Hadronic and hybrid stars subject to density-dependent magnetic fields

Casali, Rudiney Hoffmann; Castro, Luis B.; Menezes, D. P.

doi:10.1103/physrevc.89.015805

Cited by 72 publications

(85 citation statements)

References 74 publications

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“…[32] and widely adopted in subsequent works [21][22][23][33][34][35][36][37][38][39][40][41]. This ansatz, however, violates Maxwell equations.…”

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confidence: 99%

“…While some of the first works advocated that the pressure, having in mind the thermodynamical pressure obtained from the thermodynamical potential that relates pressure to density, should be isotropic [20][21][22][23], based on an interpretation given in Ref. [24], other works were based on the fact that the energy-momentum tensor gives different contributions for the parallel and perpendicular pressure [25][26][27][28] (see Ref.…”

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confidence: 99%

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Anisotropy in the equation of state of magnetized quark matter

2015

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The anisotropies in the pressure obtained from the energy-momentum tensor are studied for magnetized quark matter within the su(3) Nambu-Jona-Lasinio model for both β-equilibrium matter and quark matter with equal quark chemical potentials. The effect of the magnetic field on the particle polarization, magnetization, and quark matter constituents is discussed. It is shown that the onset of the s quark after chiral symmetry restoration of the u and d quarks gives rise to a special effect on the magnetization in the corresponding density range: A quite small magnetization just before the s onset is followed by a strong increase of this quantity as soon as the s quark sets in. It is also demonstrated that for B < 10 18 G within the two scenarios discussed, always considering a constant magnetic field, the two components of pressure are practically coincident. The structure of the QCD phase diagram is of utmost importance in understanding many physical aspects of nature, ranging from the early universe to possible nuclear liquid-gas and hadronic quark matter phase transitions to the physics of compact objects [1]. Early analyzes performed within the Nambu-Jona-Lasinio model (NJL) framework indicate that when strongly interacting matter is subject to intense magnetic fields the QCD phase diagram boundaries are modified [2]. Some of the most important changes concern the size and location of the first-order chiral transition region since the results show that a strong magnetic field favors this type of transition. At the same time, at low temperatures, the value of the coexistence chemical potential decreases as B increases in accordance with the inverse magnetic catalysis (ICM) phenomenon [3].The low-T and high-μ region where a first-order-type transition is expected to occur is currently unavailable to lattice QCD evaluations (LQCD). However, the region high-T and low-μ has already been exploited using LQCD simulations which indicate, in accordance with most model predictions, that the crossover observed at B = 0 persists when B = 0 [4][5][6][7]. On the other hand, a major disagreement between recent LQCD results [6,7] and model calculations regards the dependence of crossover pseudocritical temperature, T pc , on the strength B of the magnetic field. Specifically, the lattice results of Refs. [6,7], performed with 2 + 1 quark flavors and physical pion mass values, predict an inverse catalysis, with T pc decreasing with B, while effective models predict an increase of T pc with B. This problem has been recently addressed by different groups [8,9], who basically agree that the different results stem from the fact that most effective models miss back reaction effects (the indirect interaction of gluons and B) as well as the QCD asymptotic freedom phenomenon. At the same time, other important aspects of the effects of strong magnetic fields on the QCD phase diagram have already been studied, including the behavior of the coexistence chemical potential and the location of the critical end point (CEP) [10], the dependenc...

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“…[32] and widely adopted in subsequent works [21][22][23][33][34][35][36][37][38][39][40][41]. This ansatz, however, violates Maxwell equations.…”

mentioning

confidence: 99%

mentioning

confidence: 99%

Anisotropy in the equation of state of magnetized quark matter

2015

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“…Over the years, it has been shown that the presence of strong magnetic fields significantly affects the energy levels of charged particles due to Landau quantization. These effects have been taken into account in the EoS of models in order to describe hyperon stars (Chakrabarty et al 1997;Broderick et al 2000Broderick et al , 2002Lopes & Menezes 2012;Sinha et al 2013;Casali et al 2014;Gomes et al 2014;Gao et al 2015), quark stars (Perez Martinez et al 2008;Felipe et al 2011;Orsaria et al 2011;Paulucci et al 2011;Denke & Pinto 2013;Dexheimer et al 2014;Isayev 2015), hybrid stars (Rabhi et al 2009;Dexheimer et al 2012Dexheimer et al , 2013, and stars with meson condensates Schramm et al (2015). The effects of the anomalous magnetic moment (AMM) were also investigated through the corresponding coupling of the baryons to the electromagnetic field tensor (see Canuto & Chiu 1968a;Broderick et al 2000Broderick et al , 2002Strickland et al 2012).…”

Section: Introductionmentioning

confidence: 99%

Many-body Forces in Magnetic Neutron Stars

Gomes

Franzon

Dexheimer

et al. 2017

ApJ

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In this work, we study in detail the effects of many-body forces on the equation of state and the structure of magnetic neutron stars. The stellar matter is described within a relativistic mean field formalism that takes into account many-body forces by means of a nonlinear meson field dependence on the nuclear interaction coupling constants. We assume that matter is at zero temperature, charge neutral, in beta equilibrium, and populated by the baryon octet, electrons, and muons. In order to study the effects of different degrees of stiffness in the equation of state, we explore the parameter space of the model, which reproduces nuclear matter properties at saturation, as well as massive neutron stars. Magnetic field effects are introduced both in the equation of state and in the macroscopic structure of stars by the self-consistent solution of the Einstein-Maxwell equations. In addition, the effects of poloidal magnetic fields on the global properties of stars, as well as density and magnetic field profiles, are investigated. We find that not only different macroscopic magnetic field distributions but also different parameterizations of the model for a fixed magnetic field distribution impact the gravitational mass, deformation, and internal density profiles of stars. Finally, we show that strong magnetic fields significantly affect the particle populations of stars.

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“…The fact that strong magnetic fields populate the vast majority of the astrophysical compact objects and that they can significantly affect several properties of the star have served as motivation for many works focused on the study of the EoS of magnetized neutron stars, without considering , or considering the magnetic-field interaction with the particle anomalous-magnetic-moment [88,[99][100][101][102][103][104][105][106][107][108][109][110][111][112][113]. An important characteristic is that the EoS in a uniform magnetic field becomes anisotropic, with different pressures along the field and transverse to it [73,94,98].…”

Section: Introductionmentioning

confidence: 99%

Anomalous Electromagnetic Transport in Compact Stars

Ferrer

Incera

2018

Universe

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Abstract:We study the anomalous electromagnetic transport properties of a quark-matter phase that can be realized in the presence of a magnetic field in the low-temperature/moderate-high-density region of the Quantum Chromodynamics (QCD) phase map. In this so-called Magnetic Dual Chiral Density Wave phase, an inhomogeneous condensate is dynamically induced producing a nontrivial topology, a consequence of the asymmetry of the lowest Landau level modes of the quasiparticles in this phase. The nontrivial topology manifests in the electromagnetic effective action via a chiral anomaly term θF µνF µν , with an axion field θ given by the phase of the Dual Chiral Density Wave condensate. The coupling of the axion with the electromagnetic field leads to several macroscopic effects that include, among others, an anomalous, nondissipative Hall current, an anomalous electric charge, magnetoelectricity, and the formation of a hybridized propagating mode known as an axion polariton. The possible existence of this phase in the inner core of neutron stars opens a window to search for signals of its anomalous transport properties.

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Hadronic and hybrid stars subject to density-dependent magnetic fields

Cited by 72 publications

References 74 publications

Anisotropy in the equation of state of magnetized quark matter

Anisotropy in the equation of state of magnetized quark matter

Many-body Forces in Magnetic Neutron Stars

Anomalous Electromagnetic Transport in Compact Stars

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