The Turbulent Chiral Magnetic Cascade in the Early Universe

被引：69

作者：

Brandenburg, Axel ^{[1
,2
,3
,4
,5
,6
]}

Schober, Jennifer ^{[4
,5
]}

Rogachevskii, Igor ^{[1
,4
,5
,7
]}

Kahniashvili, Tina ^{[8
,9
,10
]}

Boyarsky, Alexey ^{[11
]}

Frohlich, Jog ^{[12
]}

Ruchayskiy, Oleg ^{[13
]}

Kleeorin, Nathan ^{[4
,5
,7
]}

机构：

[1] Univ Colorado, Lab Atmospher & Space Phys, 3665 Discovery Dr, Boulder, CO 80303 USA

[2] Univ Colorado, JILA, Box 440, Boulder, CO 80303 USA

[3] Univ Colorado, Dept Astrophys & Planetary Sci, Box 440, Boulder, CO 80303 USA

[4] KTH Royal Inst Technol, NORDITA, Roslagstullsbacken 23, SE-10691 Stockholm, Sweden

[5] Stockholm Univ, Roslagstullsbacken 23, SE-10691 Stockholm, Sweden

[6] Stockholm Univ, Dept Astron, AlbaNova Univ Ctr, SE-10691 Stockholm, Sweden

[7] Ben Gurion Univ Negev, Dept Mech Engn, POB 653, IL-84105 Beer Sheva, Israel

[8] Carnegie Mellon Univ, McWilliams Ctr Cosmol, 5000 Forbes Ave, Pittsburgh, PA 15213 USA

[9] Carnegie Mellon Univ, Dept Phys, 5000 Forbes Ave, Pittsburgh, PA 15213 USA

[10] Ilia State Univ, Abastumani Astrophys Observ, 3-5 Cholokashvili St, GE-0194 Tbilisi, Georgia

[11] Leiden Univ, Inst Lorentz Theoret Phys, Niels Bohrweg 2, NL-2333 CA Leiden, Netherlands

[12] ETH Honggerberg, Inst Theoret Phys, CH-8093 Zurich, Switzerland

[13] Niels Bohr Inst, Discovery Ctr, Blegdamsvej 17, DK-2100 Copenhagen, Denmark

来源：

ASTROPHYSICAL JOURNAL LETTERS | 2017年 / 845卷 / 02期

基金：

美国国家科学基金会; 欧洲研究理事会;

关键词：

dynamo; early universe; magnetic fields; magnetohydrodynamics (MHD); turbulence; GAMMA-RAYS; EQUILIBRIUM; FIELDS;

D O I：

10.3847/2041-8213/aa855d

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

The presence of asymmetry between fermions of opposite handedness in plasmas of relativistic particles can lead to exponential growth of a helical magnetic field via a small-scale chiral dynamo instability known as the chiral magnetic effect. Here, we show, using dimensional arguments and numerical simulations, that this process produces through the Lorentz force chiral magnetically driven turbulence. A k(-2) magnetic energy spectrum emerges via inverse transfer over a certain range of wavenumbers k. The total chirality (magnetic helicity plus normalized chiral chemical potential) is conserved in this system. Therefore, as the helical magnetic field grows, most of the total chirality gets transferred into magnetic helicity until the chiral magnetic effect terminates. Quantitative results for height, slope, and extent of the spectrum are obtained. Consequences of this effect for cosmic magnetic fields are discussed.

引用

页数：6

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