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dc.contributor.authorHuarte-Espinosa, M.
dc.contributor.authorKrause, M.
dc.contributor.authorAlexander, P.
dc.date.accessioned2017-04-20T16:00:50Z
dc.date.available2017-04-20T16:00:50Z
dc.date.issued2010-09-01
dc.identifier.citationHuarte-Espinosa , M , Krause , M & Alexander , P 2010 , ' 3D-MHD simulations of the evolution of magnetic fields in FR II radio sources ' , Proceedings of the International Astronomical Union , vol. 6 , no. S275 , pp. 170-171 . https://doi.org/10.1017/S1743921310015899
dc.identifier.issn1743-9213
dc.identifier.otherPURE: 10547262
dc.identifier.otherPURE UUID: 31447c4f-e035-49f4-9abf-6d2b4baad87e
dc.identifier.otherBibtex: urn:7c554e7f9288e73c4c5dc1b1b9f91cf8
dc.identifier.otherScopus: 84882770545
dc.identifier.otherORCID: /0000-0002-9610-5629/work/63687364
dc.identifier.urihttp://hdl.handle.net/2299/17998
dc.descriptionMartin 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
dc.description.abstract3D-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.en
dc.language.isoeng
dc.relation.ispartofProceedings of the International Astronomical Union
dc.subjectgalaxies: active
dc.subjectjets
dc.subjectmethods: numerical
dc.subjectpolarization
dc.subjectMHD
dc.title3D-MHD simulations of the evolution of magnetic fields in FR II radio sourcesen
dc.contributor.institutionSchool of Physics, Astronomy and Mathematics
dc.contributor.institutionCentre for Astrophysics Research
dc.description.statusNon peer reviewed
rioxxterms.versionofrecordhttps://doi.org/10.1017/S1743921310015899
rioxxterms.typeJournal Article/Review
herts.preservation.rarelyaccessedtrue


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