Microscopic Processes in Global Relativistic Jets Containing Helical Magnetic Fields
Department of Physics, University of Alabama in Huntsville, ZP12, Huntsville, AL 35899, USA
Institute for Theoretical Physics, Goethe University, Frankfurt am Main D-60438, Germany
Institute of Nuclear Physics PAN, ul. Radzikowskiego 152, Kraków 31-342, Poland
Institut fur Physik und Astronomie, Universität Potsdam, Potsdam-Golm 14476, Germany
DESY, Platanenallee 6, Zeuthen 15738, Germany
Instituto de Astrofísica de Andalucía, CSIC, Apartado 3004, Granada 18080, Spain
Institute of Space Science, Atomistilor 409, Bucharest-Magurele RO-077125, Romania
Physics Department, University College Cork, Cork T12 YN60, Ireland
Niels Bohr Institute, University of Copenhagen, Blegdamsvej 17, Copenhagen DK-2100, Denmark
Department of Physics and Astronomy, University of Gent, Proeftuinstraat 86, Gent B-9000, Belgium
LUTH, Observatore de Paris-Meudon, 5 place Jules Jansen, Meudon CEDEX 92195, France
Department of Physics and Astronomy, The University of Alabama, Tuscaloosa, AL 35487, USA
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
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 (
) and electron–positron (
) 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
jet simulation a recollimation-like instability occurs and jet electrons are strongly perturbed. In the
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.
This is an open access article distributed under the Creative Commons Attribution License
which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited. (CC BY 4.0).
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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.
Nishikawa K-I, Mizuno Y, Niemiec J, Kobzar O, Pohl M, Gómez JL, Duţan I, Pe’er A, Frederiksen JT, Nordlund Å, Meli A, Sol H, Hardee PE, Hartmann DH. Microscopic Processes in Global Relativistic Jets Containing Helical Magnetic Fields. Galaxies. 2016; 4(4):38.
Nishikawa, Ken-Ichi; Mizuno, Yosuke; Niemiec, Jacek; Kobzar, Oleh; Pohl, Martin; Gómez, Jose L.; Duţan, Ioana; Pe’er, Asaf; Frederiksen, Jacob T.; Nordlund, Åke; Meli, Athina; Sol, Helene; Hardee, Philip E.; Hartmann, Dieter H. 2016. "Microscopic Processes in Global Relativistic Jets Containing Helical Magnetic Fields." Galaxies 4, no. 4: 38.
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