Quark–hadron phase transition in a neutron star under strong magnetic fields

Rabhi, Aziz; Pais, Helena; Panda, P. K.; Providência, Constança

doi:10.1088/0954-3899/36/11/115204

Cited by 101 publications

(148 citation statements)

References 45 publications

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“…Many theoretical models for the NS EoS have been developed both with [10,11,12,13] and without [3] strong interior MFs. Typically these start from from an ab initio or effective nucleon-nucleon interaction in order to explain the observational mass-radius (M-R) relation data [3].…”

Section: Equations Of State For Nssmentioning

confidence: 99%

Possible ambiguities in the equation of state for neutron stars

Cheoun

Miyatsu²,

Ryu

et al. 2014

AIP Conference Proceedings

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Abstract.We addressed possible ambiguities on the properties of neutron stars (NSs) estimated in theoretical sides. First, roles of hyperons inside the NS are discussed through various relativistic mean field (RMF) theories. In particular, the extension of SU(6) spin-flavor symmetry to SU(3) flavor symmetry is shown to give rise to the increase of hyperon threshold density, similarly to the Fock term effects in RMF theories. As a result, about 2.0 solar mass is obtained with the hyperons. Second, the effect by the modified f(R) gravity, which leaves a room for the dark energy in the Einstein equation to be taken into account, is discussed for the NS in a strong magnetic field (MF). Our results show that the modified gravity with the Kaluza-Klein electro-magnetism theory expanded in terms of a length scale parameter may reasonably describe the NS in strong MF, so called magnetar. Even the super-soft equation of state is shown to be revived by the modified f(R) gravity.

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Section: Equations Of State For Nssmentioning

confidence: 99%

Possible ambiguities in the equation of state for neutron stars

Cheoun

Miyatsu²,

Ryu

et al. 2014

AIP Conference Proceedings

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“…For hyperon-meson couplings one can assume fixed fractions of nucleon-meson couplings, i.e. g iH = x iH g iN , where x σH = x ρH = 0.600, x ωH = 0.653, x ρH = 0.6 (see [22]). …”

Section: Relativistic Mean Field Theory For Dense Mattermentioning

confidence: 99%

“…Clearly, the magnetic field depends only on the baryon density n. We use a simple parameterization (see, for example, [22,25])…”

Section: Relativistic Mean Field Theory For Dense Mattermentioning

confidence: 99%

“…Realistic EoS with hyperons and quarks in presence of strong magnetic field are considered in [22][23][24][25]. The maximal mass of neutron star can exceed, in these cases, 3M ⊙ for B c ∼ 3.3 × 10 18 G. Therefore it seems that the existence of neutron stars with masses exceeding considerably two solar mass (without strong magnetic field) is impossible in the framework of General Relativity (GR).…”

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confidence: 99%

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Extreme neutron stars from Extended Theories of Gravity

Astashenok

Capozziello

Odintsov

2015

J. Cosmol. Astropart. Phys.

244

128

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We discuss neutron stars with strong magnetic mean fields in the framework of Extended Theories of Gravity. In particular, we take into account models derived from f (R) and f (G) extensions of General Relativity where functions of the Ricci curvature invariant R and the Gauss-Bonnet invariant G are respectively considered. Dense matter in magnetic mean field, generated by magnetic properties of particles, is described by assuming a model with three meson fields and baryons octet. As result, the considerable increasing of maximal mass of neutron stars can be achieved by cubic corrections in f (R) gravity. In principle, massive stars with M > 4M⊙ can be obtained. On the other hand, stable stars with high strangeness fraction (with central densities ρc ∼ 1.5 − 2.0 GeV/fm 3 ) are possible considering quadratic corrections of f (G) gravity. The magnetic field strength in the star center is of order 6 − 8 × 10 18 G. In general, we can say that other branches of massive neutron stars are possible considering the extra pressure contributions coming from gravity extensions. Such a feature can constitute both a probe for alternative theories and a way out to address anomalous self-gravitating compact systems.

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“…Hence, when investigating the field effects in the EoS, it is consistent to take a magnetic field that is locally constant and uniform. This is the reason why such an approximation has been systematically used in all the previous works on magnetized nuclear [1,20,25,28,29,34,35,72,79,87,115,121,124,136,140,143] and quark matter [32,33,74,104,105,120].…”

Section: Equation Of State Of the Mcfl Phasementioning

confidence: 99%

Magnetism in Dense Quark Matter

Ferrer

Incera

2013

Strongly Interacting Matter in Magnetic Fields

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We review the mechanisms via which an external magnetic field can affect the ground state of cold and dense quark matter. In the absence of a magnetic field, at asymptotically high densities, cold quark matter is in the Color-Flavor-Locked (CFL) phase of color superconductivity characterized by three scales: the superconducting gap, the gluon Meissner mass, and the baryonic chemical potential. When an applied magnetic field becomes comparable with each of these scales, new phases and/or condensates may emerge. They include the magnetic CFL (MCFL) phase that becomes relevant for fields of the order of the gap scale; the paramagnetic CFL, important when the field is of the order of the Meissner mass, and a spin-one condensate associated to the magnetic moment of the Cooper pairs, significant at fields of the order of the chemical potential. We discuss the equation of state (EoS) of MCFL matter for a large range of field values and consider possible applications of the magnetic effects on dense quark matter to the astrophysics of compact stars.

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Quark–hadron phase transition in a neutron star under strong magnetic fields

Cited by 101 publications

References 45 publications

Possible ambiguities in the equation of state for neutron stars

Possible ambiguities in the equation of state for neutron stars

Extreme neutron stars from Extended Theories of Gravity

Magnetism in Dense Quark Matter

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