Evolution of hydromagnetic turbulence from the electroweak phase transition

被引：83

作者：

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

Kahniashvili, Tina ^{[7
,8
,9
,10
]}

Mandal, Sayan ^{[7
,8
]}

Pol, Alberto Roper ^{[1
,11
]}

Tevzadze, Alexander G. ^{[10
,12
]}

Vachaspati, Tanmay ^{[13
]}

机构：

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

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

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

[4] KTH Royal Inst Technol, Nordita, Roslagstullsbacken 23, S-10691 Stockholm, Sweden

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

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

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

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

[9] Laurentian Univ, Dept Phys, Ramsey Lake Rd, Sudbury, ON P3E 2C, Canada

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

[11] Univ Colorado, Dept Aerosp Engn Sci, Boulder, CO 80303 USA

[12] Javakhishvili Tbilisi State Univ, Fac Exact & Nat Sci, 3 Chavchavadze Ave, Tbilisi 0179, Georgia

[13] Arizona State Univ, Dept Phys, Tempe, AZ 85287 USA

来源：

PHYSICAL REVIEW D | 2017年 / 96卷 / 12期

基金：

美国国家科学基金会;

关键词：

MAGNETIC-FIELDS; ROTATION;

D O I：

10.1103/PhysRevD.96.123528

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We present new simulations of decaying hydromagnetic turbulence for a relativistic equation of state relevant to the early Universe. We compare helical and nonhelical cases either with kinetically or magnetically dominated initial fields. Both kinetic and magnetic initial helicities lead to maximally helical magnetic fields after some time, but with different temporal decay laws. Both are relevant to the early Universe, although no mechanisms have yet been identified that produce magnetic helicity with strengths comparable to the big bang nucleosynthesis limit at scales comparable to the Hubble horizon at the electroweak phase transition. Nonhelical magnetically dominated fields could still produce picoGauss magnetic fields under most optimistic conditions. Only helical magnetic fields can potentially have nanoGauss strengths at scales up to 30 kpc today.

引用

页数：16

共 61 条

[1]

[Anonymous], 2016, arXiv:1608.06619

[2]

Arnold V., 2014, VLADIMIR I ARNOLD CO, V2, P357

[3] Evolution of cosmic magnetic fields: From the very early Universe, to recombination, to the present [J].