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3D-MHD simulations of the evolution of magnetic fields in FR II radio sources

Published online by Cambridge University Press:  24 February 2011

Martín Huarte-Espinosa ,
Martin Krause  and
Paul Alexander
Martín Huarte-Espinosa
Affiliation:
Department of Physics and Astronomy, University of Rochester 600 Wilson Boulevard, Rochester, NY, 14627-0171 Kavli Institute for Cosmology Cambridge, Madingley Road, Cambridge CB3 0HA, UK
Martin Krause
Affiliation:
Max-Planck-Institut für Extraterrestrische Physik, Giessenbachstrasse, 85748 Garching, Germany. email: [email protected] Universitätssternwarte München, Scheinerstr. 1, 81679 München, Germany
Paul Alexander
Affiliation:
Astrophysics Group, Cavendish Laboratory, 19 J. J. Thomson Ave., Cambridge CB3 0HE, UK emails: [email protected], [email protected] Kavli Institute for Cosmology Cambridge, Madingley Road, Cambridge CB3 0HA, UK
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Abstract

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3D-MHD numerical simulations of bipolar, hypersonic, weakly magnetized jets and synthetic synchrotron observations are presented to study the structure and evolution of magnetic fields in FR II radio sources. The magnetic field setup in the jet is initially random. The power of the jets as well as the observational viewing angle are investigated. We find that synthetic polarization maps agree with observations and show that magnetic fields inside the sources are shaped by the jets' backflow. Polarimetry statistics correlates with time, the viewing angle and the jet-to-ambient density contrast. The magnetic structure inside thin elongated sources is more uniform than for ones with fatter cocoons. Jets increase the magnetic energy in cocoons, in proportion to the jet velocity. Both, filaments in synthetic emission maps and 3D magnetic power spectra suggest that turbulence develops in evolved sources.

Keywords

galaxies: activejetsmethods: numericalpolarizationMHD
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 6 , Symposium S275: Jets at all Scales , September 2010 , pp. 170 - 171
Copyright
Copyright © International Astronomical Union 2011

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