Maximum mass of a hybrid star having a mixed-phase region based on constraints set by the pulsar PSR J1614-2230

Mallick, Ritam

doi:10.1103/physrevc.87.025804

Cited by 28 publications

(26 citation statements)

References 45 publications

(52 reference statements)

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“…Masses of the order of ≤ 1.8M ⊙ were obtained in non-relativistic phenomenological models [13,14], while microscopic models based on hyperon-nucleon potentials, which include the repulsive three-body forces, predict low maximal masses for hypernuclear stars [15,16]. The avenues for reconciliation of the large pulsar mass and the hyperonization (and more generally strangeness) of dense matter have been explored recently in Refs [17][18][19][20][21][22][23][24][25][26][27][28].…”

Section: Introductionmentioning

confidence: 99%

Hypernuclear matter in strong magnetic field

2013

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Compact stars with strong magnetic fields (magnetars) have been observationally determined to have surface magnetic fields of order of 10 14 − 10 15 G, the implied internal field strength being several orders larger. We study the equation of state and composition of dense hypernuclear matter in strong magnetic fields in a range expected in the interiors of magnetars. Within the non-linear Boguta-Bodmer-Walecka model we find that the magnetic field has sizable influence on the properties of matter for central magnetic field B ≥ 10 17 G, in particular the matter properties become anisotropic. Moreover, for the central fields B ≥ 10 18 G, the magnetized hypernuclear matter shows instability, which is signalled by the negative sign of the derivative of the pressure parallel to the field with respect to the density, and leads to vanishing parallel pressure at the critical value B cr ≃ 10 19 G. This limits the range of admissible homogeneously distributed fields in magnetars to fields below the critical value B cr .

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Section: Introductionmentioning

confidence: 99%

Hypernuclear matter in strong magnetic field

2013

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“…In 2010, Demorest et al first observed the massive neutron star PSR J1614-2230 [1], which was soon theoretically studied by many researchers with various methods [2][3][4][5][6][7][8][9][10][11][12].…”

Section: Introductionmentioning

confidence: 99%

Examination of the influence of thef0(975)andϕ(1020) mesons on the surface gravitational redshift of the neutron star PSR J0348+0432

Zhao

2015

Phys. Rev. C

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Examination of the influence of the f 0 (975) and φ(1020) mesons on the surface gravitional redshift of the neutron star PSR J0348+0432 The effect of the mesons f0(975) and φ(1020) on the surface gravitional redshift of the neutron star PSR J0348+0432 is examined in the framework of the relativistic mean field theory by choosing the suitable hyperon coupling constants. We find that compared with that without considering the mesons f0(975) and φ(1020), the value range of the radius R of the neutron star PSR J0348+0432 would be changed from a narrow range 12.964 km ∼ 12.364 km to a wider range 12.941 km ∼ 11.907 km corresponding to the observation mass M=1.97 M⊙∼2.05 M⊙. We also find that the value range of the surface gravitational redshift z of the neutron star PSR J0348+0432 changes from 0.3469 ∼ 0.3997 to 0.3480 ∼ 0.4263 corresponding to the observation mass M=1.97 M⊙∼2.05 M⊙ as the mesons f0(975) and φ(1020) being considered. These mean the radius R and the surface gravitational redshift z all will be constrained in a wider scope as the mesons f0(975) and φ(1020) being considered. We also can see that the difference of the radius and the surface gravitational redshift is not so large whether the mesons f0(975) and φ(1020) being considered or not. This indicates that the mesons f0(975) and φ(1020) do not play a major role in the massive neutron star PSR J0348+0432.

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“…The total energy density and pressure of the strange quark matter is given by (Mallick, 2013; Mohanta…”

Section: Magnetic Field In Quark Phasementioning

confidence: 99%

Maximum mass and radial modes of hybrid star in presence of strong magnetic field

Panda¹

2015

Proceedings of the Indian National Science Academy

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It is believed that neutron stars (NS) consist of hadronic and exotic states like strange quark or color superconducting matter. Stars having a quark core surrounded by a mixed phase followed by hadronic matter, may be considered as hybrid stars (HS). The mixed phase is well proportionate of both the hadron and quark phases. A huge magnetic field is predicted in core as well as on surface of the neutron star.Here we study the effect of this strong magnetic field on the equation of states(EOS) of HS matter. We further study the hadron-quark phase transition in the interiors of NS giving rise to HS in presence of strong magnetic field. We finally study the effect of strong magnetic field on maximum mass and eigenfrequencies of radial pulsation of such type of HS. For the EOS of hadronic matter, we have considered RMF(Relativistic Mean Field) theory and we incorporated the effect of strong magnetic fields leading to Landau quantization of the charged particles. For the EOS of quark phase we use the simple MIT bag model. We have assumed Gaussian parametrization to incorporate the density dependence of both bag pressure and magnetic field. We have constructed the intermediate mixed phase by using Glendenning conjecture. We found that magnetic field softens the EOS of both the phases, as a result the maximum mass is reduced for HS and period of oscillation is increased significantly for primary mode.

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Maximum mass of a hybrid star having a mixed-phase region based on constraints set by the pulsar PSR J1614-2230

Cited by 28 publications

References 45 publications

Hypernuclear matter in strong magnetic field

Hypernuclear matter in strong magnetic field

Examination of the influence of thef0(975)andϕ(1020) mesons on the surface gravitational redshift of the neutron star PSR J0348+0432

Maximum mass and radial modes of hybrid star in presence of strong magnetic field

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