Chiral magnetohydrodynamic turbulence

Pavlović, Petar; Leite, Natacha; Sigl, Günter

doi:10.1103/physrevd.96.023504

Cited by 41 publications

(49 citation statements)

References 86 publications

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“…Note that different choices of evolution equations for µ 5 are possible, depending on the microscopic physics; see the discussion in Boyarsky et al (2015). In particular, an evolution equation for µ 5 with a damping term, −Γ f µ 5 , and a source term, Γ sr µ 5 , has recently been used by Pavlović et al (2017) to study the influence of the chiral anomaly on the evolution of MHD turbulence. Here Γ f is the total chirality flipping rate, and Γ sr is a source term that takes into account the generation of chiral asymmetry.…”

Section: Dynamic Equation For the Chiral Chemical Potentialmentioning

confidence: 99%

“…This contribution to the electric current causes an instability in the system (Joyce & Shaposhnikov 1997) that has been analyzed in many works (Fröhlich & Pedrini 2000;Ooguri & Oshikawa 2012;Boyarsky et al 2012a;Kumar et al 2014;Grabowska et al 2015;Manuel & Torres-Rincon 2015;Buividovich & Ulybyshev 2016;Boyarsky et al 2015;). This instability may be relevant in the physics of the early universe (Joyce & Shaposhnikov 1997;Fröhlich & Pedrini 2000, 2002Semikoz & Sokoloff 2004;Semikoz et al 2009;Boyarsky et al 2012a,b;Semikoz et al 2012;Tashiro et al 2012;Dvornikov & Semikoz 2012, 2014Manuel & Torres-Rincon 2015;Gorbar et al 2016;Pavlović et al 2016;Pavlović et al 2017), of the quark-gluon plasmas (Akamatsu & Yamamoto 2013;Taghavi & Wiedemann 2015;Hirono et al 2015), or of neutron stars (Ohnishi & Yamamoto 2014;Dvornikov & Semikoz 2015a,b;Yamamoto 2016;Dvornikov 2016). However, to the best of our knowledge, a systematic analysis of the system of chiral MHD equations, including the back-reaction of the magnetic field on the chiral chemical potential and the coupling to the plasma velocity field, U (t, x) appears to be missing.…”

Section: Introductionmentioning

confidence: 99%

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Laminar and Turbulent Dynamos in Chiral Magnetohydrodynamics. I. Theory

Rogachevskii

Ruchayskiy²,

Boyarsky

et al. 2017

ApJ

125

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The magnetohydrodynamic (MHD) description of plasmas with relativistic particles necessarily includes an additional new field, the chiral chemical potential associated with the axial charge (i.e., the number difference between right-and left-handed relativistic fermions). This chiral chemical potential gives rise to a contribution to the electric current density of the plasma (chiral magnetic effect ). We present a self-consistent treatment of the chiral MHD equations, which include the back-reaction of the magnetic field on a chiral chemical potential and its interaction with the plasma velocity field. A number of novel phenomena are exhibited. First, we show that the chiral magnetic effect decreases the frequency of the Alfvén wave for incompressible flows, increases the frequencies of the Alfvén wave and of the fast magnetosonic wave for compressible flows, and decreases the frequency of the slow magnetosonic wave. Second, we show that, in addition to the well-known laminar chiral dynamo effect, which is not related to fluid motions, there is a dynamo caused by the joint action of velocity shear and chiral magnetic effect. In the presence of turbulence with vanishing mean kinetic helicity, the derived mean-field chiral MHD equations describe turbulent large-scale dynamos caused by the chiral alpha effect, which is dominant for large fluid and magnetic Reynolds numbers. The chiral alpha effect is due to an interaction of the chiral magnetic effect and fluctuations of the small-scale current produced by tangling magnetic fluctuations (which are generated by tangling of the largescale magnetic field by sheared velocity fluctuations). These dynamo effects may have interesting consequences in the dynamics of the early universe, neutron stars, and the quark-gluon plasma.

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Section: Dynamic Equation For the Chiral Chemical Potentialmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Laminar and Turbulent Dynamos in Chiral Magnetohydrodynamics. I. Theory

Rogachevskii

Ruchayskiy²,

Boyarsky

et al. 2017

ApJ

125

View full text Add to dashboard Cite

show abstract

“…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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“…This idea was also used by Sigl [3][4][5] in the context of neutron star astrophysics, and one concluded that the amplification a e-mail: garcia@dft.if.uerj.br of the magnetic field is replaced actually by an attenuation of the magnetic field. By making use also of chiral QED in spacetimes with torsion (referring to work by de Sabbata and Gasperini [6]) one derived from the polarization of vacuum and electron-positron massive fermion pairs that the time component of the torsion axial vector term in the curl B equation induces the chiral term where indeed the electric current seems to be along the magnetic field.…”

Section: Introductionmentioning

confidence: 98%

Metric-torsion decay of non-adiabatic chiral helical magnetic fields against chiral dynamo action in bouncing cosmological models

Andrade

2018

Eur. Phys. J. C

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Metric-torsion effects on chiral massless fermions are investigated in the realm of the adiabatic amplification of cosmological magnetic fields (CMFs) in a general relativistic framework and in the framework of Einstein-Cartan (EC) bouncing cosmologies. In GR the chiral effect is proportional to the Hubble factor and the solution of the dynamo equation leads to an adiabatic magnetic field, while in Einstein-Cartan bouncing cosmology we have non-adiabatic magnetic fields where the breaking of adiabaticity is given by a torsion term. Using a EWPT magnetic field of the order of B seed ∼ 10 24 G at 5 pc scale, we obtain a CMF in EC of the order of 10 −10 G, which is still able to seed a galactic dynamo which amplifies this field up to galactic magnetic fields of four orders of magnitude, which is a mild dynamo. In the case of massive chiral fermions it is shown that torsion actually attenuated the convective dynamo term in the dynamo equation obtained from the QED of an electron-positron pair e − e + . Chiral effects on general relativity may lead to strong magnetic fields of the order of ∼ 10 18 G at the early universe resulting from pure metric effects. Strong magnetic fields of the order of B metric−torsion ∼ 10 8 G may be obtained from very strong seed fields. At 1 Mpc scale of the present universe a galactic dynamo seed of the order of 10 −19 G is found. It is shown in this paper that chiral dynamo effects in the expanded universe can be obtained if one takes into account the speed of the cosmic plasma.

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Chiral magnetohydrodynamic turbulence

Cited by 41 publications

References 86 publications

Laminar and Turbulent Dynamos in Chiral Magnetohydrodynamics. I. Theory

Laminar and Turbulent Dynamos in Chiral Magnetohydrodynamics. I. Theory

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

Metric-torsion decay of non-adiabatic chiral helical magnetic fields against chiral dynamo action in bouncing cosmological models

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