Quantum Magnetic Collapse

Chaichian, M.; Masood, Samina; Montonen, C.; Martı́nez, A. Pérez; Rojas, Hugo Perez

doi:10.1103/physrevlett.84.5261

Cited by 150 publications

(173 citation statements)

References 16 publications

(18 reference statements)

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“…The classical Maxwellian contribution B 2 produces a decelerated fluid expansion in the direction of the magnetic field (z), as the latter produces a negative pressure or tension in its direction, and an accelerated expansion in the directions perpendicular to it due to a positive pressure. However, we obtain the opposite effect from the statistical contribution of B in the equation of state for the magnetised electron-positron gas mixture: the pressure in the direction parallel to the field increases and that in the perpendicular direction decreases [39,40,46,51]. Although the dominant effect in the dynamics comes from the contribution B 2 , we can observe that including the magnetised electron-positron gas leads to a slight acceleration of the cosmic rate of expansion.…”

Section: Thermodynamicsmentioning

confidence: 80%

“…However, leptons and baryons could interact with the field through their charges (if they are charged) and via their anomalous magnetic moment (if they are neutral). In any case the interactions with the field (via charges or anomalous magnetic moment) lead to a momentum-energy tensor with anisotropic stresses [39,41]. We assume hereafter that the only particle species interacting with the magnetic field are electrons and positrons (charged leptons), protons (charged baryons) and neutrons (neutral baryons).…”

Section: Physically Motivated Field Sourcesmentioning

confidence: 99%

“…In general the equation of state for these species in presence of a timedependent magnetic field can be written as follows [39,41,51]:…”

Section: Physically Motivated Field Sourcesmentioning

confidence: 99%

“…Instead of considering idealised fluids whose interaction with the magnetic field is unspecified (as in [32,33,34,35,36]), or a collision-less kinetic theory approach (suited to free streaming collision-less conditions as in [37]), we consider fluid sources that satisfy physically motivated equations of state that are well suited for an early Universe cosmic fluid interacting with a magnetic field within a hydrodynamical regime, namely: a mixture of ideal gasses of magnetised fermions [39,40,41] whose equation of state reflects the full anisotropic effects of the magnetic field. Evidently, this field introduces anisotropic momentum fluxes that modify the energy-momentum tensor and thus affect the evolution of the state variables.…”

Section: Introductionmentioning

confidence: 99%

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A non-perturbative study of the evolution of cosmic magnetised sources

et al. 2015

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We undertake a hydrodynamical study of a mixture of tightly coupled primordial radiation, neutrinos, baryons, electrons and positrons, together with a gas of already decoupled dark matter WIMPS and an already existing "frozen" magnetic field in the infinite conductivity regime. Considering this cosmic fluid as the source of a homogeneous but anisotropic Bianchi I model, we describe its interaction with the magnetic field by means of suitable equations of state that are appropriate for the particle species of the mixture between the end of the leptonic era and the beginning of the radiation-dominated epoch. Fulfilment of observational bounds on the magnetic field intensity yields a "near FLRW" (but strictly non-perturbative) evolution of the geometric, kinematic and thermodynamical variables. This evolution is roughly comparable to the weak field approximation in linear perturbations on a spatially flat FLRW background of sources in which the frozen magnetic fields are coherent over very large supra-horizon scales. Our approach and results may provide interesting guidelines in potential situations in which non-perturbative methods are required to study the interaction between magnetic fields and the cosmic fluid.

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Section: Thermodynamicsmentioning

confidence: 80%

Section: Physically Motivated Field Sourcesmentioning

confidence: 99%

“…In general the equation of state for these species in presence of a timedependent magnetic field can be written as follows [39,41,51]:…”

Section: Physically Motivated Field Sourcesmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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A non-perturbative study of the evolution of cosmic magnetised sources

et al. 2015

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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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Gravity induced evolution of a magnetized fermion gas with finite temperature

et al. 2014

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We examine the dynamics near the collapse of a self-gravitating magnetized fermion gas at finite temperature, taken as the source of a Bianchi-I spacetime described by the Kasner metric. The set of Einstein-Maxwell field equations reduces to a complete and self-consistent system of non-linear autonomous ordinary differential equations. By considering a representative set of initial conditions, the numerical solutions of this system show the gas collapsing into both, isotropic ("point-like") and anisotropic ("cigar-like") singularities. We also examined the behavior during the collapse stage of all relevant state and kinematic variables: the temperature, the expansion scalar, the magnetic field, the magnetization and energy density. We notice a significant qualitative difference in the behavior of the gas for a range of temperatures: T/m ∼ 10 −6 -10 −3 .

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Quantum Magnetic Collapse

Cited by 150 publications

References 16 publications

A non-perturbative study of the evolution of cosmic magnetised sources

A non-perturbative study of the evolution of cosmic magnetised sources

Magnetism in Dense Quark Matter

Gravity induced evolution of a magnetized fermion gas with finite temperature

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