Sign on

SAO/NASA ADS Astronomy Abstract Service

· Find Similar Abstracts (with default settings below)
· Electronic Refereed Journal Article (HTML)
· arXiv e-print (arXiv:1004.3084)
· References in the article
· Citations to the Article (6) (Citation History)
· Refereed Citations to the Article
· Also-Read Articles (Reads History)
·
· Translate This Page
Title:
Numerical simulations of the decay of primordial magnetic turbulence
Authors:
Kahniashvili, Tina; Brandenburg, Axel; Tevzadze, Alexander G.; Ratra, Bharat
Affiliation:
AA(McWilliams Center for Cosmology and Department of Physics, Carnegie Mellon University, 5000 Forbes Ave, Pittsburgh, Pennsylvania 15213, USA; Department of Physics, Laurentian University, Ramsey Lake Road, Sudbury, ON P3E 2C, Canada; Abastumani Astrophysical Observatory, Ilia State University, 2A Kazbegi Ave, Tbilisi, GE-0160, Georgia), AB(Nordita, AlbaNova University Center, Roslagstullsbacken 23, 10691 Stockholm, Sweden; Department of Astronomy, Stockholm University, SE 10691 Stockholm, Sweden), AC(Abastumani Astrophysical Observatory, Ilia State University, 2A Kazbegi Ave, Tbilisi, GE-0160, Georgia; Faculty of Exact and Natural Sciences, Tbilisi State University, 1 Chavchavadze Avenue Tbilisi, GE-0128, Georgia), AD(Department of Physics, Kansas State University, 116 Cardwell Hall, Manhattan, Kansas 66506, USA)
Publication:
Physical Review D, vol. 81, Issue 12, id. 123002 (PhRvD Homepage)
Publication Date:
06/2010
Origin:
APS
PACS Keywords:
Background radiations, Cosmology
Abstract Copyright:
(c) 2010: The American Physical Society
DOI:
10.1103/PhysRevD.81.123002
Bibliographic Code:
2010PhRvD..81l3002K

Abstract

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.
Bibtex entry for this abstract   Preferred format for this abstract (see Preferences)
   

Find Similar Abstracts:

Use: Authors
Title
Keywords (in text query field)
Abstract Text
Return: Query Results Return    items starting with number
Query Form
Database: Astronomy
Physics
arXiv e-prints