Anomalous Maxwell equations for inhomogeneous chiral plasma

Gorbar, É. V.; Shovkovy, Igor; Vilchinskiĭ, S. I.; Rudenok, Igor; Boyarsky, Alexey; Ruchayskiy, Oleg

doi:10.1103/physrevd.93.105028

Cited by 74 publications

(102 citation statements)

References 65 publications

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“…[47,55] and both studies concluded that inhomogeneities of the chiral asymmetry have a negligible role for the primordial plasma. Moreover, it was demonstrated in [47] that the inverse cascade proceeds practically in the same way as in the chirally homogeneous model. This assumption can therefore be taken as justified, especially since our main concern in this work is the interplay between the anomaly induced and MHD inverse cascade.…”

Section: Modified Mhd Equationsmentioning

confidence: 99%

“…Some of these objects such as core collapse supernovae, reach high temperatures which makes studies of the chiral magnetic effect in such objects and in the early Universe technically similar. In [46] the formalism was extended to the case of spatially dependent µ 5 , and in [47] it was demonstrated that these inhomogeneities do not prevent the anomalydriven inverse cascade. Again, in all the approaches it was assumed that there are no velocity fields and therefore no turbulence occurring, although even some simple estimates seem to show that it could play a potentially important role both in the early universe [17,38] and in neutron stars [43].…”

Section: Introductionmentioning

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: Introductionmentioning

confidence: 99%

Chiral magnetohydrodynamic turbulence

2017

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“…(37), (38), and (39) into Eqs. (25), (29), and (30), respectively, and performing the integral over t with assumingn 5 (∞) = 0 in the first, 5 we havē…”

Section: E Physical Consequencesmentioning

confidence: 99%

“…(38) and (39)] and the scaling laws of the magnetic and kinetic correlation lengths in chiral matter [see Eqs. (47), (48), and (59)].…”

Section: Introductionmentioning

confidence: 99%

Scaling laws in chiral hydrodynamic turbulence

Yamamoto

2016

Phys. Rev. D

134

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We study the turbulent regime of chiral (magneto)hydrodynamics for charged and neutral matter with chirality imbalance. We find that the chiral magnetohydrodynamics for charged plasmas possesses a unique scaling symmetry, only without fluid helicity under the local charge neutrality. We also find a different type of unique scaling symmetry in the chiral hydrodynamics for neutral matter with fluid helicity in the inertial range. We show that these symmetries dictate the self-similar inverse cascade of the magnetic and kinetic energies. Our results imply the possible inverse energy cascade in core-collapse supernovae due to the chiral transport of neutrinos.

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“…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%

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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Anomalous Maxwell equations for inhomogeneous chiral plasma

Cited by 74 publications

References 65 publications

Chiral magnetohydrodynamic turbulence

Chiral magnetohydrodynamic turbulence

Scaling laws in chiral hydrodynamic turbulence

Laminar and Turbulent Dynamos in Chiral Magnetohydrodynamics. I. Theory

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