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The Evolution of Magnetic Fields in Galaxy Clusters

Published online by Cambridge University Press:  26 May 2016

Matthias Bartelmann ,
Klaus Dolag  and
Harald Lesch
Matthias Bartelmann
Affiliation:
Max-Planck-Institut für Astrophysik, P.O. Box 1317, D-85741 Garching, Germany
Klaus Dolag
Affiliation:
Max-Planck-Institut für Astrophysik, P.O. Box 1317, D-85741 Garching, Germany
Harald Lesch
Affiliation:
Universitätssternwarte München, Scheinerstr. 1, D-81679 München, Germany

Abstract

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Cosmological simulations of magnetic fields in galaxy clusters show that remarkable agreement between simulations and observations of Faraday rotation and radio haloes can be achieved assuming that seed fields of ∼ 10−9 G were present at redshifts ∼ 15−20. The structure of the seed field is irrelevant for the final intracluster field. On average, the field grows exponentially with decreasing cluster redshift, but merger events cause steep transient increases in the field strength. Typical field-reversal scales are of order 50h−1kpc. In most cases, the intracluster fields are dynamically unimportant. Assuming secondary electron models, the average structure of cluster radio haloes can naturally be reproduced.

Type
Galactic Dynamics
Information
Symposium - International Astronomical Union , Volume 208: Astrophysical Supercomputing using Particle Simulations , 2003 , pp. 189 - 198
Copyright
Copyright © Astronomical Society of the Pacific 2003 

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