakash, Cooke, & Lattimer 1995 ;Cheng, Dai, & Yao 1996 ;Dai & Cheng 1997. Note that the BB and ZM models are usually referred to as the nonlinear p [ u models.…”

Section: Introductionmentioning

confidence: 99%

The Effects of Interior Magnetic Fields on the Properties of Neutron Stars in the Relativistic Mean‐Field Theory

Yuan

Zhang

1999

ApJ

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“…The masses of the baryon octet are approximately taken to be their mean values of the same family (Glendenning 1985), which will not obviously alter the quantitative results. The meson masses and the constants g vn , g sn and g ρn (coupling constants for interactions between mesons and nucleons, Cheng et al 1996) are given in Table 2. Define…”

Section: The Zm Model With Hyperons Includedmentioning

confidence: 99%

“…Along this direction, many authors (Kapusta & Olive 1990;Ellis et al 1991;Sumiyoshi et al 1992;Sumiyoshi & Toki 1994;Sumiyoshi et al 1995;Cheng et al 1996;Schaffner & Mishustin 1996) studied the EOSs for dense matter and the properties of neutron stars. Zimanyi & Moszkowski (1990, hereafter ZM) proposed another nonlinear model, in which the nonlinearity is contained in connection between the effective nucleon mass and the scalar field.…”

Section: Introduced Cubic Andmentioning

confidence: 99%

“…The ZM model also gives reasonable incompressibility values. This model has been employed to study the properties of neutron stars (Cheng et al 1996) and of supernova cores (Dai & Cheng 1998). These theories can be considered as phenomenological, since the coupling constants and meson masses of the effective mesonnucleon Lagrangian are taken as free parameters which are adjusted to fit the properties of nuclear matter and finite nuclei.…”

Section: Introduced Cubic Andmentioning

confidence: 99%

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Properties of neutron stars with hyperons in the relativistic mean field theory

Dai

Liu

2001

A&A

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Abstract.We study the equation of state (EOS) of the dense matter in the core of neutron stars with hyperons included and the star structure based on the Zimanyi & Moszkowski (ZM) model in the relativistic mean-field theory with a set of recent satisfactory parameters. The relation between hyperon abundances and baryon number densities is calculated and the distribution of baryons in the core of a typical neutron star of 1.4 M is presented. Our results satisfy the requirements from observations of the mass of binary radio pulsars, and the ratio, Ic/Itot, of the crustal momentum of inertia to the total one. The actual surface thermal radiation detected seems to indicate that baryons in the core of neutron stars should pair to form a superfluid phase, if hyperons appear in the core of neutron stars.

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Neutron Stars and Black Holes in X-ray Binaries

Paradijs¹

1998

The Many Faces of Neutron Stars

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Galactic accretion driven stellar X-ray sources can be divided into groups in different ways. An important division, which covers almost all known X-ray binaries, can be made according to the mass of the donor star: high-mass X-ray binaries and low-mass X-ray binaries. Another distinction (partially overlapping with the previous one) can be made on the basis of the nature of the accreting object: a strongly magnetized neutron star, a neutron star with a weak magnetic field, or a black hole. In this review I describe the properties of these different types of X-ray binaries, and discuss the mass determinations which are the basis for distinguishing accreting neutron stars from black holes.

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Properties of Neutron Stars in the Relativistic Mean-Field Theory

Cited by 8 publications

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The Effects of Interior Magnetic Fields on the Properties of Neutron Stars in the Relativistic Mean‐Field Theory

The Effects of Interior Magnetic Fields on the Properties of Neutron Stars in the Relativistic Mean‐Field Theory

Properties of neutron stars with hyperons in the relativistic mean field theory

Neutron Stars and Black Holes in X-ray Binaries

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