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

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3D-MHD simulations of the evolution of magnetic fields in FR II radio sources. / Huarte-Espinosa, M.; Krause, M.; Alexander, P.

In: Proceedings of the International Astronomical Union, Vol. 6, No. S275, 01.09.2010, p. 170-171.

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@article{31447c4fe03549f49abf6d2b4baad87e,
title = "3D-MHD simulations of the evolution of magnetic fields in FR II radio sources",
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.",
keywords = "galaxies: active, jets, methods: numerical, polarization, MHD",
author = "M. Huarte-Espinosa and M. Krause and P. Alexander",
note = "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: {\textcopyright} International Astronomical Union 2011",
year = "2010",
month = sep,
day = "1",
doi = "10.1017/S1743921310015899",
language = "English",
volume = "6",
pages = "170--171",
journal = "Proceedings of the International Astronomical Union",
issn = "1743-9213",
publisher = "Cambridge University Press",
number = "S275",

}

RIS

TY - JOUR

T1 - 3D-MHD simulations of the evolution of magnetic fields in FR II radio sources

AU - Huarte-Espinosa, M.

AU - Krause, M.

AU - Alexander, P.

N1 - 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

PY - 2010/9/1

Y1 - 2010/9/1

N2 - 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.

AB - 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.

KW - galaxies: active

KW - jets

KW - methods: numerical

KW - polarization

KW - MHD

U2 - 10.1017/S1743921310015899

DO - 10.1017/S1743921310015899

M3 - Article

VL - 6

SP - 170

EP - 171

JO - Proceedings of the International Astronomical Union

JF - Proceedings of the International Astronomical Union

SN - 1743-9213

IS - S275

ER -