Equilibrium models of relativistic stars with a toroidal magnetic field

Frieben, J.; Rezzolla, Luciano

doi:10.1111/j.1365-2966.2012.22027.x

Cited by 161 publications

(192 citation statements)

References 60 publications

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“…[57] using pure toroidal magnetic field equilibrium models of relativistic stars for both nonrotating and rotating hadronic stars, fields as large as 10 18 G were obtained on the equatorial plane deep inside the star. In this calculation, however, the magnetic field effects on the EOS have been neglected.…”

Section: Final Remarksmentioning

confidence: 99%

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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Section: Final Remarksmentioning

confidence: 99%

Anisotropy in the equation of state of magnetized quark matter

2015

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“…Stationary and axisymmetric solutions of rotating relativistic stars with strong poloidal fields have been successfully calculated in [3], and with toroidal fields in [4,5]. In these computations, the spacetime is assumed to be orthogonally transitive (circular -invariant under a simultaneous inversion of t → −t, and φ → −φ), because the configuration of magnetic fields is restricted to either purely poloidal or toroidal fields and the velocity field is to circular [6][7][8][9] A relativistic formulation for more general magnetized relativistic stars with mixed poloidal and toroidal fields has been derived by Bekenstein and Oron [10].…”

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Equilibrium solutions of relativistic rotating stars with mixed poloidal and toroidal magnetic fields

et al. 2014

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Stationary and axisymmetric solutions of relativistic rotating stars with strong mixed poloidal and toroidal magnetic fields are obtained numerically. Because of the mixed components of the magnetic field, the underlying stationary and axisymmetric spacetimes are no longer circular. These configurations are computed from the full set of the Einstein-Maxwell equations, Maxwell's equations and from first integrals and integrability conditions of the magnetohydrodynamic equilibrium equations. After a brief introduction of the formulation of the problem, we present the first results for highly deformed magnetized rotating compact stars.

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“…Accordingly, the stellar deformation could be reduced by 50% when a mixture of poloidal and toroidal fields of similar strength are presented in the star. The distortion of the star scale with its quadrupole moment as ε ∼ Q (Frieben & Rezzolla 2012). Therefore, we expect that the gravitational wave amplitude, which scale with Q as h 0 ∼ Q, should be only roughly reduced by a factor of 2 compared to those obtained in this work.…”

Section: Discussionmentioning

confidence: 69%

AR Scorpii and possible gravitational wave radiation from pulsar white dwarfs

Franzon¹,

Schramm²

2017

Monthly Notices of the Royal Astronomical Society

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In view of the new recent observation and measurement of the rotating and highlymagnetized white dwarf AR Scorpii Marsh et al. (2016), we determine bounds of its moment of inertia, magnetic fields and radius. Moreover, we investigate the possibility of fast rotating and/or magnetized white dwarfs to be source of detectable gravitational wave (GW) emission. Numerical stellar models at different baryon masses are constructed. For each star configuration, we compute self-consistent relativistic solutions for white dwarfs endowed with poloidal magnetic fields by solving the Einstein-Maxwell field equations in a self-consistent way. The magnetic field supplies an anisotropic pressure, leading to the braking of the spherical symmetry of the star. In this case, we compute the quadrupole moment of the mass distribution. Next, we perform an estimate of the GW of such objects. Finally, we show that the new recent observation and measurement pulsar white dwarf AR Scorpii, as well as other stellar models, might generate gravitational wave radiation that lies in the bandwidth of the discussed next generation of space-based GW detectors DECI-hertz interferometer Gravitational wave Observatory (DECIGO) and Big Bang Observer (BBO).

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Equilibrium models of relativistic stars with a toroidal magnetic field

Cited by 161 publications

References 60 publications

Anisotropy in the equation of state of magnetized quark matter

Anisotropy in the equation of state of magnetized quark matter

Equilibrium solutions of relativistic rotating stars with mixed poloidal and toroidal magnetic fields

AR Scorpii and possible gravitational wave radiation from pulsar white dwarfs

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