Numerical simulations of the decay of primordial magnetic turbulence

Journal Article · Tue Jun 15 00:00:00 EDT 2010 · Physical Review. D, Particles Fields

DOI:https://doi.org/10.1103/PHYSREVD.81.123002· OSTI ID:21408024

Kahniashvili, Tina ^[1]; Brandenburg, Axel ^[2]; Tevzadze, Alexander G ^[3]; Ratra, Bharat ^[4]

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1. McWilliams Center for Cosmology and Department of Physics, Carnegie Mellon University, 5000 Forbes Ave, Pittsburgh, Pennsylvania 15213 (United States)
2. Nordita, AlbaNova University Center, Roslagstullsbacken 23, 10691 Stockholm (Sweden)
3. Abastumani Astrophysical Observatory, Ilia State University, 2A Kazbegi Ave, Tbilisi, GE-0160 (Georgia)
4. Department of Physics, Kansas State University, 116 Cardwell Hall, Manhattan, Kansas 66506 (United States)

We perform direct numerical simulations of forced and freely decaying 3D magnetohydrodynamic turbulence in order to model magnetic field evolution during cosmological phase transitions in the early Universe. Our approach assumes the existence of a magnetic field generated either by a process during inflation or shortly thereafter, or by bubble collisions during a phase transition. We show that the final configuration of the magnetic field depends on the initial conditions, while the velocity field is nearly independent of initial conditions.

• OSTI ID: 21408024
• Journal Information: Physical Review. D, Particles Fields, Vol. 81, Issue 12; Other Information: DOI: 10.1103/PhysRevD.81.123002; (c) 2010 The American Physical Society; ISSN 0556-2821
• Country of Publication: United States
• Language: English

Related Subjects

79 ASTROPHYSICS
COSMOLOGY AND ASTRONOMY
72 PHYSICS OF ELEMENTARY PARTICLES AND FIELDS
COLLISIONS
COMPUTERIZED SIMULATION
CONFIGURATION
COSMOLOGICAL MODELS
EVOLUTION
INFLATIONARY UNIVERSE
MAGNETIC FIELDS
MAGNETOHYDRODYNAMICS
PARTICLE DECAY
PHASE TRANSFORMATIONS
TURBULENCE
UNIVERSE
VELOCITY
DECAY
FLUID MECHANICS
HYDRODYNAMICS
MATHEMATICAL MODELS
MECHANICS
SIMULATION