Surface structure of neutron stars with high magnetic fields

Fushiki, Ikko; Gudmundsson, E. H.; Pethick, C. J.

doi:10.1086/167653

Cited by 86 publications

(117 citation statements)

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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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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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“…In the past few years, several authors have investigated the modifications of the 3a reaction that occurs with increasing density. Fushiki and Lamb (1987) showed how to take account of screening in these reactions by performing an 5-matrix calculation for the 3a process. Their general calculation is valid for both the thermonuclear and pycnonuclear regimes.…”

Section: He-"burning" At T =mentioning

confidence: 99%

“…Fushiki et al (1989) have computed the equation of state in the non-relativistic limit, near the surface of a neutron star. In contrast with earlier calculations, they find that the density of matter does not approach zero gradually as the pressure P falls to zero; instead they find a finite and large surface (P = 0) density, p ~ several xlO 3 g c m -3 , for magnetic field strengths ~ 10 12 G. More recently, Lai and Shapiro (1991) have extended these calculations to include relativistic electrons.…”

Section: Matter In Strong Magnetic Fieldsmentioning

confidence: 99%

Equations of State in Stellar Structure and Evolution

Horn

1994

International Astronomical Union Colloquium

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In this paper I summarize some of the recent advances in studies of dense matter. Research on phase separation in the binary ionic mixtures (BIMs) that constitute the matter in white dwarfs has been motivated by the need to obtain accurate estimates for the ages of the faintest white dwarfs and thus of the disk of our Galaxy. Substantial age increases appear possible, but it is not yet clear whether such large increases occur in real white dwarfs. A second advance is the prediction, based on state-of-the-art physical calculations, that ionization of H at low temperatures and increasing densities may occur via a first-order "plasma phase transition" (PPT). Astrophysical consequences of this result are still being explored in an effort to test this prediction. Related to these equation-of-state calculations are calculations of the enhancement of nuclear reaction rates at high densities. New thermonuclear rates have been computed for C+C reactions in BIMs, although there is currently some controversy about results at the highest densities. New pycnonuclear reaction rates have also been calculated for BIMs, and it has been suggested that He-burning at T = 0 may occur through a first-order phase transition. Finally, calculations of the equation of state of matter in strong magnetic fields and of radiative opacities at high densities have undergone very recent and substantial improvements, which are just beginning to be utilized in astrophysical calculations.Dans cette revue, je resumme les travaux les plus recents dans l'etude

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“…According to virial theorem arguments, which give an upper estimate for the magnetic inside neutron stars, they can possess central magnetic fields as large as 10 18−20 G, see e.g. [7,8,9,10].…”

Section: Introductionmentioning

confidence: 99%

Effects of strong magnetic fields on hybrid stars

Franzon¹,

Dexheimer²,

Schramm³

2016

Proceedings of the Modern Physics of Compact Stars 2015 — PoS(MPCS2015)

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In this work we study the effects of strong magnetic fields on hybrid stars by using a full general-relativity approach, solving the coupled Maxwell-Einstein equation in a selfconsistent way. The magnetic field is assumed to be axi-symmetric and poloidal. We take into consideration the anisotropy of the energy-momentum tensor due to the magnetic field, magnetic field effects on equation of state, the interaction between matter and the magnetic field (magnetization), and the anomalous magnetic moment of the hadrons. The equation of state used is an extended hadronic and quark SU(3) non-linear realization of the sigma model that describes magnetized hybrid stars containing nucleons, hyperons and quarks. According to our results, the effects of the magnetization and the magnetic field on the EoS do not play an important role on global properties of these stars. On the other hand, the magnetic field causes the central density in these objects to be reduced, inducing major changes in the populated degrees of freedom and, potentially, converting a hybrid star into a hadronic star.

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Surface structure of neutron stars with high magnetic fields

Cited by 86 publications

References 0 publications

Magnetism in Dense Quark Matter

Magnetism in Dense Quark Matter

Equations of State in Stellar Structure and Evolution

Effects of strong magnetic fields on hybrid stars

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