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

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Original languageEnglish
Pages (from-to)170-171
JournalProceedings of the International Astronomical Union
Journal publication date1 Sep 2010
Volume6
IssueS275
DOIs
Publication statusPublished - 1 Sep 2010

Abstract

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.

Notes

Martin Huarte-Espinoza, Martin Krause, and Paul Alexander, '3D-MHD simulations of the evolution of magnetic fields in FR II radio sources', Proceedings of the International Astronomical Union, Vol. 6 (S275), September 2010, pp. 170-171, available online at DOI: https://doi.org/10.1017/S1743921310015899. COPYRIGHT: © International Astronomical Union 2011

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