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Galaxies 2016, 4(4), 38; doi:10.3390/galaxies4040038

Microscopic Processes in Global Relativistic Jets Containing Helical Magnetic Fields

1
Department of Physics, University of Alabama in Huntsville, ZP12, Huntsville, AL 35899, USA
2
Institute for Theoretical Physics, Goethe University, Frankfurt am Main D-60438, Germany
3
Institute of Nuclear Physics PAN, ul. Radzikowskiego 152, Kraków 31-342, Poland
4
Institut fur Physik und Astronomie, Universität Potsdam, Potsdam-Golm 14476, Germany
5
DESY, Platanenallee 6, Zeuthen 15738, Germany
6
Instituto de Astrofísica de Andalucía, CSIC, Apartado 3004, Granada 18080, Spain
7
Institute of Space Science, Atomistilor 409, Bucharest-Magurele RO-077125, Romania
8
Physics Department, University College Cork, Cork T12 YN60, Ireland
9
Niels Bohr Institute, University of Copenhagen, Blegdamsvej 17, Copenhagen DK-2100, Denmark
10
Department of Physics and Astronomy, University of Gent, Proeftuinstraat 86, Gent B-9000, Belgium
11
LUTH, Observatore de Paris-Meudon, 5 place Jules Jansen, Meudon CEDEX 92195, France
12
Department of Physics and Astronomy, The University of Alabama, Tuscaloosa, AL 35487, USA
13
Department of Physics and Astronomy, Clemson University, Clemson, SC 29634, USA
*
Author to whom correspondence should be addressed.
Academic Editors: Jose L. Gòmez, Alan P. Marscher and Svetlana G. Jorstad
Received: 13 July 2016 / Revised: 14 September 2016 / Accepted: 22 September 2016 / Published: 29 September 2016
(This article belongs to the Special Issue Blazars through Sharp Multi-wavelength Eyes)
View Full-Text   |   Download PDF [8405 KB, uploaded 29 September 2016]   |  

Abstract

In the study of relativistic jets one of the key open questions is their interaction with the environment on the microscopic level. Here, we study the initial evolution of both electron–proton ( e p + ) and electron–positron ( e ± ) relativistic jets containing helical magnetic fields, focusing on their interaction with an ambient plasma. We have performed simulations of “global” jets containing helical magnetic fields in order to examine how helical magnetic fields affect kinetic instabilities such as the Weibel instability, the kinetic Kelvin-Helmholtz instability (kKHI) and the Mushroom instability (MI). In our initial simulation study these kinetic instabilities are suppressed and new types of instabilities can grow. In the e p + jet simulation a recollimation-like instability occurs and jet electrons are strongly perturbed. In the e ± jet simulation a recollimation-like instability occurs at early times followed by a kinetic instability and the general structure is similar to a simulation without helical magnetic field. Simulations using much larger systems are required in order to thoroughly follow the evolution of global jets containing helical magnetic fields. View Full-Text
Keywords: relativistic jets; particle-in-cell simulations; global jets; helical magnetic fields; kinetic instabilities; kink instability relativistic jets; particle-in-cell simulations; global jets; helical magnetic fields; kinetic instabilities; kink instability
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MDPI and ACS Style

Nishikawa, K.-I.; Mizuno, Y.; Niemiec, J.; Kobzar, O.; Pohl, M.; Gómez, J.L.; Duţan, I.; Pe’er, A.; Frederiksen, J.T.; Nordlund, Å.; Meli, A.; Sol, H.; Hardee, P.E.; Hartmann, D.H. Microscopic Processes in Global Relativistic Jets Containing Helical Magnetic Fields. Galaxies 2016, 4, 38.

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