Role of higher order couplings in the presence of kaons in relativistic mean field description of neutron stars

Gupta, Neha; Arumugam, P.

doi:10.1103/physrevc.85.015804

Cited by 25 publications

(25 citation statements)

References 50 publications

(121 reference statements)

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“…In our earlier calculations, we described NS matter with the K − [23] and with K − andK 0 [37] condensation. Here we extend these models further with the inclusion of hyperons.…”

Section: Extended Relativistic Mean-field Models With Hyperons Anmentioning

confidence: 98%

“…The detailed list of nucleon coupling constants (g σ N , g ωN , g ρN , κ 3 , κ 4 , η 1 , η 2 , η ρ , ζ 0 , and v ) in the cases of G1, G2, and NL3 are given in Ref. [23]. The nucleon coupling constants for the IUFSU parameter set is taken from Ref.…”

Section: A Nucleon Coupling Constantsmentioning

confidence: 99%

“…Recently, we have studied the role of antikaons [23,37] in the presence of higher order couplings of the extended RMF models. In the present work we consider * nehaguptaiitr@gmail.com both hyperons and antikoans in the recent versions of the extended RMF models to study NS properties.…”

Section: Introductionmentioning

confidence: 99%

“…Neutron stars were studied within RMF models with the inclusion of hyperons [5][6][7][8][9][10][11][12][13][14][15][16][17][18][19], the antikaon K − [20][21][22][23][24][25][26][27], the antikaons K − andK 0 [28][29][30][31], and both hyperons and antikaons [32][33][34][35][36]. Recently, we have studied the role of antikaons [23,37] in the presence of higher order couplings of the extended RMF models.…”

Section: Introductionmentioning

confidence: 99%

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Impact of hyperons and antikaons in an extended relativistic mean-field description of neutron stars

Gupta¹,

Arumugam²

2013

Phys. Rev. C

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We study the role of higher order couplings in extended relativistic mean-field models, along with the condensation of antikaons and hyperons, on neutron star properties. Though this approach seems to be better and inclusive, the results are sensitive to the hyperon-nucleon and antikaon-nucleon coupling constants, which are poorly known. Despite this aspect, we find that both the hyperons and the antikaons can play a significant role, even in extended relativistic mean-field models which yield softer equations of state. We find that there is a strong interplay between antikaons and hyperons affecting each other's influence on neutron star properties. We discuss the implications of our results in light of the recently observed pulsar with 1.97 ± 0.04 solar masses.

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“…In our earlier calculations, we described NS matter with the K − [23] and with K − andK 0 [37] condensation. Here we extend these models further with the inclusion of hyperons.…”

Section: Extended Relativistic Mean-field Models With Hyperons Anmentioning

confidence: 98%

Section: A Nucleon Coupling Constantsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

See 2 more Smart Citations

Impact of hyperons and antikaons in an extended relativistic mean-field description of neutron stars

Gupta¹,

Arumugam²

2013

Phys. Rev. C

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“…However, as hyperonic stellar matter has already been extensively discussed within the quark-meson coupling (QMC) model [21][22][23], in this work we restrict ourselves to the possible appearance of the kaon condensation in finite temperature systems. It is well known that the onset of the kaon condensation is model dependent and varies according to the strength of the kaon optical potential [20,24,25]. In the present work, we revisit the possibility that a hybrid compact star can be constituted by hadrons and kaon condensed matter at higher densities [20] by using the quark-meson coupling model at finite temperature [21,26] with the inclusion of the ω-ρ interaction [11,12].…”

Section: Introductionmentioning

confidence: 99%

Effects of the symmetry energy on the kaon condensates in the quark-meson coupling model

2014

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In this work we investigate protoneutron star properties within a modified version of the quark-meson coupling (QMC) model that incorporates an ω-ρ interaction plus kaon condensed matter at finite temperature. Fixed entropy and trapped neutrinos are taken into account. Our results are compared with the ones obtained with the GM1 parametrization of the nonlinear Walecka model for similar values of the symmetry energy slope. Contrary to GM1, within the QMC model the formation of low mass black holes during cooling are not probable. It is shown that the evolution of the protoneutron star may include the melting of the kaon condensate driven by the neutrino diffusion, followed by the formation of a second condensate after cooling. The signature of this complex process could be a neutrino signal followed by a gamma ray burst. We have seen that both models can, in general, describe very massive stars.

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Phase transitions in dense matter and the maximum mass of neutron stars

Chamel

Fantina

Pearson

et al. 2013

A&A

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Context. The recent precise measurement of the mass of pulsar PSR J1614−2230, as well as observational indications of even more massive neutron stars, has revived the question of the composition of matter at the high densities prevailing inside neutron-star cores. Aims. We study the impact on the maximum possible neutron-star mass of an "exotic" core consisting of non-nucleonic matter. For this purpose, we study the occurrence of a first-order phase transition in nucleonic matter. Methods. Given the current lack of knowledge of non-nucleonic matter, we consider the stiffest possible equation of state subject only to the constraints of causality and thermodynamic stability. The case of a hadron-quark phase transition is discussed separately. The purely nucleonic matter is described using a set of unified equations of state that have been recently developed to permit a consistent treatment of both homogeneous and inhomogeneous phases. We then compute the mass-radius relation of cold nonaccreting neutron stars with and without exotic cores from the Tolman-Oppenheimer-Volkoff equations. Results. We find that even if there is a significant softening of the equation of state associated with the actual transition to an exotic phase, there can still be a stiffening at higher densities closer to the center of the star that is sufficient to increase the maximum possible mass. However, with quarks the maximum neutron-star mass is always reduced by assuming that the sound speed is limited by c/ √ 3 as suggested by QCD calculations. In particular, by invoking such a phase transition, it becomes possible to support PSR J1614−2230 with a nucleonic equation of state that is soft enough to be compatible with the kaon and pion production in heavy-ion collisions.

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Role of higher order couplings in the presence of kaons in relativistic mean field description of neutron stars

Cited by 25 publications

References 50 publications

Impact of hyperons and antikaons in an extended relativistic mean-field description of neutron stars

Impact of hyperons and antikaons in an extended relativistic mean-field description of neutron stars

Effects of the symmetry energy on the kaon condensates in the quark-meson coupling model

Phase transitions in dense matter and the maximum mass of neutron stars

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