Chiral magnetic effect in protoneutron stars and magnetic field spectral evolution

Sigl, Günter; Leite, Natacha

doi:10.1088/1475-7516/2016/01/025

Cited by 71 publications

(76 citation statements)

References 45 publications

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“…is the equilibrium value of the chiral potential of the background medium in the absence of magnetic helicity [43]. E and B denote from hereon both hyper and ordinary electric and magnetic fields, respectively.…”

Section: Modified Mhd Equationsmentioning

confidence: 99%

“…Refs. [38,43]). In the second case, we take the Γ f (t) = (G Total magnetic energy density spectrum (solid) and background magnetic energy density spectrum (dashed) at different times, computed from (37) and (11), and (39), respectively, with µ mass, which represents the reaction rate given by the weak interaction, dominant, for instance, shortly after the electroweak crossover [38].…”

Section: Weak Anomaly Regimementioning

confidence: 99%

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Chiral magnetohydrodynamic turbulence

2017

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In this work the influence of the chiral anomaly effect on the evolution of magnetohydrodynamic turbulence was studied. We argue that before the electroweak symmetry breaking and for temperatures high enough such that the electron mass can be ignored, the description of a charged plasma in general needs to take into account the interplay between turbulence and the anomaly effects. It was demonstrated that this generalization can have important consequences on the evolution of turbulence, leading to the creation of maximally-helical fields from initially non-helical ones. Therefore, chiral effects can strongly support turbulent inverse cascade, and lead to a slower decrease of the magnetic field with time, and also to a faster growth of the correlation length, when compared to the evolution predicted by the standard magnetohydrodynamics description. Using the weak anomaly approximation, and treating the anomaly contributions to magnetic energy and helicity as a small perturbation, we derive the specific solutions for the inverse cascade regime that demonstrate how chiral effects support the inverse cascade.

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Section: Modified Mhd Equationsmentioning

confidence: 99%

Section: Weak Anomaly Regimementioning

confidence: 99%

Chiral magnetohydrodynamic turbulence

2017

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“…[23] adding anomalous current janom " e 2 µ5B{2π 2 for chiral plasma. 8 We remind that we use units kB " c " " 1.…”

Section: Chiral Anomaly Evolution In the Sn Progenitor Of A Nascent Nsmentioning

confidence: 99%

Generation of strong magnetic fields in a nascent neutron star accounting for the chiral magnetic effect

2020

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We propose the mean field dynamo model for the generation of strongest magnetic fields, B " 10 15 G, in a neutron star (NS) accounting for the chiral magnetic effect (CME) driven by the shock in a supernova (SN) progenitor of that NS. The temperature jump at a narrow shock front, where an initial magnetic field existing in inflowing matter rises sharply, is the source of the CME that prevails significantly the erasure of the CME due to the spin-flip through Coulomb collisions in plasma. The growth of the magnetic field just behind the shock given by the instability term ∇ˆpαBq in induction equation, stops after a successful SN explosion that throws out the mantle of a protoneutron star. As a result, such an explosion interrupts the transfer of strongly magnetized plasma from the shock onto NS surface and leads to the saturation of the magnetic field. Assuming the rigid protostar rotation, we employ the mean field dynamo, which is similar to the α 2 -dynamo known in the standard magnetohydrodynamics (MHD). The novelty of our model is that α 2 -dynamo is based on concepts of particle physics, applied in MHD, rather than by a mirror asymmetry of convective vortices in the rotating convection.

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“…This instability has been a subject of intensive study in recent years [25,[42][43][44][45][46][47][48][49][50][51][52][53][54][55][56][57][58]. It is established that the growth of this instability is governed by the chiral anomaly equation.…”

Section: Application To Heavy-ion Collisionsmentioning

confidence: 99%

Impact of domain walls on the chiral magnetic effect in hot QCD matter

Tuchin

2018

Phys. Rev. C

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The chiral magnetic effect (CME)-the separation of positive and negative electric charges along the direction of the external magnetic field in quark-gluon plasma and other topologically nontrivial media-is a consequence of the coupling of electrodynamics to the topological gluon field fluctuations that form metastable CP -odd domains. In phenomenological models it is usually assumed that the domains are uniform and the influence of the domain walls on the electric current flow is not essential. This article challenges the latter assumption. A simple model consisting of a uniform spherical domain in a uniform time-dependent magnetic field is introduced and analytically solved. It is shown that (i) no electric current flows into or out of the domain; (ii) the charge separation current, viz. the total electric current flowing inside the domain in the external field direction, is a dissipative Ohm current; (iii) the CME effect can be produced either by the anomalous current or by the boundary conditions on the domain wall; and (iv) the charge separation current oscillates in plasma long after the external field decays. These properties are qualitatively different from the CME in an infinite medium.

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Chiral magnetic effect in protoneutron stars and magnetic field spectral evolution

Cited by 71 publications

References 45 publications

Chiral magnetohydrodynamic turbulence

Chiral magnetohydrodynamic turbulence

Generation of strong magnetic fields in a nascent neutron star accounting for the chiral magnetic effect

Impact of domain walls on the chiral magnetic effect in hot QCD matter

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